Author name code: berger ADS astronomy entries on 2022-09-14 author:"Berger, Thomas E." OR author:"Berger, Tom" ------------------------------------------------------------------------ Title: 4π Heliospheric Observing System - 4π-HeliOS: Exploring the Heliosphere from the Solar Interior to the Solar Wind Authors: Raouafi, Nour E.; Gibson, Sarah; Ho, George; Laming, J. Martin; Georgoulis, Manolis K.; Szabo, Adam; Vourlidas, Angelos; Mason, Glenn M.; Hoeksema, J. Todd; Velli, Marco; Berger, Thomas; Hassler, Donald M.; Kinnison, James; Viall, Nicholeen; Case, Anthony; Newmark, Jeffrey; Lepri, Susan; Krishna Jagarlamudi, Vamsee; Raouafi, Nour; Bourouaine, Sofiane; Vievering, Juliana T.; Englander, Jacob A.; Shannon, Jackson L.; Perez, Rafael M.; Chattopadhyay, Debarati; Mason, James P.; Leary, Meagan L.; Santo, Andy; Casti, Marta; Upton, Lisa A. Bibcode: 2022cosp...44.1530R Altcode: The 4$\pi$ Heliospheric Observing System (4$\pi$-HeliOS) is an innovative mission concept study for the next Solar and Space Physics Decadal Survey to fill long-standing knowledge gaps in Heliophysics. A constellation of spacecraft will provide both remote sensing and in situ observations of the Sun and heliosphere from a full 4$\pi$-steradian field of view. The concept implements a holistic observational philosophy that extends from the Sun's interior, to the photosphere, through the corona, and into the solar wind simultaneously with multiple spacecraft at multiple vantage points optimized for continual global coverage over much of a solar cycle. The mission constellation includes two spacecraft in the ecliptic and two flying as high as $\sim$70$^\circ$ solar latitude. 4$\pi$-HeliOS will provide new insights into the fundamental processes that shape the whole heliosphere. The overarching goals of the 4$\pi$-HeliOS concept are to understand the global structure and dynamics of the Sun's interior, the generation of solar magnetic fields, the origin of the solar cycle, the causes of solar activity, and the structure and dynamics of the corona as it creates the heliosphere. The mission design study is underway at the Johns Hopkins Applied Physics Laboratory Concurrent Engineering Laboratory (ACE Lab), a premier mission design center, fostering rapid and collaborative mission design evolutions. Title: Thermospheric Drag Sondes: on-demand probes of the lower Thermosphere/Mesosphere system Authors: Berger, Thomas; Pilinski, Marcin; Nock, Kerry; Sutton, Eric; Bernstein, Research Valerie; Aaron, Kim; Warnecke, Mark; Thayer, Jeffrey Bibcode: 2022cosp...44..804B Altcode: The Thermospheric Drag Sonde (TDS) is a system concept designed to provide multiple, affordable, and expendable thermosphere/mesosphere probes in a compact format that can be stored on space stations, like the International Space Station (ISS), and launched on demand. The motivation for the concept is the lack of data on the lower ionosphere/thermosphere/mesosphere (ITM) system (~100 - 300 km AMSL) and the difficulty in sustaining orbital platforms at these very Low Earth Orbit (VLEO) altitudes for periods sufficient to sample a wide variety of conditions in geospace. The TDS concept takes its inspiration from upper atmospheric radiosondes that are launched on demand on balloons to provide critical data for terrestrial weather forecasting models. The recent loss of forty SpaceX Starlink satellites due to unexpectedly large atmospheric drag increases at their staging altitude of 210 km during a minor geomagnetic storm emphasizes the need for improved forecasting and nowcasting information at VLEO altitudes. Probe-on-demand systems such as the TDS would fill a key gap in ITM science and data assimilation in forecasting models. A single TDS consists of a compact storage format that deploys into large, lightweight satellite equipped with one or more accelerometers to directly measure drag effects, a dual-frequency GNSS receiver, a compact radio link, and a passive de-orbit system that enables prompt re-entry after deployment from the ISS. Utilizing innovative spherical profile technology to simplify coefficient of drag calculations, TDS deployments will obtain acceleration and GPS Precise Orbit Determination (POD) data during descent and re-entry, providing neutral density profiles for novel science investigations of the ITM system, forecast model data assimilation, and nowcasting data to inform launch operations. The concept is in development with a notional deployment to the ISS in the 2026 timeframe. Title: Space Weather with Quantified Uncertainty (SWQU): Ensemble Learning for Accurate and Reliable Uncertainty Quantification Authors: Camporeale, Enrico; Bortnik, Jacob; Berger, Thomas; Guedes dos Santos, Luiz Fernando; Hu, Andong Bibcode: 2022cosp...44..865C Altcode: We give an overview of the NASA/NSF funded "Ensemble Learning for Accurate and Reliable Uncertainty Quantification" SWQU project. The objective of the project is to create the algorithmic prototype that will combine a small number of high-fidelity (low error, but computationally expensive) runs from physics-based models with a large number of (possibly) less accurate but faster runs from machine learning models. The goal is to obtain a more accurate overall prediction than any individual model, and an estimation of the associated uncertainties. We showcase application examples ranging from geomagnetic index predictions to solar wind, radiation belt fluxes, and ground based magnetic field forecasting. The core engine of the probabilistic predictions is the Accurate and Reliable Uncertainty Estimate (ACCRUE) model, that is briefly discussed. ACCRUE is able to estimate uncertainties associated to deterministic predictions, by solving a deep learning semi-supervised regression problem. Title: ESA's Human Interplanetary Exploration Radiation Risk Assessment System (HIERRAS) Authors: Heynderickx, Daniel; Berger, Thomas; Jiggens, Piers; Vainio, Rami; Matthiä, Daniel; Lei, Fan; Raukunen, Osku; Sandberg, Ingmar; Clucas, Simon; Truscott, Pete Bibcode: 2022cosp...44.2708H Altcode: The Human Interplanetary Exploration Radiation Risk Assessment System (HIERRAS, ESA Contract No 4000127129/19/NL/HK) is a chain of tools for calculation of human radiological and equipment radiation effects for future interplanetary missions within helio-radii 0.9-1.6 AU. The system uses existing software tools and models rather than creating new tools and focusses on seamless and intuitive interfaces between software modules in order to minimise user intervention in the model chains. This presentation will describe the overall HIERRAS system architecture and the following components: \begin{itemize} \item Development of a Python based application framework to collect user requests, execute model runs and return the results to the users. Data are passed internally as json structures which include a standardised set of descriptive metadata. This HIERRAS framework uses the SPECTIRES Python software to run environment and effects analysis models and tools locally as well as through ESA's Network of Models (NoM) infrastructure. Information on registered users and on run requests and results is maintained in an SQL database. \item Development of a GUI to allow users to set up model configurations, execute model runs and collect the results on a series of web pages. The GUI communicates with the application framework by exchanging json structures. Extensive background information and a user manual are provided as well. \item Use of a response function type approach to handle atmospheric transport and geometry shielding of the primary radiation environment and derivation of radiation quantities inside (and outside) space vehicles and habitats. \item HIERRAS uses the Geant4 GRAS software to simulate 3D particle interactions with planetary atmospheres and surfaces in addition to spacecraft structures, equipment and astronauts. A GRAS pre-processor software tool (GRAPPA, abstract submitted to Scientific Event F2.3) was developed to define position- and epoch-dependent planetary surface geometries based on the Mars Climate Database (MCD v5.3), LIP's SOILCOMPI dataset for Mars's surface composition, and Lunar Prospector gamma-ray spectrometer data for the Moon's surface composition. \item Re-processing and re-calibration of the GOES HEPAD high energy proton flux time series. The data were used to extend the SEPEM reference data with three energy channels (up to 875 MeV). A new background identification and removal algorithm was applied to the dataset. The SAPPHIRE SEP model was updated accordingly. \item Definition of validation and verification procedures using interplanetary mission datasets and outputs from the ROSSINI3 study (ESA Contract No 4000125785/18/NL/GLC). \item Updates to the Geant4 space applications and setting up of docker containers for easy distribution, bypassing Geant4 installation. \end{itemize} Title: Poster Presentation and Discussion Authors: Berger, Thomas Bibcode: 2022cosp...44.2707B Altcode: Poster Presentation and Discussion Title: The Dosis 3D Project On-Board the International Space Sta- Tion - Status and Science Overview of 10 Years of Measurements (2012 - 2022) Authors: Berger, Thomas Bibcode: 2022cosp...44.2691B Altcode: The radiation environment encountered in space differs in nature from that on Earth, consisting mostly of highly energetic ions from protons up to iron, resulting in radiation levels far exceeding the ones present on Earth for occupational radiation workers. Since the beginning of the space era the radiation exposure during space missions has been monitored with various passive and active radiation instruments. Also, on-board the International Space Station (ISS) a number of area monitoring devices provide data related to the spatial and temporal variation of the radiation field in - and outside the ISS. The aim of the DOSIS 3D (2012 - ongoing) experiment is the measurement of the radiation environment within the European Columbus Laboratory of the ISS. These measurements are, on the one hand, performed with passive radiation detectors mounted at eleven locations within Columbus for the determination of the spatial distribution of the radiation field parameters and, on the other hand, with two active radiation detectors (DOSTEL) mounted at a fixed position inside Columbus for the determination of the temporal variation of the radiation field parameters. The talk will give an overview of the current results of the data evaluation performed for the passive and active radiation detectors for DOSIS 3D in the years 2012 to 2022 and further focus on the work in progress for data comparison with other passive and active radiation detector systems measuring on-board the ISS. Acknowledgments: The participation of the Technische Universität Wien, Atominstitut (ATI), Vienna, Austria in the DOSIS-1 and -2 experiments was supported by the Austrian Space Applications Programme (ASAP) under contract no. 819643. The Polish contribution for the Institute of Nuclear Physics (IFJ), Krakow, Poland was supported by the National Science Center (project No DEC-2012/06/M/ST9/00423). EK greatly acknowledges the possibility to participate in the project to DLR and to the ESA PECS for the financial grant No. PECS4000108464. The participation of the Nuclear Physics Institute of the Czech Academy of Sciences has been supported by the grant of Czech Science Foundation (GACR) No. 15-16622Y. The CAU, University of Kiel was supported by DLR under grants 50WB0826, 50WB1026, 50WB1232, 50WB1533 and 50WB1817. Title: SEP Measurements on the Surface of Mars with the Radiation Assessment Detector (RAD) aboard the Curiosity rover Authors: Ehresmann, Bent; Berger, Thomas; Reitz, Guenther; Guo, Jingnan; Zeitlin, Cary; Wimmer-Schweingruber, Robert; Matthiä, Daniel; Hassler, Donald M. Bibcode: 2022cosp...44.1174E Altcode: Exposure to space radiation remains one of the major risks for human space exploration. Besides the ever-present Galactic Cosmic Radiation (GCR), spontaneous Solar Energetic Particles (SEPs) emitted from the Sun during Coronal Mass Ejections (CMEs) or solar flares, can dominate planetary and interplanetary radiation fields and increase the radiation dose by potentially orders of magnitudes. To better understand SEP propagation throughout the heliosphere and their radial and longitudinal dependencies, space weather monitoring at various location throughout the heliosphere is required. On the surface of Mars, the Radiation Assessment Detector (RAD) aboard NASA's Curiosity rover has been analyzing the radiation environment in Gale crater since 2012. Besides characterizing the radiation dose, RAD is also capable of measuring energy spectra and integral fluxes of charged and neutral particles. For the example of charged particles, RAD can distinguish between different ion species and for low-Z particles also between the different isotopes. RAD's location on the surface of Mars allows for unique space weather observations at 1.5 AU that are directly relevant to understanding particle propagation through the inner heliosphere, and the impact of space weather on future human explorers of the Red Planet. RAD's detailed measurements of SEP events, and other interesting observations, such as arrival times and duration of Forbush Decreases, CMEs, or the occurrence of Co-Rotating Interaction Regions (CIRs) provide valuable data for inter-comparison with measurements from other instrument at Earth and throughout the heliosphere. To contextualize the RAD SEP measurements, it is important to consider that Mars possesses an, albeit thin, atmosphere that can filter out lower-energy particles. Thus, protons need about 150 - 170 MeV to propagate through the atmosphere, reach the surface, and be detected by RAD. During the first nine years of its mission, RAD detected five moderate SEP events on the surface of Mars. As the solar cycle is now progressing towards the next solar maximum, strong SEP events are more likely to occur. Consequently, RAD has measured the two strongest events yet encountered, in the past four months. In this presentation, we will provide an overview of 10 years of SEP event observations on the surface of Mars with the RAD instrument. We will then focus on the last two strongest SEP events: the October 28, 2021 event where dose rates increased by a factor of 2.25; and the February 16, 2022 event where dose rates increased by a factor of 3.5 during the event. Title: Development of the Internal Dosimetry Array for Gateway Authors: Zabori, Balazs; Berger, Thomas; Hirn, Attila; Nagamatsu, Aiko; Gutay, Gergely; Fetter, Viktor; Granja, Carlos; Boersma, Nadine Bibcode: 2022cosp...44.2698Z Altcode: The Gateway space station, to be built in orbit around the Moon in the mid-2020s, will not be protected by the Earth's magnetic field or the atmosphere; hence, astronauts could be exposed to up to 700 times the radiation dose of an average human on Earth from space radiation. The Internal Dosimeter Array (IDA) instrument suite is the very first internal ESA experiment on board Gateway. The IDA payload is accommodated inside the US HALO module within a Payload Bank and it is composed of the following already existing and flight proven instruments: - TRITEL 3D silicon detector telescope provided by Centre for Energy Research (EK); - European Active Dosimeter (EAD) provided by German Aerospace Center (DLR); - Medipix (MPX) detector provided by Advacam s.r.o. (AVD); - PADLES and D-SPACE provided by Japanese Space Agency (JAXA). IDA instruments provide, based on measurements of energy deposition and particle track analysis, particle fluxes and fluences, LET spectra, mean quality factors, absorbed dose and dose equivalent rates, as well as intergrated absorbed dose and dose equivalent from the charged particle component of space radiation. Besides charged particles (electrons, protons, He ions and HZE particles), X-rays and gamma-rays are also measured. The IDA instrument suite covers an overall LET range up to 1470 keV/$\mu$m in water (including the full range of 0.1 - 150 keV/$\mu$m relevant relevant to radiation protection from space radiation), and an absorbed dose rate range between nGy/h and a few hundred mGy/h. IDA data acquisition will start soon after HALO launch and will continue on a long term, including transit and on the final halo-like orbit around the Moon. This final orbit will also pass through the Van Allen radiation belts. Operations will be continuous even during uncrewed periods. The scientific radiation data provided by IDA will help the space dosimetry community to improve radiation physics models for cancer and non-cancer (cardio-vascular system, central nervous system) effects. These are of utmost importance in supporting crew risk assessment for deep space exploration missions, not only in the frame of the Artemis programme but for the future plans of human missions to Mars. Radiation data provided by the Instruments will serve also as inputs for studying radiation effects on electronics in deep space. The present paper gives a brief descripton of the scientific instruments in IDA and an overview of the system level concept of the IDA payload to integrate all required instruments within a Gateway Payload Bank and to provide a system interface between the instrumentation and Gateway onboard system from electrical and software point of view. Title: Solar flare prediction with reduced false positives using a hybrid CNN-ERT machine learning model Authors: Berger, Thomas; Flyer, Natasha; Deshmukh, Varad; van der Sande, Kiera Bibcode: 2022AAS...24043102B Altcode: Solar flare prediction using modern machine learning models has been an active field of research for the past several years. Due to the impulsive, episodic, nature of solar flares, the datasets used to train the models, whether from solar magnetic field or atmospheric imaging instruments, are highly imbalanced: there are always many more "non-flare" data than "flare" data for any given prediction window. This dataset imbalance has two major impacts: one, it forces adaption of training algorithms or model parameters that lead to unacceptably high false-positive rates (FPR); and two, it skews the skill metrics used to evaluate predictive performance of any model.
Here we demonstrate a hybrid Convolutional Neural Network (CNN) and Extremely Randomized Trees (ERT) model that is trained and tested on fully imbalanced Solar Dynamics Observatory (SDO) Helioseismic and Magnetic Imager (HMI) vector magnetic field data but which achieves a 48% reduction in FPR relative to traditional single-architecture models for a 12-hour forecasting window. The reduction in FPR is accompanied by only a slight reduction in true positive rate (-12%), leading to a slight decrease in the True Skill Score (TSS), but a large increase in the Heidke Skill Score (HSS) and F1 score. The addition of the ERT stage to the "deep learning" CNN model has the added advantage of enabling ranking of magnetogram features used to achieve a high skill flare prediction. We find that the probability of flaring provided by the CNN model is the most predictive input, followed by the Schrijver R-parameter, measures of magnetic field topological complexity, and then the total unsigned vertical current and helicity. The resulting model could be transitioned to operations to increase the short-term forecasting skill of human-in-the-loop solar flare prediction systems currently in use in space weather forecasting offices. We also demonstrate that the SDO Atmospheric Imaging Assembly (AIA) extreme ultraviolet (EUV) images that are concurrent with the HMI magnetic field data can be used to both replace the NOAA GOES X-ray flare catalog as a source for supervised learning data labels, and as an additional data source for increasing the skill of ML flare prediction models. Title: Decreasing False-alarm Rates in CNN-based Solar Flare Prediction Using SDO/HMI Data Authors: Deshmukh, Varad; Flyer, Natasha; van der Sande, Kiera; Berger, Thomas Bibcode: 2022ApJS..260....9D Altcode: 2021arXiv211110704D A hybrid two-stage machine-learning architecture that addresses the problem of excessive false positives (false alarms) in solar flare prediction systems is investigated. The first stage is a convolutional neural network (CNN) model based on the VGG-16 architecture that extracts features from a temporal stack of consecutive Solar Dynamics Observatory Helioseismic and Magnetic Imager magnetogram images to produce a flaring probability. The probability of flaring is added to a feature vector derived from the magnetograms to train an extremely randomized trees (ERT) model in the second stage to produce a binary deterministic prediction (flare/no-flare) in a 12 hr forecast window. To tune the hyperparameters of the architecture, a new evaluation metric is introduced: the "scaled True Skill Statistic." It specifically addresses the large discrepancy between the true positive rate and the false positive rate in the highly unbalanced solar flare event training data sets. Through hyperparameter tuning to maximize this new metric, our two-stage architecture drastically reduces false positives by ≍48% without significantly affecting the true positives (reduction by ≍12%), when compared with predictions from the first-stage CNN alone. This, in turn, improves various traditional binary classification metrics sensitive to false positives, such as the precision, F1, and the Heidke Skill Score. The end result is a more robust 12 hr flare prediction system that could be combined with current operational flare-forecasting methods. Additionally, using the ERT-based feature-ranking mechanism, we show that the CNN output probability is highly ranked in terms of flare prediction relevance. Title: Zodiacal exoplanets in time (ZEIT) XII: a directly imaged planetary-mass companion to a young Taurus M dwarf star Authors: Gaidos, E.; Hirano, T.; Kraus, A. L.; Kuzuhara, M.; Zhang, Z.; Lee, R. A.; Salama, M.; Berger, T. A.; Grunblatt, S. K.; Ansdell, M.; Liu, M. C.; Harakawa, H.; Hodapp, K. W.; Jacobson, S.; Konishi, M.; Kotani, T.; Kudo, T.; Kurokawa, T.; Nishikawa, J.; Omiya, M.; Serizawa, T.; Tamura, M.; Ueda, A.; Vievard, S. Bibcode: 2022MNRAS.512..583G Altcode: 2021arXiv211008655G; 2021MNRAS.tmp.2819G We report the discovery of a resolved (0.9 arcsec) substellar companion to a member of the 1-5 Myr Taurus star-forming region. The host star (2M0437) is a single mid-M type (Teff ≍ 3100 K) dwarf with a position, space motion, and colour-magnitude that support Taurus membership, and possible affiliation with a ~2.5-Myr-old subgroup. A comparison with stellar models suggests a 2-5 Myr age and a mass of 0.15-0.18M⊙. Although K2 detected quasi-periodic dimming from close-in circumstellar dust, the star lacks detectable excess infrared emission from a circumstellar disc and its H α emission is not commensurate with accretion. Astrometry based on 3 yr of AO imaging shows that the companion (2M0437b) is comoving, while photometry of two other sources at larger separation indicates that they are likely heavily reddened background stars. A comparison of the luminosity of 2M0437b with models suggests a mass of 3-5 MJUP, well below the deuterium burning limit, and an effective temperature of 1400-1500 K, characteristic of a late L spectral type. The H - K colour is redder than the typical L dwarf, but comparable to other directly detected young planets, e.g. those around HR 8799. The discovery of a super-Jupiter around a very young, very low-mass star challenges models of planet formation by either core accretion (which requires time) or disc instability (which requires mass). We also detected a second, comoving, widely separated (75 arcsec) object that appears to be a heavily extincted star. This is certainly a fellow member of this Taurus subgroup and statistically likely to be a bound companion. Title: Passive Radiometry of Subsurface Temperatures Using the Mars 2020 Rimfax Instrument Authors: Siegler, M. A.; White, M. N.; Brovoll, S.; Hamran, S.; Russell, P.; Mellon, M.; Berger, T.; Paige, D. A.; Hausrath, E.; Martinez, G.; Rimfax; Mars 2020 Team Bibcode: 2022LPICo2678.1491S Altcode: We are using a passive radiometry model of the Mars 2020 RIMFAX ground penetrating radar instrument to constrain temperatures and properties of the subsurface. Title: Dielectric Permittivity and Density of the Shallow Martian Subsurface in Jezero Crater Authors: Casademont, T. M.; Hamran, S. -E.; Amundsen, H. E. F.; Eide, S.; Dypvik, H.; Berger, T.; Russell, P. Bibcode: 2022LPICo2678.1513C Altcode: RIMFAX estimates of local radar wave propagation velocity by hyperbola matching. With that, relative dielectric permittivity and bulk rock density are derived. Title: Machine Learning Approaches to Solar-Flare Forecasting: Is Complex Better? Authors: Deshmukh, Varad; Baskar, Srinivas; Bradley, Elizabeth; Berger, Thomas; Meiss, James D. Bibcode: 2022arXiv220208776D Altcode: Recently, there has been growing interest in the use of machine-learning methods for predicting solar flares. Initial efforts along these lines employed comparatively simple models, correlating features extracted from observations of sunspot active regions with known instances of flaring. Typically, these models have used physics-inspired features that have been carefully chosen by experts in order to capture the salient features of such magnetic field structures. Over time, the sophistication and complexity of the models involved has grown. However, there has been little evolution in the choice of feature sets, nor any systematic study of whether the additional model complexity is truly useful. Our goal is to address these issues. To that end, we compare the relative prediction performance of machine-learning-based, flare-forecasting models with varying degrees of complexity. We also revisit the feature set design, using topological data analysis to extract shape-based features from magnetic field images of the active regions. Using hyperparameter training for fair comparison of different machine-learning models across different feature sets, we show that simpler models with fewer free parameters \textit{generally perform better than more-complicated models}, ie., powerful machinery does not necessarily guarantee better prediction performance. Secondly, we find that \textit{abstract, shape-based features contain just as much useful information}, for the purposes of flare prediction, as the set of hand-crafted features developed by the solar-physics community over the years. Finally, we study the effects of dimensionality reduction, using principal component analysis, to show that streamlined feature sets, overall, perform just as well as the corresponding full-dimensional versions. Title: Classification of Solar Flare Magnitudes Using SDO/AIA Movies with 4D Convolutional Neural Networks Authors: van der Sande, Kiera; Berger, Thomas; Flyer, Natasha; Deshmukh, Varad Bibcode: 2021AGUFMNG45B0571V Altcode: Currently, solar flares are labeled with a magnitude based on a single global measurement of the sun -- the peak X-ray intensity over the flaring event, as measured by the GOES satellite. Given that solar flares are local events, human forecasters are then tasked with labeling the active region on the sun associated with the flare. This has potential for errors since it mandates using at least two separate observational systems. Interest has been growing in using imaging instruments to classify flare intensity and location simultaneously. In addition, imaging instruments such as the Solar Dynamics Observatory (SDO) Atmospheric Imaging Assembly (AIA), which provides full-Sun images in ultraviolet and extreme ultraviolet wavelengths, are increasingly used in machine learning (ML) solar flare prediction models, as these images may reveal more features associated with flaring than the photospheric magnetic field data that has been mostly used to date. We demonstrate the use of AIA image cutouts of solar active regions to characterize the peak X-ray magnitude of solar flares via ML regression to the GOES measurements, offering an alternative to using the GOES flare catalog for event location and data labelling. We use a 4D Convolutional Neural Network (CNN) algorithm trained on a temporal series of AIA images in various wavelengths, with the corresponding outputs being the GOES flare magnitude for the event. However, a challenge is that solar flare peak times and the length of flaring vary as a function of wavelength, e.g., the flare peak time in the SDO/AIA 171 Angstrom bandpass (as determined, e.g., by the maximum size of saturated pixels in the flare region) can be as much as 40 minutes after the flare peak in the GOES data). We will address this complication in constructing training databases for the ML algorithm and present preliminary results of our regression modeling. Title: The SWx TREC Space Weather Data Portal: bringing data from diverse sources to the community Authors: Knuth, Jenny; Lucas, Greg; Pankratz, Christopher; Berger, Thomas Bibcode: 2021AGUFMSM52A..08K Altcode: An obstacle to understanding, viewing, and communicating space weather is accessing relevant data. Users spend hours collecting data from disparate sources and repositories. The learning curve for finding relevant data is high, and only the most dedicated make the leap. Datasets are viewed in separate repositories or downloaded and visualized locally with a custom script. It takes specialized skills to bring space weather data together for analysis. This results in space weather often seeming cryptic, invisible, and difficult to grasp. The University of Colorado at Boulders Space Weather Technology, Research, and Education Center (SWx TREC), is working to lower these barriers. SWx TRECs Space Weather Data Portal found at https://lasp.colorado.edu/space-weather-portal, provides uniform access to data housed in various remote repositories. In this presentation I will show how the SWx Data Portal can address the needs of a broad spectrum of end users: from space weather enthusiasts to educators, scientists, and operational professionals. The SWx Data Portal enables users to quickly view and download disparate data relevant to past space weather events, all in one place. The selected data can be easily compared, overplotted, curated, saved, downloaded, and shared. For example, we will demonstrate how the SWx Data Portal can be used to watch the unfolding of a space weather event from its initiation on the Sun to its journey through space to its impacts on the Earth. The relevant coronagraphs and solar images can be easily selected and aligned in time with X-ray flux and particle data. The solar winds speed, density, and temperature along with magnetic field direction and strength can be traced alongside models of satellite drag, D-Region Absorption, and geomagnetically induced currents. All of these data products can be synced and viewed on one screen. Events can be saved, shared, and submitted to the Data Portal's community Event Library. The SWx Data Portal can help bridge the gap between scientists, forecasters, and stakeholders by allowing graphical exploration of space weather data and events. Such tools that connect disparate space weather data will speed understanding and enable clearer communication to policy makers and the public, ultimately protecting against space weathers social and economic impacts. Title: University of Colorado SWx TREC Model Staging Platform: Facilitating Model/Algorithm R2O and O2R Development within a Cloud Computing Environment Authors: Craft, James; Lucas, Greg; Pankratz, Christopher; Berger, Thomas; Sutton, Eric Bibcode: 2021AGUFMSM52A..04C Altcode: The Space Weather Technology, Research and Education Center (SWx TREC) is an emerging national center of excellence in cross-disciplinary research, technology, innovation, and education, intended to facilitate evolving space weather research and forecasting needs. Within this center, we are developing a Space Weather Model Staging Platform (MSP) to facilitate the R2O and O2R pipelines. The MSP leverages cloud computing to provide a managed computational environment for independent science teams to deploy their processing software into an operational-like system. Using cloud computing for the environment enables traditional defined-cadence (daily, hourly) model runs to be scheduled while also providing the ability to submit on-demand runs during storm times with no additional bulk hardware purchases that would otherwise sit idle most of the time. In this presentation, we demonstrate the ways that the MSP is being utilized. First, in the R2O pipeline, we have implemented code from the USGS to produce electric field maps at a set cadence to demonstrate that the code can be run in an operational mode. Second, in the O2R pipeline, we are taking operational codes such as the Enlil Solar Wind Model and the NOAA Whole Atmosphere Model (WAM), and enabling researchers to investigate new data assimilation techniques that can supplement and enhance current operational code capabilities. Finally, we demonstrate the use of cloud resources to generate automatic flare forecasts from satellite images. Title: A New Interactive 3-Dimensional Data Viewer for the Enlil Solar Wind Model Authors: Pankratz, Christopher; Lucas, Greg; Knuth, Jenny; Odstrcil, Dusan; Craft, James; Berger, Thomas Bibcode: 2021AGUFMSM53B..05P Altcode: One of the critical models in space weather forecasting is the Enlil solar wind prediction model that can inform space weather forecasters the direction and speed of coronal mass ejections CMEs. The Enlil code calculates the propagation of the solar wind throughout the 3D heliosphere, but current visualization capabilities in the forecasting offices are restricted to 2D planes intersecting Earth. This limits forecasters to only be able to view CME properties that are traveling directly in the plane of the Earth. Here, we present a new visualization capability being developed to take advantage of the full Enlil 3D data volume and interactively visualize the CME expansion out of the plane of the Earth. This is designed to give forecasters and researchers the full view of the heliosphere in a manner that can be tailored to these different types of users. To accomplish this, we are deploying the Enlil solar wind model into a scalable Cloud-based model staging platform computing environment, which will allow the full 3D Enlil output to reside in-situ with the visualization engine. We will discuss our progress in deploying and running the Enlil model in the Cloud-based testbed environment, the process of interacting with space weather forecasters to design a new interactive 3D visualization tool that meets their needs, and will demonstrate use of the visualization tool itself. Title: From 1973 to the 2020s, from SKYLAB to 3D vector magnetic fields in prominences Authors: Lacatus, Daniela; Judge, Philip; Gilbert, Holly; Paraschiv, Alin; Berger, Thomas Bibcode: 2021AGUFMSH42B..05L Altcode: Routine measurement of the vector magnetic fields threading prominences would mark a significant advance in our ability to determine the dynamics of the Sun's corona. Gilbert et al. (AGU abstract #849653) have identified the near-UV (250-281 nm) as a prime region for measurements of magnetic fields within the chromosphere and lower transition region. Here, we perform an in depth analysis of the near UV spectra of all prominences observed by the SKYLAB SO82B instrument during 1973, for the first time. Using over 100 spectral lines we process the photographic data from scratch, and solve for plasma properties of several prominences. Given the known complexity of the thermal and dynamical conditions within prominence plasma, we develop a model to find mean electron temperatures, densities and mass columns which capture each spectrums essential characteristics. Prominence plasmas are optically thick in the cores of many spectral lines of Fe II and Mg II present in this spectral region. The different optical depths probe different surfaces along the line-of-sight, so that near-UV spectro-polarimetry will uniquely determine vector magnetic fields within the 3D volume of prominences. Therefore, we show that this technique offers the best future method for answering critical problems related to coronal dynamics, not only above active regions as shown by Gilbert et al., but also in prominence plasmas. Title: New Insights into the Martian Radiation Environment gained with the MSL/RAD Investigation Authors: Ehresmann, Bent; Hassler, Don; Zeitlin, Cary; Wimmer-Schweingruber, Robert; Loeffler, Sven; Guo, Jingnan; Khaksarighiri, Salman; Matthiae, Daniel; Berger, Thomas; Reitz, Gunther Bibcode: 2021AGUFM.P24A..02E Altcode: The Mars Science Laboratory / Radiation Assessment Detector (MSL/RAD) has been conducting detailed measurements of the radiation environment in Gale crater on Mars for more than 9 years. Understanding of this radiation field, its composition, and its temporal evolution are vital for the preparation of human exploration missions to Mars. Thereby, protecting astronauts from the effects of space radiation remains a critical step for the exploration of Mars. Long-term exposure to radiation can lead to severe health effects and affects allowable mission duration. Astronauts need to be protected from exposure to both the long-term Galactic Cosmic Ray (GCR)-induced radiation, as well as from short-term, but highly intense Solar Energetic Particles (SEPs). Here, we provide new insights into the changes the Martian radiation field has undergone since the beginning of the MSL mission in mid-2012 (close to solar maximum of solar cycle 24) throughout the deepest part of the solar minimum of cycle 24. We present how the evolving solar cycle has affected dosimetric quantities, such as the RAD-measured absorbed dose rate, Linear Energy Transfer (LET) spectrum, and the biologically highly-important dose equivalent rate. From these measurements, we make estimates of how much radiation astronauts would be exposed to under different mission scenarios and timing. Furthermore, we present new analysis of the natural radiation shielding effect of Martian terrain, measured for the first-time in-situ by MSL/RAD. We find that natural terrain, such as cliff sides or buttes, when high enough, block out part of the incoming GCR radiation, leading to an overall decrease in the measured dose rate. We present data from 5 occasions where such a shielding effect was observed by MSL/RAD and analyze how the angle of vertical obstruction of the natural terrain affects the measured decrease in dose. These first-ever in-situ measurements of the radiation shielding effect are crucial for the planning of radiation shelters for future Mars explorers by providing insight into the angular distribution of the radiation environment on the Martian surface. These measurements are vital to validate radiation transport models used to calculate the effectiveness of proposed radiation shelter designs. Title: Directionality of the Martian Surface Radiation and Derivation of the Upward Albedo Radiation Authors: Guo, Jingnan; Khaksarighiri, Salman; Wimmer-Schweingruber, Robert F.; Hassler, Donald M.; Ehresmann, Bent; Zeitlin, Cary; Löffler, Sven; Matthiä, Daniel; Berger, Thomas; Reitz, Günther; Calef, Fred Bibcode: 2021GeoRL..4893912G Altcode: Since 2012 August, the Radiation Assessment Detector (RAD) on the Curiosity rover has been characterizing the Martian surface radiation field which is essential in preparation for future crewed Mars missions. RAD observed radiation dose is influenced by variable topographical features as the rover traverses through the terrain. In particular, while Curiosity was parked near a butte in the Murray Buttes area, we find a decrease of the dose rate by (5 ± 1)% as 19% of the sky was obstructed, versus 10% in an average reference period. Combining a zenith-angle-dependent radiation model and the rover panoramic visibility map leads to a predicted reduction of the downward dose by ∼12% due to the obstruction, larger than the observed decrease. With the hypothesis that this difference is attributable to albedo radiation coming from the butte, we estimate the (flat-terrain) albedo radiation to be about 19% of the total surface dose. Title: Measuring the Magnetic Origins of Solar Flares, Coronal Mass Ejections, and Space Weather Authors: Judge, Philip; Rempel, Matthias; Ezzeddine, Rana; Kleint, Lucia; Egeland, Ricky; Berdyugina, Svetlana V.; Berger, Thomas; Bryans, Paul; Burkepile, Joan; Centeno, Rebecca; de Toma, Giuliana; Dikpati, Mausumi; Fan, Yuhong; Gilbert, Holly; Lacatus, Daniela A. Bibcode: 2021ApJ...917...27J Altcode: 2021arXiv210607786J We take a broad look at the problem of identifying the magnetic solar causes of space weather. With the lackluster performance of extrapolations based upon magnetic field measurements in the photosphere, we identify a region in the near-UV (NUV) part of the spectrum as optimal for studying the development of magnetic free energy over active regions. Using data from SORCE, the Hubble Space Telescope, and SKYLAB, along with 1D computations of the NUV spectrum and numerical experiments based on the MURaM radiation-magnetohydrodynamic and HanleRT radiative transfer codes, we address multiple challenges. These challenges are best met through a combination of NUV lines of bright Mg II, and lines of Fe II and Fe I (mostly within the 4s-4p transition array) which form in the chromosphere up to 2 × 104 K. Both Hanle and Zeeman effects can in principle be used to derive vector magnetic fields. However, for any given spectral line the τ = 1 surfaces are generally geometrically corrugated owing to fine structure such as fibrils and spicules. By using multiple spectral lines spanning different optical depths, magnetic fields across nearly horizontal surfaces can be inferred in regions of low plasma β, from which free energies, magnetic topology, and other quantities can be derived. Based upon the recently reported successful sub-orbital space measurements of magnetic fields with the CLASP2 instrument, we argue that a modest space-borne telescope will be able to make significant advances in the attempts to predict solar eruptions. Difficulties associated with blended lines are shown to be minor in an Appendix. Title: VizieR Online Data Catalog: A list of ~330000 stars Kepler missed (Wolniewicz+, 2021) Authors: Wolniewicz, L. M.; Berger, T. A.; Huber, D. Bibcode: 2021yCat..51610231W Altcode: In this paper we have analyzed the Kepler mission's target selection function by using Gaia DR2 as the ground truth to characterize the ~500000 stars that Kepler could have observed, and compared this population to the sample of ~200000 stars that were selected for observations. We started with a subset of 2.4million targets within the KIC that are located in the Kepler field of view, which we downloaded from the Mikulski Archive for Space Telescopes (MAST). As a first step, we cross-matched the KIC with Gaia DR2 to obtain Gaia information for each star in the KIC. To do this, we used the Centre de Donnees astronomiques de Strasbourg (CDS) cross-match. We conducted a positional match with a matching radius of 5", because the astrometric offsets between the KIC and Gaia have not been well characterized. We removed duplicates by only selecting the Kepler and Gaia ID associated with the most similar magnitudes in the Kepler passband Kp and Gaia passband. We then extracted Gaia Re-normalized unit weight error (RUWE) values for all sources. (1 data file). Title: Solar Prominence Bubbles and Associated Plasma Instabilities: IRIS and SDO/AIA Observations Authors: Liu, W.; Berger, T. Bibcode: 2021AAS...23811311L Altcode: Solar prominences are cool and dense plasma in the hot corona. The so-called prominence bubbles are mysterious, dome-shaped, apparently void structures residing in the lower portions of prominences. Such bubbles are associated with various plasma instabilities, such as the Rayleigh-Taylor (RT) and Kelvin-Helmholtz (KH) instabilities. The former is manifested in plumes that are often produced at the top boundary of a bubble and intrude upward into the dense prominence material. The latter is found to be triggered by shear flows at the bubble boundaries. We present recent observations of prominence bubbles by IRIS and SDO/AIA, focusing on the diagnostic potential of RT and KH instabilities on the physical conditions of the prominence and its supporting magnetic field. We search for evidence of magnetic flux emergence as the origin of prominence bubbles. We discuss their role in mass ad magnetic flux transport in the solar atmosphere. Title: Rotation Distributions around the Kraft Break with TESS and Kepler: The Influences of Mass, Metallicity, and Binarity Authors: Avallone, E. A.; Tayar, J.; Van Saders, J.; Berger, T.; Claytor, Z. Bibcode: 2021AAS...23831407A Altcode: The year-long lightcurves observed in the southern continuous viewing zone (SCVZ) of the Transiting Exoplanet Survey Satellite (TESS) and the abundance of rotation periods measured with the Kepler Space Telescope provide the ideal laboratory to understand stellar rotation across the main sequence. Here, we find that while we can measure rotation periods from lightcurves in the TESS SCVZ and use TESS lightcurves to identify other classes of stellar variability (e.g. pulsations), instrument systematics prevent the detection of rotation signals longer than the TESS orbital period of 13.7 days. Due to this detection limit, we combine more traditional methods of measuring rotation from spectroscopic data with data from TESS and Kepler to conduct our analysis. Using rotation periods derived from rotational velocities measured by the APOGEE spectroscopic survey and radii inferred using the Gaia mission, we find that we can trace rotation as a function of evolutionary state and analyze the distribution of rotation periods as a function of binarity around the Kraft Break. Additionally, the distribution of detected stars in Kepler and TESS reveals key differences between stellar populations probed by these two missions, with TESS probing a significant population of young stars that were not present in the Kepler sample. Title: Critical Science Plan for the Daniel K. Inouye Solar Telescope (DKIST) Authors: Rast, Mark P.; Bello González, Nazaret; Bellot Rubio, Luis; Cao, Wenda; Cauzzi, Gianna; Deluca, Edward; de Pontieu, Bart; Fletcher, Lyndsay; Gibson, Sarah E.; Judge, Philip G.; Katsukawa, Yukio; Kazachenko, Maria D.; Khomenko, Elena; Landi, Enrico; Martínez Pillet, Valentín; Petrie, Gordon J. D.; Qiu, Jiong; Rachmeler, Laurel A.; Rempel, Matthias; Schmidt, Wolfgang; Scullion, Eamon; Sun, Xudong; Welsch, Brian T.; Andretta, Vincenzo; Antolin, Patrick; Ayres, Thomas R.; Balasubramaniam, K. S.; Ballai, Istvan; Berger, Thomas E.; Bradshaw, Stephen J.; Campbell, Ryan J.; Carlsson, Mats; Casini, Roberto; Centeno, Rebecca; Cranmer, Steven R.; Criscuoli, Serena; Deforest, Craig; Deng, Yuanyong; Erdélyi, Robertus; Fedun, Viktor; Fischer, Catherine E.; González Manrique, Sergio J.; Hahn, Michael; Harra, Louise; Henriques, Vasco M. J.; Hurlburt, Neal E.; Jaeggli, Sarah; Jafarzadeh, Shahin; Jain, Rekha; Jefferies, Stuart M.; Keys, Peter H.; Kowalski, Adam F.; Kuckein, Christoph; Kuhn, Jeffrey R.; Kuridze, David; Liu, Jiajia; Liu, Wei; Longcope, Dana; Mathioudakis, Mihalis; McAteer, R. T. James; McIntosh, Scott W.; McKenzie, David E.; Miralles, Mari Paz; Morton, Richard J.; Muglach, Karin; Nelson, Chris J.; Panesar, Navdeep K.; Parenti, Susanna; Parnell, Clare E.; Poduval, Bala; Reardon, Kevin P.; Reep, Jeffrey W.; Schad, Thomas A.; Schmit, Donald; Sharma, Rahul; Socas-Navarro, Hector; Srivastava, Abhishek K.; Sterling, Alphonse C.; Suematsu, Yoshinori; Tarr, Lucas A.; Tiwari, Sanjiv; Tritschler, Alexandra; Verth, Gary; Vourlidas, Angelos; Wang, Haimin; Wang, Yi-Ming; NSO and DKIST Project; DKIST Instrument Scientists; DKIST Science Working Group; DKIST Critical Science Plan Community Bibcode: 2021SoPh..296...70R Altcode: 2020arXiv200808203R The National Science Foundation's Daniel K. Inouye Solar Telescope (DKIST) will revolutionize our ability to measure, understand, and model the basic physical processes that control the structure and dynamics of the Sun and its atmosphere. The first-light DKIST images, released publicly on 29 January 2020, only hint at the extraordinary capabilities that will accompany full commissioning of the five facility instruments. With this Critical Science Plan (CSP) we attempt to anticipate some of what those capabilities will enable, providing a snapshot of some of the scientific pursuits that the DKIST hopes to engage as start-of-operations nears. The work builds on the combined contributions of the DKIST Science Working Group (SWG) and CSP Community members, who generously shared their experiences, plans, knowledge, and dreams. Discussion is primarily focused on those issues to which DKIST will uniquely contribute. Title: RIMFAX GPR on the MARS 2020 Investigation at Jezero Crater Authors: Hamran, S. -E.; Paige, D. A.; Amundsen, H. E. F.; Berger, T.; Brovoll, S.; Carter, L.; Damsgård, L.; Dypvik, H.; Eide, S.; Ghent, R.; Kohler, J.; Mellon, M.; Nunes, D. C.; Plettemeier, D.; Russell, P. Bibcode: 2021LPI....52.1223H Altcode: The Radar Imager for Mars' Subsurface Experiment (RIMFAX) is a Ground Penetrating Radar on the Mars 2020 mission's Perseverance rover, which is planned to land in Jezero Crater on February 18, 2021. Title: VizieR Online Data Catalog: 117 exoplanets in habitable zone with Kepler DR25 (Bryson+, 2021) Authors: Bryson, S.; Kunimoto, M.; Kopparapu, R. K.; Coughlin, J. L.; Borucki, W. J.; Koch, D.; Aguirre, V. S.; Allen, C.; Barentsen, G.; Batalha, N. M.; Berger, T.; Boss, A.; Buchhave, L. A.; Burke, C. J.; Caldwell, D. A.; Campbell, J. R.; Catanzarite, J.; Chandrasekaran, H.; Chaplin, W. J.; Christiansen, J. L.; Christensen-Dalsgaard, J.; Ciardi, D. R.; Clarke, B. D.; Cochran, W. D.; Dotson, J. L.; Doyle, L. R.; Duarte, E. S.; Dunham, E. W.; Dupree, A. K.; Endl, M.; Fanson, J. L.; Ford, E. B.; Fujieh, M.; Gautier, T. N., III; Geary, J. C.; Gilliland, R. L.; Girouard, F. R.; Gould, A.; Haas, M. R.; Henze, C. E.; Holman, M. J.; Howard, A. W.; Howell, S. B.; Huber, D.; Hunter, R. C.; Jenkins, J. M.; Kjeldsen, H.; Kolodziejczak, J.; Larson, K.; Latham, D. W.; Li, J.; Mathur, S.; Meibom, S.; Middour, C.; Morris, R. L.; Morton, T. D.; Mullally, F.; Mullally, S. E.; Pletcher, D.; Prsa, A.; Quinn, S. N.; Quintana, E. V.; Ragozzine, D.; Ramirez, S. V.; Sanderfer, D. T.; Sasselov, D.; Seader, S. E.; Shabram, M.; Shporer, A.; Smith, J. C.; Steffen, J. H.; Still, M.; Torres, G.; Troeltzsch, J.; Twicken, J. D.; Uddin, A. K.; van Cleve, J. E.; Voss, J.; Weiss, L. M.; Welsh, W. F.; Wohler, B.; Zamudio, K. A. Bibcode: 2021yCat..51610036B Altcode: We present the occurrence rates for rocky planets in the habitable zones (HZs) of main-sequence dwarf stars based on the Kepler DR25 planet candidate catalog and Gaia-based stellar properties. We provide the first analysis in terms of star-dependent instellation flux, which allows us to track HZ planets. We define {eta}{Earth} as the HZ occurrence of planets with radii between 0.5 and 1.5 R{Earth} orbiting stars with effective temperatures between 4800 and 6300K. We find that {eta}{Earth} for the conservative HZ is between 0.37-0.21+0.48 (errors reflect 68% credible intervals) and 0.60-0.36+0.90 planets per star, while the optimistic HZ occurrence is between 0.58-0.33+0.73 and 0.88-0.51+1.28 planets per star. These bounds reflect two extreme assumptions about the extrapolation of completeness beyond orbital periods where DR25 completeness data are available. The large uncertainties are due to the small number of detected small HZ planets. We find similar occurrence rates between using Poisson likelihood Bayesian analysis and using Approximate Bayesian Computation. Our results are corrected for catalog completeness and reliability. Both completeness and the planet occurrence rate are dependent on stellar effective temperature. We also present occurrence rates for various stellar populations and planet size ranges. We estimate with 95% confidence that, on average, the nearest HZ planet around G and K dwarfs is ~6pc away and there are ~4 HZ rocky planets around G and K dwarfs within 10pc of the Sun. (1 data file). Title: The Stars Kepler Missed: Investigating the Biases Behind the Kepler Target Selection Function Authors: Wolniewicz, L. M.; Berger, T.; Huber, D. Bibcode: 2021AAS...23721104W Altcode: The Kepler Mission revolutionized exoplanet science by obtaining highly precise photometry of 170,000 stars over 4 years. A critical piece of information needed to accurately exploit Kepler data is the Kepler selection function, since nearly 200,000 targets had to be selected for observation from a sample of over a million stars positioned over the Kepler CCDs with minimal information of their evolutionary state, stellar multiplicity, or proper motions. In this talk I will explain how I use Gaia DR2 to reconstruct the Kepler selection function and explore its biases with respect to evolutionary state, stellar multiplicity, and proper motions. By comparing the stars positioned on the Kepler CCDs that were not chosen for observation to those that were, I will present the first evaluation of the biases of the Kepler target selection function. I find that Kepler was complete for stars brighter than Kp = 14 magnitude, unbiased with respect to proper motions, and that the selection function shows some bias against stellar multiplicity, in the sense that stars without companions were preferentially selected for observation. Title: Precise Demographics of Kepler Planets in the Gaia Era Authors: Berger, T. A.; Huber, D.; Van Saders, J.; Gaidos, E.; Tayar, J.; Weiss, L.; Kraus, A. Bibcode: 2021AAS...23731703B Altcode: A major bottleneck for transiting exoplanet demographics has been the lack of precise properties for most of the observed stars, as the transit method measures exoplanet radii relative to their host's radii. We live in a golden era of host star characterization because of access to Gaia Data Release 2 (DR2) photometry, parallaxes, and proper motions, large-scale spectroscopic surveys, and ground-based photometric and spectroscopic follow-up. In this talk, I will present a sharpened view of Kepler exoplanet demographics using Gaia DR2 parallaxes. First, I will present a comprehensive classification of main sequence, subgiant, and giant stars in Kepler target sample. Using revised planet radii and incident fluxes, I will identify the planet radius gap, planets within the hot sub-Neptunian desert, the hot Jupiter inflation trend, and present an updated census of habitable zone planets. I will also present the Gaia-Kepler Stellar Properties Catalog, the first homogeneous Kepler catalog to include stellar ages, in addition to precise radii, masses, and mean stellar densities for Kepler target stars. I will reveal the first observational evidence of a stellar age dependence of the planet radius gap, where sub-Neptunes become super-Earths on roughly Gyr timescales. In addition, I will show that the planet radius valley exhibits a stellar mass dependence and provide stringent constraints that will be required to discern between the theories of core-powered mass-loss and photoevaporation. Finally, I will reveal that most planets within the hot sub-Neptunian desert only entered recently because of their host's evolution, identify Jupiters with large radii at low incident fluxes, and demonstrate that planets in single and multiple transiting systems share the same age distribution. Title: On Cooling Condensation Near Magnetic Null Points and the Formation of Solar Coronal Rain and Prominences Authors: Liu, Wei; Titov, Viacheslav; Downs, Cooper; Antolin, Patrick; Luna, Manuel; Sun, Xudong; Berger, Thomas; Yu, Sijie; Yoffe, Luke Bibcode: 2021cosp...43E.975L Altcode: The Sun's outer atmosphere, the corona, is million-degrees hot and tenuous. Such hot plasma, under certain conditions, can enigmatically undergo a radiative cooling instability and condense into material of 100 times cooler in the form of coronal rain or prominences. Where, when, and how such cooling condensation takes place remain poorly understood. Answers to these questions are not only important in their own right, but also bear implications for the fundamental question of coronal heating and the chromosphere-corona mass cycle. Magnetic fields in the magnetized corona undoubtedly play a crucial role (e.g., by trapping the plasma), but where and how? We report recent imaging and spectroscopic observations from SDO/AIA/HMI and IRIS that can shed light on this puzzle. Through a systematic survey, we found that a large fraction of quiet-Sun condensations preferentially occur at the dips of coronal loops or funnels. Such dips are located at/near magnetic topological features, such as null points and quasi-separatrix layers (QSLs), which are regions characterized by high values of the squashing factor. We also identified evidence of magnetic reconnection at such locations, which can produce favorable conditions, e.g., density enhancement by compression and/or mass trapping in plasmoids, that can trigger run-away radiative cooling. We present proof-of-concept MHD simulations that demonstrate the role of reconnection in transporting cooled mass from overlying, long loops to underlying, short loops where it slides down as coronal rain. We will discuss the significance and broader implications of these results beyond the Sun. Title: The Dosis 3d Project On-Board the International Space Station - Status and Science Overview of 8 Years of Measurements (2012 - 2020) Authors: Berger, Thomas; Burmeister, Soenke Bibcode: 2021cosp...43E1878B Altcode: The radiation environment encountered in space differs in nature from that on Earth, consisting mostly of highly energetic ions from protons up to iron, resulting in radiation levels far exceeding the ones present on Earth for occupational radiation workers. Since the beginning of the space era the radiation exposure during space missions has been monitored with various passive and active radiation instruments. Also on-board the International Space Station (ISS) a number of area monitoring devices provide data related to the spatial and temporal variation of the radiation field in - and outside the ISS. The aim of the DOSIS 3D (2012 - ongoing) experiment is the measurement of the radiation environment within the European Columbus Laboratory of the ISS. These measurements are, on the one hand, performed with passive radiation detectors mounted at eleven locations within Columbus for the determination of the spatial distribution of the radiation field parameters and, on the other hand, with two active radiation detectors (DOSTEL) mounted at a fixed position inside Columbus for the determination of the temporal variation of the radiation field parameters. The talk will give an overview of the current results of the data evaluation performed for the passive and active radiation detectors for DOSIS 3D in the years 2012 to 2020 and further focus on the work in progress for data comparison with other passive and active radiation detector systems measuring on-board the ISS. Acknowledgments: The participation of the Technische Universität Wien, Atominstitut (ATI), Vienna, Austria in the DOSIS-1 and -2 experiments was supported by the Austrian Space Applications Programme (ASAP) under contract no. 819643. The Polish contribution for the Institute of Nuclear Physics (IFJ), Krakow, Poland was supported by the National Science Center (project No DEC-2012/06/M/ST9/00423). MTA EK greatly acknowledges the possibility to participate in the project to DLR and to the ESA PECS for the financial grant No. PECS4000108464. The participation of the Nuclear Physics Institute of the Czech Academy of Sciences has been supported by the grant of Czech Science Foundation (GACR) No. 15-16622Y. The CAU, University of Kiel was supported by DLR under grants 50WB0826, 50WB1026, 50WB1232, 50WB1533 and 50WB1817. Title: A New Interactive 3-Dimensional Data Viewer for the Enlil Solar Wind Model Authors: Pankratz, C. K.; Lucas, G.; Odstrcil, D.; Craft, J.; Knuth, J.; Berger, T. E. Bibcode: 2020AGUFMSH0030017P Altcode: One of the critical models in space weather forecasting is the Enlil solar wind prediction model that can inform space weather forecasters the direction and speed of coronal mass ejections CMEs. The Enlil code calculates the propagation of the solar wind throughout the 3D heliosphere, but current visualization capabilities in the forecasting offices are restricted to 2D planes intersecting Earth. This limits forecasters to only be able to view CME properties that are traveling directly in the plane of the Earth. Here, we present a new visualization capability being developed to take advantage of the full Enlil 3D data volume and visualize the CME expansion out of the plane of the Earth that is designed to give forecasters the full view of the heliosphere. We will discuss our initial progress in deploying and running the Enlil model in an on-demand mode in a Cloud-based Testbed and will also describe the process of interacting with space weather forecasters to design a tool that meets their needs. Title: Solar Prominence Bubbles and Associated Plasma Instabilities: IRIS Observations and MHD Modeling Authors: Liu, W.; Berger, T. E.; Fan, Y. Bibcode: 2020AGUFMSH0010014L Altcode: Solar prominences are cool and dense plasma in the hot corona. The so-called prominence bubbles are mysterious, dome-shaped, apparently void structures residing in the lower portions of prominences. Such bubbles are associated with various plasma instabilities, such as the Rayleigh-Taylor (RT) and Kelvin-Helmholtz (KH) instabilities. The former is manifested in plumes that are often produced at the top boundary of a bubble and intrude upward into the dense prominence material. The latter is found to be triggered by shear flows at the bubble boundaries. We present recent observations of prominence bubbles by IRIS, focusing on the diagnostic potential of RT and KH instabilities on the physical conditions of the prominence and its supporting magnetic field. We search for evidence of magnetic flux emergence as the origin of prominence bubbles. We also present preliminary 3D MHD simulations of the interaction of a bipole, as a hypothetical bubble, emerging into an overlying prominence-carrying flux-rope system. The simulations can provide further clues to the origin and nature of prominence bubbles. We discuss their roll in mass ad magnetic flux transport in the solar atmosphere. Title: A Cloud-based Testbed environment to help make models more "useful" Authors: Lucas, G.; Pankratz, C. K.; Craft, J.; Knuth, J.; Berger, T. E. Bibcode: 2020AGUFMSA0040001L Altcode: In the quote "All models are wrong, but some are useful", a key point is that a model has to be made useful to the community in some way, even if it may be "wrong". Here, we present a new Cloud-based Modeling Testbed environment that is designed to help fill in the missing "useful" piece when transitioning research models into operational frameworks. We define the usefulness of the models by iteratively engaging with the end-user, space weather forecasters and researchers, during model development to assure that the end product meets the needs of the community. We will present several specific examples of research codes that we have transitioned to running in the Cloud and made available to the public and how community and user feedback has led to a better end product. Title: SWx TREC's Space Weather Data Portal: a launch pad for space weather research Authors: Knuth, J.; Lucas, G.; Pankratz, C. K.; Berger, T. E.; Clark, R. D.; Skov, T. M. Bibcode: 2020AGUFMSM0030018K Altcode: One obstacle to space weather research is the practical challenge of accessing relevant data. Space weather data are housed in disparate repositories, each with its own unique focus , be it solar, magnetospheric, atmospheric , or earth-based. Much of the effort spent acquiring data could instead be spent on space weather research and education. To address this problem, the Space Weather Technology, Research, and Education Center (SWx TREC), at the University of Colorado, Boulder, in collaboration with the Laboratory for Atmospheric and Space Physics (LASP), has developed the Space Weather Data Portal (https://lasp.colorado.edu/space-weather-portal), a tool built by and for the space weather community. Through the Data Portal, previously dispersed space weather data are in one unified place, accessible to scientists, students, and curious individuals. The focus is on the users and their ability to discover, display, compare, overplot, and download relevant data. A user can filter for past events then easily display and download data related to that event, from the moment it occurs on the Sun, as it travels through space and the atmosphere, to the impacts it has on the Earth. Analysis of space weather events via the Data Portal has proved useful for forecaster training and online learning. The community-created Event Library is a short-cut to curated data collections that provide narratives for context and serve as launch pads for further space weather exploration. Title: Detecting spatiotemporal correlation in microflares for improved solar eruption forecasting Authors: Berger, T. E.; Deshmukh, V.; Flyer, N.; Poduval, B. Bibcode: 2020AGUFMSM047..04B Altcode: No abstract at ADS Title: Shape-based Feature Engineering for Solar Flare Prediction Authors: Deshmukh, Varad; Berger, Thomas; Meiss, James; Bradley, Elizabeth Bibcode: 2020arXiv201214405D Altcode: Solar flares are caused by magnetic eruptions in active regions (ARs) on the surface of the sun. These events can have significant impacts on human activity, many of which can be mitigated with enough advance warning from good forecasts. To date, machine learning-based flare-prediction methods have employed physics-based attributes of the AR images as features; more recently, there has been some work that uses features deduced automatically by deep learning methods (such as convolutional neural networks). We describe a suite of novel shape-based features extracted from magnetogram images of the Sun using the tools of computational topology and computational geometry. We evaluate these features in the context of a multi-layer perceptron (MLP) neural network and compare their performance against the traditional physics-based attributes. We show that these abstract shape-based features outperform the features chosen by the human experts, and that a combination of the two feature sets improves the forecasting capability even further. Title: Evidence for Top Quark Production in Nucleus-Nucleus Collisions Authors: Sirunyan, A. M.; Tumasyan, A.; Adam, W.; Ambrogi, F.; Bergauer, T.; Dragicevic, M.; Erö, J.; Escalante Del Valle, A.; Frühwirth, R.; Jeitler, M.; Krammer, N.; Lechner, L.; Liko, D.; Madlener, T.; Mikulec, I.; Rad, N.; Schieck, J.; Schöfbeck, R.; Spanring, M.; Templ, S.; Waltenberger, W.; Wulz, C. -E.; Zarucki, M.; Chekhovsky, V.; Litomin, A.; Makarenko, V.; Suarez Gonzalez, J.; Darwish, M. R.; De Wolf, E. A.; Di Croce, D.; Janssen, X.; Kello, T.; Lelek, A.; Pieters, M.; Rejeb Sfar, H.; Van Haevermaet, H.; Van Mechelen, P.; Van Putte, S.; Van Remortel, N.; Blekman, F.; Bols, E. S.; Chhibra, S. S.; D'Hondt, J.; De Clercq, J.; Lontkovskyi, D.; Lowette, S.; Marchesini, I.; Moortgat, S.; Python, Q.; Tavernier, S.; Van Doninck, W.; Van Mulders, P.; Beghin, D.; Bilin, B.; Clerbaux, B.; De Lentdecker, G.; Delannoy, H.; Dorney, B.; Favart, L.; Grebenyuk, A.; Kalsi, A. 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M.; Jayananda, MK; Kailasapathy, B.; Sonnadara, D. U. J.; Wickramarathna, DDC; Dharmaratna, W. G. D.; Liyanage, K.; Perera, N.; Wickramage, N.; Aarrestad, T. K.; Abbaneo, D.; Akgun, B.; Auffray, E.; Auzinger, G.; Baechler, J.; Baillon, P.; Ball, A. 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J.; Lammel, S.; Lewis, J.; Lincoln, D.; Lipton, R.; Liu, M.; Liu, T.; Lykken, J.; Maeshima, K.; Mason, D.; McBride, P.; Merkel, P.; Mrenna, S.; Nahn, S.; O'Dell, V.; Papadimitriou, V.; Pedro, K.; Pena, C.; Prokofyev, O.; Ravera, F.; Reinsvold Hall, A.; Ristori, L.; Schneider, B.; Sexton-Kennedy, E.; Smith, N.; Soha, A.; Spalding, W. J.; Spiegel, L.; Stoynev, S.; Strait, J.; Taylor, L.; Tkaczyk, S.; Tran, N. V.; Uplegger, L.; Vaandering, E. W.; Wang, M.; Weber, H. A.; Woodard, A.; Acosta, D.; Avery, P.; Bourilkov, D.; Cadamuro, L.; Cherepanov, V.; Errico, F.; Field, R. D.; Guerrero, D.; Joshi, B. M.; Kim, M.; Konigsberg, J.; Korytov, A.; Lo, K. H.; Matchev, K.; Menendez, N.; Mitselmakher, G.; Rosenzweig, D.; Shi, K.; Wang, J.; Wang, S.; Zuo, X.; Joshi, Y. R.; Adams, T.; Askew, A.; Diaz, D.; Habibullah, R.; Hagopian, S.; Hagopian, V.; Johnson, K. F.; Khurana, R.; Kolberg, T.; Martinez, G.; Prosper, H.; Schiber, C.; Yohay, R.; Zhang, J.; Baarmand, M. M.; Butalla, S.; Elkafrawy, T.; Hohlmann, M.; Noonan, D.; Rahmani, M.; Saunders, M.; Yumiceva, F.; Adams, M. R.; Apanasevich, L.; Becerril Gonzalez, H.; Cavanaugh, R.; Chen, X.; Dittmer, S.; Evdokimov, O.; Gerber, C. E.; Hangal, D. A.; Hofman, D. J.; Mills, C.; Oh, G.; Roy, T.; Tonjes, M. B.; Varelas, N.; Viinikainen, J.; Wang, H.; Wang, X.; Wu, Z.; Alhusseini, M.; Bilki, B.; Dilsiz, K.; Durgut, S.; Gandrajula, R. P.; Haytmyradov, M.; Khristenko, V.; Köseyan, O. K.; Merlo, J. -P.; Mestvirishvili, A.; Moeller, A.; Nachtman, J.; Ogul, H.; Onel, Y.; Ozok, F.; Penzo, A.; Snyder, C.; Tiras, E.; Wetzel, J.; Yi, K.; Amram, O.; Blumenfeld, B.; Corcodilos, L.; Eminizer, M.; Gritsan, A. V.; Kyriacou, S.; Maksimovic, P.; Mantilla, C.; Roskes, J.; Swartz, M.; Vámi, T. Á.; Baldenegro Barrera, C.; Baringer, P.; Bean, A.; Bylinkin, A.; Isidori, T.; Khalil, S.; King, J.; Krintiras, G.; Kropivnitskaya, A.; Lindsey, C.; Mcbrayer, W.; Minafra, N.; Murray, M.; Rogan, C.; Royon, C.; Sanders, S.; Schmitz, E.; Tapia Takaki, J. D.; Wang, Q.; Williams, J.; Wilson, G.; Duric, S.; Ivanov, A.; Kaadze, K.; Kim, D.; Maravin, Y.; Mendis, D. R.; Mitchell, T.; Modak, A.; Mohammadi, A.; Rebassoo, F.; Wright, D.; Adams, E.; Baden, A.; Baron, O.; Belloni, A.; Eno, S. C.; Feng, Y.; Hadley, N. J.; Jabeen, S.; Jeng, G. Y.; Kellogg, R. G.; Koeth, T.; Mignerey, A. C.; Nabili, S.; Seidel, M.; Skuja, A.; Tonwar, S. C.; Wang, L.; Wong, K.; Abercrombie, D.; Allen, B.; Bi, R.; Brandt, S.; Busza, W.; Cali, I. A.; Chen, Y.; D'Alfonso, M.; Gomez Ceballos, G.; Goncharov, M.; Harris, P.; Hsu, D.; Hu, M.; Klute, M.; Kovalskyi, D.; Krupa, J.; Lee, Y. -J.; Luckey, P. D.; Maier, B.; Marini, A. C.; Mcginn, C.; Mironov, C.; Narayanan, S.; Niu, X.; Paus, C.; Rankin, D.; Roland, C.; Roland, G.; Shi, Z.; Stephans, G. S. F.; Sumorok, K.; Tatar, K.; Velicanu, D.; Wang, J.; Wang, T. W.; Wang, Z.; Wyslouch, B.; Chatterjee, R. M.; Evans, A.; Guts, S.; Hansen, P.; Hiltbrand, J.; Jain, Sh.; Krohn, M.; Kubota, Y.; Lesko, Z.; Mans, J.; Revering, M.; Rusack, R.; Saradhy, R.; Schroeder, N.; Strobbe, N.; Wadud, M. A.; Acosta, J. G.; Oliveros, S.; Bloom, K.; Chauhan, S.; Claes, D. R.; Fangmeier, C.; Finco, L.; Golf, F.; González Fernández, J. R.; Kravchenko, I.; Siado, J. E.; Snow, G. R.; Stieger, B.; Tabb, W.; Agarwal, G.; Harrington, C.; Iashvili, I.; Kharchilava, A.; McLean, C.; Nguyen, D.; Parker, A.; Pekkanen, J.; Rappoccio, S.; Roozbahani, B.; Alverson, G.; Barberis, E.; Freer, C.; Haddad, Y.; Hortiangtham, A.; Madigan, G.; Marzocchi, B.; Morse, D. M.; Nguyen, V.; Orimoto, T.; Skinnari, L.; Tishelman-Charny, A.; Wamorkar, T.; Wang, B.; Wisecarver, A.; Wood, D.; Bhattacharya, S.; Bueghly, J.; Chen, Z.; Gilbert, A.; Gunter, T.; Hahn, K. A.; Odell, N.; Schmitt, M. H.; Sung, K.; Velasco, M.; Bucci, R.; Dev, N.; Goldouzian, R.; Hildreth, M.; Hurtado Anampa, K.; Jessop, C.; Karmgard, D. J.; Lannon, K.; Li, W.; Loukas, N.; Marinelli, N.; Mcalister, I.; Meng, F.; Mohrman, K.; Musienko, Y.; Ruchti, R.; Siddireddy, P.; Taroni, S.; Wayne, M.; Wightman, A.; Wolf, M.; Zygala, L.; Alimena, J.; Bylsma, B.; Cardwell, B.; Durkin, L. S.; Francis, B.; Hill, C.; Ji, W.; Lefeld, A.; Winer, B. L.; Yates, B. R.; Dezoort, G.; Elmer, P.; Greenberg, B.; Haubrich, N.; Higginbotham, S.; Kalogeropoulos, A.; Kopp, G.; Kwan, S.; Lange, D.; Lucchini, M. T.; Luo, J.; Marlow, D.; Mei, K.; Ojalvo, I.; Olsen, J.; Palmer, C.; Piroué, P.; Stickland, D.; Tully, C.; Malik, S.; Norberg, S.; Barnes, V. E.; Chawla, R.; Das, S.; Gutay, L.; Jones, M.; Jung, A. W.; Mahakud, B.; Negro, G.; Neumeister, N.; Peng, C. C.; Piperov, S.; Qiu, H.; Schulte, J. F.; Trevisani, N.; Wang, F.; Xiao, R.; Xie, W.; Cheng, T.; Dolen, J.; Parashar, N.; Baty, A.; Dildick, S.; Ecklund, K. M.; Freed, S.; Geurts, F. J. M.; Kilpatrick, M.; Kumar, A.; Li, W.; Padley, B. P.; Redjimi, R.; Roberts, J.; Rorie, J.; Shi, W.; Stahl Leiton, A. G.; Tu, Z.; Zhang, A.; Bodek, A.; de Barbaro, P.; Demina, R.; Dulemba, J. L.; Fallon, C.; Ferbel, T.; Galanti, M.; Garcia-Bellido, A.; Hindrichs, O.; Khukhunaishvili, A.; Ranken, E.; Taus, R.; Chiarito, B.; Chou, J. P.; Gandrakota, A.; Gershtein, Y.; Halkiadakis, E.; Hart, A.; Heindl, M.; Hughes, E.; Kaplan, S.; Karacheban, O.; Laflotte, I.; Lath, A.; Montalvo, R.; Nash, K.; Osherson, M.; Salur, S.; Schnetzer, S.; Somalwar, S.; Stone, R.; Thayil, S. A.; Thomas, S.; Acharya, H.; Delannoy, A. G.; Spanier, S.; Bouhali, O.; Dalchenko, M.; Delgado, A.; Eusebi, R.; Gilmore, J.; Huang, T.; Kamon, T.; Kim, H.; Luo, S.; Malhotra, S.; Marley, D.; Mueller, R.; Overton, D.; Perniè, L.; Rathjens, D.; Safonov, A.; Akchurin, N.; Damgov, J.; Hegde, V.; Kunori, S.; Lamichhane, K.; Lee, S. W.; Mengke, T.; Muthumuni, S.; Peltola, T.; Undleeb, S.; Volobouev, I.; Wang, Z.; Whitbeck, A.; Appelt, E.; Greene, S.; Gurrola, A.; Janjam, R.; Johns, W.; Maguire, C.; Melo, A.; Ni, H.; Padeken, K.; Romeo, F.; Sheldon, P.; Tuo, S.; Velkovska, J.; Verweij, M.; Ang, L.; Arenton, M. W.; Cox, B.; Cummings, G.; Hakala, J.; Hirosky, R.; Joyce, M.; Ledovskoy, A.; Neu, C.; Tannenwald, B.; Wang, Y.; Wolfe, E.; Xia, F.; Karchin, P. E.; Poudyal, N.; Sturdy, J.; Thapa, P.; Black, K.; Bose, T.; Buchanan, J.; Caillol, C.; Dasu, S.; De Bruyn, I.; Dodd, L.; Galloni, C.; He, H.; Herndon, M.; Hervé, A.; Hussain, U.; Lanaro, A.; Loeliger, A.; Loveless, R.; Madhusudanan Sreekala, J.; Mallampalli, A.; Pinna, D.; Ruggles, T.; Savin, A.; Shang, V.; Sharma, V.; Smith, W. H.; Teague, D.; Trembath-reichert, S.; Vetens, W.; CMS Collaboration Bibcode: 2020PhRvL.125v2001S Altcode: Ultrarelativistic heavy ion collisions recreate in the laboratory the thermodynamical conditions prevailing in the early universe up to 10-6 sec , thereby allowing the study of the quark-gluon plasma (QGP), a state of quantum chromodynamics (QCD) matter with deconfined partons. The top quark, the heaviest elementary particle known, is accessible in nucleus-nucleus collisions at the CERN LHC, and constitutes a novel probe of the QGP. Here, we report the first evidence for the production of top quarks in nucleus-nucleus collisions, using lead-lead collision data at a nucleon-nucleon center-of-mass energy of 5.02 TeV recorded by the CMS experiment. Two methods are used to measure the cross section for top quark pair production (σt t ¯ ) via the selection of charged leptons (electrons or muons) and bottom quarks. One method relies on the leptonic information alone, and the second one exploits, in addition, the presence of bottom quarks. The measured cross sections, σt t ¯=2.5 4-0.74+0.84 and 2.03-0.64+0.71 μ b , respectively, are compatible with expectations from scaled proton-proton data and QCD predictions. Title: Projected WIMP sensitivity of the XENONnT dark matter experiment Authors: Aprile, E.; Aalbers, J.; Agostini, F.; Alfonsi, M.; Althueser, L.; Amaro, F. D.; Antochi, V. C.; Angelino, E.; Angevaare, J. R.; Arneodo, F.; Barge, D.; Baudis, L.; Bauermeister, B.; Bellagamba, L.; Benabderrahmane, M. L.; Berger, T.; Brown, A.; Brown, E.; Bruenner, S.; Bruno, G.; Budnik, R.; Capelli, C.; Cardoso, J. M. R.; Cichon, D.; Cimmino, B.; Clark, M.; Coderre, D.; Colijn, A. P.; Conrad, J.; Cussonneau, J. P.; Decowski, M. P.; Depoian, A.; Di Gangi, P.; Di Giovanni, A.; Di Stefano, R.; Diglio, S.; Elykov, A.; Eurin, G.; Ferella, A. D.; Fulgione, W.; Gaemers, P.; Gaior, R.; Galloway, M.; Gao, F.; Grandi, L.; Hasterok, C.; Hils, C.; Hiraide, K.; Hoetzsch, L.; Howlett, J.; Iacovacci, M.; Itow, Y.; Joerg, F.; Kato, N.; Kazama, S.; Kobayashi, M.; Koltman, G.; Kopec, A.; Landsman, H.; Lang, R. F.; Levinson, L.; Lin, Q.; Lindemann, S.; Lindner, M.; Lombardi, F.; Long, J.; Lopes, J. A. M.; López Fune, E.; Macolino, C.; Mahlstedt, J.; Mancuso, A.; Manenti, L.; Manfredini, A.; Marignetti, F.; Marrodán Undagoitia, T.; Martens, K.; Masbou, J.; Masson, D.; Mastroianni, S.; Messina, M.; Miuchi, K.; Mizukoshi, K.; Molinario, A.; Morå, K.; Moriyama, S.; Mosbacher, Y.; Murra, M.; Naganoma, J.; Ni, K.; Oberlack, U.; Odgers, K.; Palacio, J.; Pelssers, B.; Peres, R.; Pienaar, J.; Pizzella, V.; Plante, G.; Qin, J.; Qiu, H.; Ramírez García, D.; Reichard, S.; Rocchetti, A.; Rupp, N.; dos Santos, J. M. F.; Sartorelli, G.; Šarčević, N.; Scheibelhut, M.; Schreiner, J.; Schulte, D.; Schumann, M.; Scotto Lavina, L.; Selvi, M.; Semeria, F.; Shagin, P.; Shockley, E.; Silva, M.; Simgen, H.; Takeda, A.; Therreau, C.; Thers, D.; Toschi, F.; Trinchero, G.; Tunnell, C.; Valerius, K.; Vargas, M.; Volta, G.; Wang, H.; Wei, Y.; Weinheimer, C.; Weiss, M.; Wenz, D.; Wittweg, C.; Xu, Z.; Yamashita, M.; Ye, J.; Zavattini, G.; Zhang, Y.; Zhu, T.; Zopounidis, J. P. Bibcode: 2020JCAP...11..031A Altcode: 2020arXiv200708796T XENONnT is a dark matter direct detection experiment, utilizing 5.9 t of instrumented liquid xenon, located at the INFN Laboratori Nazionali del Gran Sasso. In this work, we predict the experimental background and project the sensitivity of XENONnT to the detection of weakly interacting massive particles (WIMPs). The expected average differential background rate in the energy region of interest, corresponding to (1, 13) keV and (4, 50) keV for electronic and nuclear recoils, amounts to 12.3 ± 0.6 (keV t y)-1 and (2.2± 0.5)× 10-3 (keV t y)-1, respectively, in a 4 t fiducial mass. We compute unified confidence intervals using the profile construction method, in order to ensure proper coverage. With the exposure goal of 20 t y, the expected sensitivity to spin-independent WIMP-nucleon interactions reaches a cross-section of 1.4×10-48 cm2 for a 50 GeV/c2 mass WIMP at 90% confidence level, more than one order of magnitude beyond the current best limit, set by XENON1T . In addition, we show that for a 50 GeV/c2 WIMP with cross-sections above 2.6×10-48 cm2 (5.0×10-48 cm2) the median XENONnT discovery significance exceeds 3σ (5σ). The expected sensitivity to the spin-dependent WIMP coupling to neutrons (protons) reaches 2.2×10-43 cm2 (6.0×10-42 cm2). Title: Main-Sequence Reinflation of Hot Jupiters Authors: Thorngren, D.; Lopez, E.; Fortney, J.; Berger, T.; Huber, D. Bibcode: 2020DPS....5221604T Altcode: The unexpectedly large radii of hot Jupiters is an open question in exoplanetary science for which a large number of explanations have been proposed. We leverage the strong relationship between hot Jupiter radii and incident fluxes to test these hypotheses by examining whether planets inflate as their parent stars brighten along the main sequence. To do this, we first study how the various observable parameters of the system can be used to predict the planetary radius. Next we show that stellar brightening is sufficient to cause detectable reinflation. We then argue that the predictors of radius, especially fractional age, flux, and ZAMS flux, point towards rapid reinflation that keeps pace with stellar brightening. We also find evidence for a delayed cooling effect in the first few gigayears of a planet's life, though it is not sufficient alone to explain the inflation phenomenon. Finally, we identify a negative relationship between stellar metallicity and planet radius (corrected for mass and flux), likely as a result of higher planetary metallicities. Title: Calibrating GONG Magnetograms with End-to-End Instrument Simulation II: Theory of Calibration Authors: Plowman, Joseph E.; Berger, Thomas E. Bibcode: 2020SoPh..295..142P Altcode: 2020arXiv200202490P This is the second of three papers describing an `absolute' calibration of the GONG magnetograph using an end-to-end simulation of its measurement process. In the first paper, we described the GONG instrument and our `end-to-end' simulation of its measurement process. In this paper, we consider the theory of calibration, and magnetograph comparison in general, identifying some of the significant issues and pitfalls. The calibration of a magnetograph is a function of whether or not it preserves flux, independent of its spatial resolution. However, we find that the one-dimensional comparison methods most often used for magnetograph calibration and comparison will show dramatic differences between two magnetograms with differing spatial resolution, even if they both preserve flux. Some of the apparent disagreement between magnetograms found in the literature are likely a result of these instrumental resolution differences rather than any intrinsic calibration differences. To avoid them, spatial resolution must be carefully matched prior to comparing magnetograms or making calibration curves. In the third paper, we apply the lessons learned here to absolute calibration of GONG using our `end-to-end' measurement simulation. Title: Calibrating GONG Magnetograms with End-to-end Instrument Simulation I: Background, the GONG Instrument, and End-to-end Simulation Authors: Plowman, Joseph E.; Berger, Thomas E. Bibcode: 2020SoPh..295..143P Altcode: 2020arXiv200202489P This is the first of three papers describing an `absolute' calibration of the GONG magnetograph using an end-to-end simulation of its measurement process. The input to this simulation is a MURaM 3D MHD photospheric simulation and the output is the corresponding set of simulated data numbers which would be recorded by the GONG detectors. These simulated data numbers are then used to produce `synthetic magnetograms' which can be compared with the simulation inputs. This paper describes the GONG instrument, the MURaM datacube, our instrument simulator, and calculation of synthetic magnetograms, setting the stage for the subsequent two papers. These will first lay groundwork for calibration (and magnetogram comparison in general), then apply them to calibration of GONG using the simulation results. Title: Calibrating GONG Magnetograms with End-to-End Instrument Simulation III: Comparison, Calibration, and Results Authors: Plowman, Joseph E.; Berger, Thomas E. Bibcode: 2020SoPh..295..144P Altcode: 2020arXiv200202486P This is the last of three papers describing an `absolute' calibration of the GONG magnetograph using and end-to-end simulation of its measurement process. The simulation begins with a MURaM 3D MHD datacube and ends with a `synthetic magnetogram' of the corresponding magnetic field values as they would be observed by GONG. We determine a calibration by comparing the synthetic magnetic field measurements with the MURaM magnetic field values that produced them. The previous two papers have described the GONG measurement process (both instrument and data processing), our simulation of it, and the theory of magnetogram comparison and calibration. In this paper, we address some final points on calibration, combine all of this work into a set of calibration curves, and consider the results. We also review the results of the previous two papers for locality of reference. Our calibration indicates that GONG magnetograms underestimate weak flux by a factor of ∼2 near disk center, but that factor decreases to ∼1 as the line-of-sight approaches the limb. A preliminary investigation of the generalizability of these results suggests other instruments will be affected in a similar way. We also find that some differences in previous magnetograph comparisons are artifacts of instrumental resolution which do not reflect an intrinsic calibration difference, and the measurements are more similar than sometimes thought. These results are directly applicable to question of solar wind prediction model accuracies, particularly in the search for the cause of the common discrepancy between predicted solar wind magnetic flux at 1 AU and values measured in situ by current satellite missions. Title: Excess electronic recoil events in XENON1T Authors: Aprile, E.; Aalbers, J.; Agostini, F.; Alfonsi, M.; Althueser, L.; Amaro, F. D.; Antochi, V. C.; Angelino, E.; Angevaare, J. R.; Arneodo, F.; Barge, D.; Baudis, L.; Bauermeister, B.; Bellagamba, L.; Benabderrahmane, M. L.; Berger, T.; Brown, A.; Brown, E.; Bruenner, S.; Bruno, G.; Budnik, R.; Capelli, C.; Cardoso, J. M. R.; Cichon, D.; Cimmino, B.; Clark, M.; Coderre, D.; Colijn, A. P.; Conrad, J.; Cussonneau, J. P.; Decowski, M. P.; Depoian, A.; di Gangi, P.; di Giovanni, A.; di Stefano, R.; Diglio, S.; Elykov, A.; Eurin, G.; Ferella, A. D.; Fulgione, W.; Gaemers, P.; Gaior, R.; Galloway, M.; Gao, F.; Grandi, L.; Hasterok, C.; Hils, C.; Hiraide, K.; Hoetzsch, L.; Howlett, J.; Iacovacci, M.; Itow, Y.; Joerg, F.; Kato, N.; Kazama, S.; Kobayashi, M.; Koltman, G.; Kopec, A.; Landsman, H.; Lang, R. F.; Levinson, L.; Lin, Q.; Lindemann, S.; Lindner, M.; Lombardi, F.; Long, J.; Lopes, J. A. M.; López Fune, E.; Macolino, C.; Mahlstedt, J.; Mancuso, A.; Manenti, L.; Manfredini, A.; Marignetti, F.; Marrodán Undagoitia, T.; Martens, K.; Masbou, J.; Masson, D.; Mastroianni, S.; Messina, M.; Miuchi, K.; Mizukoshi, K.; Molinario, A.; Morâ, K.; Moriyama, S.; Mosbacher, Y.; Murra, M.; Naganoma, J.; Ni, K.; Oberlack, U.; Odgers, K.; Palacio, J.; Pelssers, B.; Peres, R.; Pienaar, J.; Pizzella, V.; Plante, G.; Qin, J.; Qiu, H.; Ramírez García, D.; Reichard, S.; Rocchetti, A.; Rupp, N.; Dos Santos, J. M. F.; Sartorelli, G.; Šarčević, N.; Scheibelhut, M.; Schreiner, J.; Schulte, D.; Schumann, M.; Scotto Lavina, L.; Selvi, M.; Semeria, F.; Shagin, P.; Shockley, E.; Silva, M.; Simgen, H.; Takeda, A.; Therreau, C.; Thers, D.; Toschi, F.; Trinchero, G.; Tunnell, C.; Vargas, M.; Volta, G.; Wang, H.; Wei, Y.; Weinheimer, C.; Weiss, M.; Wenz, D.; Wittweg, C.; Xu, Z.; Yamashita, M.; Ye, J.; Zavattini, G.; Zhang, Y.; Zhu, T.; Zopounidis, J. P.; Xenon Collaboration, Mougeot, X. Bibcode: 2020PhRvD.102g2004A Altcode: 2020arXiv200609721A We report results from searches for new physics with low-energy electronic recoil data recorded with the XENON1T detector. With an exposure of 0.65 tonne-years and an unprecedentedly low background rate of 76 ±2stat events /(tonne ×year ×keV ) between 1 and 30 keV, the data enable one of the most sensitive searches for solar axions, an enhanced neutrino magnetic moment using solar neutrinos, and bosonic dark matter. An excess over known backgrounds is observed at low energies and most prominent between 2 and 3 keV. The solar axion model has a 3.4 σ significance, and a three-dimensional 90% confidence surface is reported for axion couplings to electrons, photons, and nucleons. This surface is inscribed in the cuboid defined by gae<3.8 ×10-12 , gaeganeff<4.8 ×10-18 , and gaega γ<7.7 ×10-22 GeV-1 , and excludes either gae=0 or gaega γ=gaeganeff=0 . The neutrino magnetic moment signal is similarly favored over background at 3.2 σ , and a confidence interval of μν∈(1.4 ,2.9 )×10-11 μB (90% C.L.) is reported. Both results are in strong tension with stellar constraints. The excess can also be explained by β decays of tritium at 3.2 σ significance with a corresponding tritium concentration in xenon of (6.2 ±2.0 )×10-25 mol /mol . Such a trace amount can neither be confirmed nor excluded with current knowledge of its production and reduction mechanisms. The significances of the solar axion and neutrino magnetic moment hypotheses are decreased to 2.0 σ and 0.9 σ , respectively, if an unconstrained tritium component is included in the fitting. With respect to bosonic dark matter, the excess favors a monoenergetic peak at (2.3 ±0.2 ) keV (68% C.L.) with a 3.0 σ global (4.0 σ local) significance over background. This analysis sets the most restrictive direct constraints to date on pseudoscalar and vector bosonic dark matter for most masses between 1 and 210 keV /c2 . We also consider the possibility that 37Ar may be present in the detector, yielding a 2.82 keV peak from electron capture. Contrary to tritium, the 37Ar concentration can be tightly constrained and is found to be negligible. Title: VizieR Online Data Catalog: Gaia-Kepler stellar properties catalog. II. Planets (Berger+, 2020) Authors: Berger, T. A.; Huber, D.; Gaidos, E.; van Saders, J. L.; Weiss, L. M. Bibcode: 2020yCat..51600108B Altcode: We computed the updated planet radii utilizing the planet-to-star radius ratios provided in the KOI table from the NASA Exoplanet Archive and the stellar radii computed in Paper I (Berger+, 2020, J/AJ/159/280). In addition, we updated semimajor axes using the stellar masses in Paper I and the orbital periods in Thompson+, 2018, J/ApJS/235/38. Finally, we updated the incident fluxes for each planet by using the semimajor axes and stellar luminosities from Paper I. (1 data file). Title: VizieR Online Data Catalog: Stellar parameters for 13196 Kepler dwarfs (Angus+, 2020) Authors: Angus, R.; Beane, A.; Price-Whelan, A. M.; Newton, E.; Curtis, J. L.; Berger, T.; van Saders, J.; Kiman, R.; Foreman-Mackey, D.; Lu, Y.; Anderson, L.; Faherty, J. K. Bibcode: 2020yCat..51600090A Altcode: We used the publicly available Kepler-Gaia DR2 crossmatched catalog to combine the McQuillan+ (2014, J/ApJS/211/24) catalog of stellar rotation periods, measured from Kepler light curves, with the Gaia DR2 catalog of parallaxes, proper motions, and apparent magnitudes. (1 data file). Title: VizieR Online Data Catalog: Gaia-Kepler stellar properties catalog.I. KIC stars (Berger+, 2020) Authors: Berger, T. A.; Huber, D.; van Saders, J. L.; Gaidos, E.; Tayar, J.; Kraus, A. L. Bibcode: 2020yCat..51590280B Altcode: In this paper, we utilize Gaia DR2 parallaxes, homogeneous stellar g and Ks photometry, and spectroscopic metallicities, where available, to improve on previous analyses and present the most accurate, homogeneous, and precise analysis of stars in the Kepler field. We re-derive stellar Teff, logg, radii, masses, densities, luminosities, and ages for 186301 Kepler targets, and investigate the stellar properties of a number of noteworthy Kepler exoplanet-hosting stars. (2 data files). Title: Energy resolution and linearity of XENON1T in the MeV energy range Authors: Aprile, E.; Aalbers, J.; Agostini, F.; Alfonsi, M.; Althueser, L.; Amaro, F. D.; Antochi, V. C.; Angelino, E.; Angevaare, J.; Arneodo, F.; Barge, D.; Baudis, L.; Bauermeister, B.; Bellagamba, L.; Benabderrahmane, M. L.; Berger, T.; Breur, P. A.; Brown, A.; Brown, E.; Bruenner, S.; Bruno, G.; Budnik, R.; Capelli, C.; Cardoso, J. M. R.; Cichon, D.; Cimmino, B.; Clark, M.; Coderre, D.; Colijn, A. P.; Conrad, J.; Cussonneau, J. P.; Decowski, M. P.; Depoian, A.; Di Gangi, P.; Di Giovanni, A.; Di Stefano, R.; Diglio, S.; Elykov, A.; Eurin, G.; Ferella, A. D.; Fulgione, W.; Gaemers, P.; Gaior, R.; Rosso, A. Gallo; Galloway, M.; Gao, F.; Garbini, M.; Grandi, L.; Hasterok, C.; Hils, C.; Hiraide, K.; Hoetzsch, L.; Hogenbirk, E.; Howlett, J.; Iacovacci, M.; Itow, Y.; Joerg, F.; Kato, N.; Kazama, S.; Kobayashi, M.; Koltman, G.; Kopec, A.; Landsman, H.; Lang, R. F.; Levinson, L.; Lin, Q.; Lindemann, S.; Lindner, M.; Lombardi, F.; Lopes, J. A. M.; Fune, E. López; Macolino, C.; Mahlstedt, J.; Manenti, L.; Manfredini, A.; Marignetti, F.; Undagoitia, T. Marrodán; Martens, K.; Masbou, J.; Masson, D.; Mastroianni, S.; Messina, M.; Miuchi, K.; Molinario, A.; Morâ, K.; Moriyama, S.; Mosbacher, Y.; Murra, M.; Naganoma, J.; Ni, K.; Oberlack, U.; Odgers, K.; Palacio, J.; Pelssers, B.; Peres, R.; Pienaar, J.; Pizzella, V.; Plante, G.; Qin, J.; Qiu, H.; García, D. Ramírez; Reichard, S.; Rocchetti, A.; Rupp, N.; dos Santos, J. M. F.; Sartorelli, G.; Šarčević, N.; Scheibelhut, M.; Schindler, S.; Schreiner, J.; Schulte, D.; Schumann, M.; Lavina, L. Scotto; Selvi, M.; Semeria, F.; Shagin, P.; Shockley, E.; Silva, M.; Simgen, H.; Takeda, A.; Therreau, C.; Thers, D.; Toschi, F.; Trinchero, G.; Tunnell, C.; Vargas, M.; Volta, G.; Wack, O.; Wang, H.; Wei, Y.; Weinheimer, C.; Xu, M. Weiss; Wenz, D.; Wittweg, C.; Wulf, J.; Xu, Z.; Yamashita, M.; Ye, J.; Zavattini, G.; Zhang, Y.; Zhu, T.; Zopounidis, J. P. Bibcode: 2020EPJC...80..785A Altcode: 2020arXiv200303825A Xenon dual-phase time projection chambers designed to search for weakly interacting massive particles have so far shown a relative energy resolution which degrades with energy above ∼ 200 keV due to the saturation effects. This has limited their sensitivity in the search for rare events like the neutrinoless double-beta decay of 136Xe at its Q value, Qβ β≃2.46 MeV . For the XENON1T dual-phase time projection chamber, we demonstrate that the relative energy resolution at 1 σ /μ is as low as (0.80 ±0.02 ) % in its one-ton fiducial mass, and for single-site interactions at Qβ β. We also present a new signal correction method to rectify the saturation effects of the signal readout system, resulting in more accurate position reconstruction and indirectly improving the energy resolution. The very good result achieved in XENON1T opens up new windows for the xenon dual-phase dark matter detectors to simultaneously search for other rare events. Title: The Lunar Lander Neutron and Dosimetry (LND) Experiment on Chang'E 4 Authors: Wimmer-Schweingruber, Robert F.; Yu, Jia; Böttcher, Stephan I.; Zhang, Shenyi; Burmeister, Sönke; Lohf, Henning; Guo, Jingnan; Xu, Zigong; Schuster, Björn; Seimetz, Lars; Freiherr von Forstner, Johan L.; Ravanbakhsh, Ali; Knierim, Violetta; Kolbe, Stefan; Woyciechowski, Hauke; Kulkarni, Shrinivasrao R.; Yuan, Bin; Shen, Guohong; Wang, Chunqing; Chang, Zheng; Berger, Thomas; Hellweg, Christine E.; Matthiä, Daniel; Hou, Donghui; Knappmann, Alke; Büschel, Charlotte; Hou, Xufeng; Ren, Baoguo; Fu, Qiang Bibcode: 2020SSRv..216..104W Altcode: 2020arXiv200111028W Chang'E 4 is the first mission to the far side of the Moon and consists of a lander, a rover, and a relay spacecraft. Lander and rover were launched at 18:23 UTC on December 7, 2018 and landed in the von Kármán crater at 02:26 UTC on January 3, 2019. Here we describe the Lunar Lander Neutron & Dosimetry experiment (LND) which is part of the Chang'E 4 Lander scientific payload. Its chief scientific goal is to obtain first active dosimetric measurements on the surface of the Moon. LND also provides observations of fast neutrons which are a result of the interaction of high-energy particle radiation with the lunar regolith and of their thermalized counterpart, thermal neutrons, which are a sensitive indicator of subsurface water content. Title: Long term variations of galactic cosmic radiation on board the International Space Station, on the Moon and on the surface of Mars Authors: Berger, Thomas; Matthiä, Daniel; Burmeister, Sönke; Zeitlin, Cary; Rios, Ryan; Stoffle, Nicholas; Schwadron, Nathan A.; Spence, Harlan E.; Hassler, Donald M.; Ehresmann, Bent; Wimmer-Schweingruber, Robert F. Bibcode: 2020JSWSC..10...34B Altcode: The radiation environment in free space and the related radiation exposure is seen as one of the main health detriments for future long-duration human exploration missions beyond Low Earth Orbit (LEO). The steady flux of energetic particles in the galactic cosmic radiation (GCR) produces a low dose-rate radiation exposure, which is heavily influenced by several factors including the solar cycle, the presence of an atmosphere, relevant magnetic fields (as on Earth) and of course by the relevant spacecraft shielding. Investigations of the GCR variations over the course of a solar cycle provide valuable data for exploration mission planning and for the determination of the radiation load received due to the GCR environment. Within the current work these investigations have been performed applying three datasets generated on board the International Space Station (ISS) with the DOSTEL instruments in the frame of the DOSIS and DOSIS-3D projects, with the CRaTER instrument in a Moon orbit and with the MSL-RAD instrument on the way to and on the surface of Mars. To derive GCR dose contributions on board the ISS two procedures have been developed separating the contributions from GCR from passing's through the South Atlantic Anomaly (SAA), as well as ways to extrapolate the GCR dose measured on board the ISS to free space based on various ranges of the McIlwain L-shell parameter. At the end we provide a dataset spanning the timeframe for GCR measurements on the ISS (2009-2011 & 2012-2019), Moon (2009-2019) and Mars (2012-2019), thereby covering the time span from the deep minimum of solar cycle 23, the ascending phase and maximum of solar cycle 24, and the descending phase of cycle 24, which is ongoing at the time of this writing. Title: Feasibility of Near-Real-Time GOLD Data Products Authors: Codrescu, S. M.; Rowland, W. F.; Plummer, T. M.; Vanier, B. A.; Berger, T. E.; Codrescu, M. V. Bibcode: 2020JGRA..12527819C Altcode: A primary limitation for accurate specification and forecasting of the thermosphere-ionosphere (TI) system is uncertainty in the system forcing. This significantly impacts users who have operational and real-time interests in the current and future state of the TI system. Since Global-Scale Observations of the Limb and Disk (GOLD) observations are expected to provide information about both the current state and forcing of the TI system, GOLD products could be an operational asset if they could be provided in near real time. Production of GOLD data products requires knowledge of the satellite pointing and location. The current scientific processing implementation contains an operationally significant delay to await definitive location and as-flown pointing. We present the results of a demonstration low-latency processing system that assumes the nominal satellite position and pointing to produce low-latency GOLD data products. The resulting products are reasonably similar to the scientific version but are available within minutes rather than hours. Title: Zodiacal exoplanets in time - X. The orbit and atmosphere of the young 'neptune desert'-dwelling planet K2-100b Authors: Gaidos, E.; Hirano, T.; Mann, A. W.; Owens, D. A.; Berger, T. A.; France, K.; Vanderburg, A.; Harakawa, H.; Hodapp, K. W.; Ishizuka, M.; Jacobson, S.; Konishi, M.; Kotani, T.; Kudo, T.; Kurokawa, T.; Kuzuhara, M.; Nishikawa, J.; Omiya, M.; Serizawa, T.; Tamura, M.; Ueda, A. Bibcode: 2020MNRAS.495..650G Altcode: 2020MNRAS.tmp..180G; 2020arXiv200312940G We obtained high-resolution infrared spectroscopy and short-cadence photometry of the 600-800 Myr Praesepe star K2-100 during transits of its 1.67-d planet. This Neptune-size object, discovered by the NASA K2 mission, is an interloper in the 'desert' of planets with similar radii on short-period orbits. Our observations can be used to understand its origin and evolution by constraining the orbital eccentricity by transit fitting, measuring the spin-orbit obliquity by the Rossiter-McLaughlin effect, and detecting any extended, escaping the hydrogen-helium envelope with the 10 830 -Å line of neutral helium in the 2s3S triplet state. Transit photometry with 1-min cadence was obtained by the K2 satellite during Campaign 18 and transit spectra were obtained with the IRD spectrograph on the Subaru telescope. While the elevated activity of K2-100 prevented us from detecting the Rossiter-McLaughlin effect, the new photometry combined with revised stellar parameters allowed us to constrain the eccentricity to e < 0.15/0.28 with 90/99 per cent confidence. We modelled atmospheric escape as an isothermal, spherically symmetric Parker wind, with photochemistry driven by ultraviolet radiation, which we estimate by combining the observed spectrum of the active Sun with calibrations from observations of K2-100 and similar young stars in the nearby Hyades cluster. Our non-detection (<5.7 m Å) of a transit-associated He I line limits mass-loss of a solar-composition atmosphere through a T ≤ 10000 K wind to <0.3 M⊕ Gyr-1. Either K2-100b is an exceptional desert-dwelling planet, or its mass-loss is occurring at a lower rate over a longer interval, consistent with a core accretion-powered scenario for escape. Title: A Probabilistic Approach to Kepler Completeness and Reliability for Exoplanet Occurrence Rates Authors: Bryson, S.; Coughlin, J.; Batalha, N. M.; Berger, T.; Huber, D.; Burke, C.; Dotson, J.; Mullally, S. E. Bibcode: 2020AJ....159..279B Altcode: 2019arXiv190603575B Exoplanet catalogs produced by surveys suffer from a lack of completeness (not every planet is detected) and less than perfect reliability (not every planet in the catalog is a true planet), particularly near the survey's detection limit. Exoplanet occurrence rate studies based on such a catalog must be corrected for completeness and reliability. The final Kepler data release, DR25, features a uniformly vetted planet candidate catalog and data products that facilitate corrections. We present a new probabilistic approach to the characterization of Kepler completeness and reliability, making full use of the Kepler DR25 products. We illustrate the impact of completeness and reliability corrections with a Poisson-likelihood occurrence rate method, using a recent stellar properties catalog that incorporates Gaia stellar radii and essentially uniform treatment of the stellar population. Correcting for reliability has a significant impact: the exoplanet occurrence rate for orbital period and radius within 20% of Earth's around GK dwarf stars, corrected for reliability, is ${0.015}_{-0.007}^{+0.011}$ , whereas not correcting results in ${0.034}_{-0.012}^{+0.018}$ —correcting for reliability reduces this occurrence rate by more than a factor of two. We further show that using Gaia-based versus DR25 stellar properties impacts the same occurrence rate by a factor of two. We critically examine the the DR25 catalog and the assumptions behind our occurrence rate method. We propose several ways in which confidence in both the Kepler catalog and occurrence rate calculations can be improved. This work provides an example of how the community can use the DR25 completeness and reliability products. Title: Energetic particles measurements on the lunar far-side by Lunar Lander Neutron and Dosimetry(LND) experiment Authors: Xu, Zigong; Wimmer-Schweingruber, Robert F.; Guo, Jingnan; Yu, Jia; Zhang, Shenyi; Berger, Thomas; Matthiae, Daniel; Burmeister, Soenke; Boettcher, Stephan; Heber, Bernd Bibcode: 2020EGUGA..2221246X Altcode: After Chang'E 4 successfully landed on the far side of the moon on Jan 3rd, 2019, the Lunar Lander Neutron and Dosimetry experiment has been working for 13 lunar days from January, 2019 to January, 2020, sending back the measurements of dose, linear energy transfer (LET) spectrum, neutrons, and charged particles. Here, we show observations of charged particles especially protons and Helium ions during quiet time. We also present two solar energetic particle events registered by LND in May 2019, which are also the first such measurements on the far-side surface of the moon. The temporal variations of particle fluxes on the far side of the moon detected by LND provide a new observation site in space and can be helpful to improve our understanding of particle propagation and transport in the heliosphere. Title: RIMFAX Ground Penetrating Radar Field Tests in the Western USA Authors: Russell, P. S.; Nunes, D.; Hamran, S. -E.; Paige, D. A.; Berger, T.; Amundsen, H. E. F.; Brovoll, S.; Carter, L. M.; Dypvik, H.; Ghent, R.; Kohler, J.; Mellon, M. T.; Plettemeier, D. Bibcode: 2020LPI....51.3012R Altcode: The RIMFAX GPR on Mars2020 was tested for performance and for insight into Mars subsurfaces in several locations, lithologies, and structures in the western US. Title: Leveraging the mathematics of shape for solar magnetic eruption prediction Authors: Deshmukh, Varad; Berger, Thomas E.; Bradley, Elizabeth; Meiss, James D. Bibcode: 2020JSWSC..10...13D Altcode: 2020arXiv200305827D Current operational forecasts of solar eruptions are made by human experts using a combination of qualitative shape-based classification systems and historical data about flaring frequencies. In the past decade, there has been a great deal of interest in crafting machine-learning (ML) flare-prediction methods to extract underlying patterns from a training set - e.g. a set of solar magnetogram images, each characterized by features derived from the magnetic field and labeled as to whether it was an eruption precursor. These patterns, captured by various methods (neural nets, support vector machines, etc.), can then be used to classify new images. A major challenge with any ML method is the featurization of the data: pre-processing the raw images to extract higher-level properties, such as characteristics of the magnetic field, that can streamline the training and use of these methods. It is key to choose features that are informative, from the standpoint of the task at hand. To date, the majority of ML-based solar eruption methods have used physics-based magnetic and electric field features such as the total unsigned magnetic flux, the gradients of the fields, the vertical current density, etc. In this paper, we extend the relevant feature set to include characteristics of the magnetic field that are based purely on the geometry and topology of 2D magnetogram images and show that this improves the prediction accuracy of a neural-net based flare-prediction method. Title: Flying Through Uncertainty Authors: Berger, T. E.; Holzinger, M. J.; Sutton, E. K.; Thayer, J. P. Bibcode: 2020SpWea..1802373B Altcode: Space weather is the main source of uncertainty in the position of all objects in low Earth orbit (LEO) below about 1,000 km. The main impact is strong variation in the neutral density of the thermosphere as it responds to radiative inputs from the Sun in the extreme ultraviolet wavelength range, energetic particle precipitation in the high-latitude auroral zones, and global-scale electrical currents generated during geomagnetic storms. Waves and instabilities from the lower atmosphere can also influence thermospheric density in complex ways. The variation in neutral density leads to variable drag forces on satellites flying through the thermosphere, which in turn causes orbital track changes. We currently lack the ability to accurately model and predict the neutral density changes in the thermosphere in response to space weather inputs. Operational empirical models of thermospheric density are inaccurate during space weather events, and mandate that LEO orbital tracks carry large "error ellipsoids" around all objects to account for positional uncertainty. This leads to many more "conjunction" warnings than necessary as large error ellipsoids are frequently calculated to intersect in orbit. As the LEO domain becomes more crowded with the advent of commercial "megaconstellations" we face a growing challenge to reduce orbital uncertainties by developing whole atmosphere models to enable timely and accurate forecasts of thermospheric conditions. We recommend that researchers, forecasters, and policy makers coordinate to ensure that space weather research and forecasting is tightly integrated into upcoming changes to the operational Space Traffic Management system. Title: Radiation in Space: Relevance and Risk for Human Missions Authors: Hellweg, Christine E.; Berger, Thomas; Matthiä, Daniel; Baumstark-Khan, Christa Bibcode: 2020rsrr.book.....H Altcode: No abstract at ADS Title: University of Colorado Space Weather Technology, Research, and Education Center (SWx TREC): An academic center of excellence to accelerate research to operations and operations to research transitions Authors: Berger, T. E.; Thayer, J. P.; Baker, D. N.; Knipp, D. J.; Pankratz, C. K.; Cranmer, S. R.; Sutton, E. K.; Baltzer, T.; Lucas, G.; Craft, J.; Bosanac, N.; Smith, T. R. Bibcode: 2019AGUFMSA13A..06B Altcode: The University of Colorado at Boulder Space Weather Technology Research and Education Center (SWx TREC) is a University Chancellor's Grand Challenge Initiative forming a campus-wide center for research, mission and technology development, and educational initiatives in the space weather enterprise. SWx TREC offers a unique open academic environment with contributions not only from the departments of Astrophysics and Planetary Sciences, Aerospace Engineering Sciences, and Atmospheric and Oceanic Sciences, but from campus institutes such as the Laboratory for Atmospheric and Space Physics (LASP) and the Cooperative Institute for Research in Environmental Sciences (CIRES) as well. In addition, SWx TREC serves as a "Front Range" space weather collaboration engine, reaching out to local government (NOAA/SWPC, USAF/SpaceCommand) and industry (Ball Aerospace, Lockheed Martin, Raytheon, Google) elements, commercial space weather providers such as Astra LLC and Space Environment Technologies (SET), and local FFRDCs such as the National Solar Observatory (NSO), NCAR's High Altitude Observatory (HAO), the Southwest Research Institute (SWRI), and Northwest Research Associates (NWRA) to pursue opportunities to advance space weather forecasting through innovative research. We discuss how SWx TREC is working with these partners to develop new satellite drag models for Civil Space Traffic Management (STM) applications, a Space Weather Data Portal to ease multi-instrument data display and analysis, and a Space Weather Testbed that will allow academic and commercial developers to test new models and forecasting tools in a cloud-based prototyping facility with student and professional forecaster engagement. SWx TREC is also developing two innovative mission concepts to fill major gaps in the current space weather observing system: the Solar Polar Observing Constellation (SPOC) with Ball Aerospace, and the Operational Radiation Belts (ORB) mission for the Air Force. Title: SWx TREC: An Emerging Community Resource for Integrative Space Weather Data Access and Model/Algorithm R2O Promotion Authors: Pankratz, C. K.; Baltzer, T.; Lucas, G.; Craft, J.; Knuth, J.; Berger, T. E.; Sutton, E. K.; Baker, D. N.; Jaynes, A. N. Bibcode: 2019AGUFMSH33C3373P Altcode: The Space Weather Technology, Research and Education Center (SWx TREC) is an emerging national center of excellence in cross-disciplinary research, technology, innovation, and education, intended to facilitate evolving space weather research and forecasting needs. SWx TREC is positioned to facilitate breakthrough research advances, innovative missions, and data and computing technologies that directly support the needs of the operational forecasting enterprise to ensure closure of the Research to Operations (R2O) and Operations to Research (O2R) loop. Improving our understanding and prediction of space weather requires coupled Research and Operations. SWx-TREC is working to provide new research models, applications and data for use in operational environments, improving the Research-to-Operations (R2O) pipeline. Advancement in the fundamental scientific understanding of space weather processes is also vital, requiring that researchers have convenient and effective access to a wide variety of data sets and models from multiple sources. The space weather research community, as with many scientific communities, must access data from dispersed and often uncoordinated data repositories to acquire the data necessary for the analysis and modeling efforts that advance our understanding of solar influences and space physics in the Earth's environment. The University of Colorado (CU) is a leading institution in both producing data products and advancing the state of scientific understanding of space weather processes, and is serving many of these needs, including 1) implementation of an interoperable data portal intended to more effectively serve the needs of the Space Weather research community and 2) implementing a community-accessible testbed environment to support development, testing, transition, and use of new models and algorithms. In this presentation, we will outline the motivating factors for effective space weather data access and modeling support, describe a new testbed environment for supporting model, algorithm, and visualization testing/incubation needs, and demonstrate a new Space Weather Data Portal, designed to meet the data management and access needs of the disparate communities who require space weather data and information. Title: Adding Lunar Observations to Multi-point Observations around Earth to Determine the Structure Heliospheric Discontinuities Authors: Wimmer-Schweingruber, R. F.; Yu, J.; Xu, Z.; Zhang, S.; Hou, D.; Guo, J.; Freiherr von Forstner, J. L.; Lohf, H.; Boettcher, S. I.; Burmeister, S.; Matthiae, D.; Berger, T.; Hellweg, C. Bibcode: 2019AGUFMSH41A..01W Altcode: The Chinese Chang'E 4 spacecraft landed on the Moon on January 3, 2019. The Lunar Lander Neutrons and Dosimetry (LND) instrument aboard the Chang'E 4 lander provides measurements of the radiation environment on the Moon. Some of its data products are provided at a cadence of once per minute. Combining such data with high time resolution data from other spacecraft near Earth (i.e., ACE, DSCOVR, SOHO, and Wind at L1) allows to determine the three-dimensional structure of discontinuities in the solar wind when (instrumental) counting statistics are good enough. We will present first attempts at reconstructing the inclination angles of large-scale heliospheric discontinuities using data from ACE, Chang'E 4, DSCOVR, SOHO, and Wind. We assume a radially flowing solar wind speed of constant speed in individual solar wind streams and investigate the timing of discontinuities in count rates of particle and solar-wind instruments on these spacecraft. Title: Energetic particles measurements on the lunar far side by Lunar Lander Neutron and Dosimetry(LND) experiment Authors: Xu, Z.; Wimmer-Schweingruber, R. F.; Guo, J.; Yu, J.; Zhang, S.; Berger, T.; Matthiae, D.; Burmeister, S.; Boettcher, S. I.; Heber, B. Bibcode: 2019AGUFMSH41D3340X Altcode: After Chang'E 4 successfully landed on the far side of the moon on Jan 3rd, 2019, the Lunar Lander Neutron and Dosimetry experiment has been working for 7 lunar days from January to July, sending back the measurements of dose, linear energy transfer (LET) spectrum, neutrons and charged particles. Here, we show observations of charged particles especially protons and Helium ions, including long term variation and solar energetic events, which are also the first such measurements on the surface of the moon. The long-term variation is mainly caused by solar modulation of galactic cosmic rays (GCR) and anomalous cosmic rays (ACR). Comparing the energy spectra of protons and He4 with those detected by EPHIN in 2019 and during the previous solar minimum in 1996, as well as the Crème and BO10 models, we find that the protons detected by LND were from GCR and solar source, while the He4 were mainly from the ACR. This is a consequence of LND's energy coverage. We also derive the upward proton fluxes due to the interaction of downward energetic particles with lunar regolith. We will also present a solar energetic particle event registered by LND in May, 2019. The temporal variations of particle fluxes on the far side of the moon detected by LND provide a new observation site in space and can be helpful to improve our understanding of particle propagation and transport in the heliosphere. Title: The Solar Polar Observing Constellation (SPOC) Mission: research and operational monitoring of space weather from polar heliocentric orbits Authors: Berger, T. E.; Bosanac, N.; Smith, T. R.; Duncan, N. A.; Wu, G.; Turner, E.; Hurlburt, N.; Korendyke, C. Bibcode: 2019AGUFMSH43F3352B Altcode: The Sun's polar regions remain largely unobserved and yet understanding and monitoring of the magnetic field, convective flows, and coronal outflow conditions in the solar polar regions are the keys to accurately modeling and forecasting the solar cycle, solar wind conditions, and CME arrival times at Earth. We describe the Solar Polar Observing Constellation (SPOC), a mission to establish continuous high-resolution imaging of solar magnetic field dynamics, high-latitude surface and sub-surface convective flows, and coronal mass ejection tracking from a low-eccentricity polar heliocentric orbit. SPOC will consist of two identical spacecraft, each equipped with a Lockheed Martin Compact Magnetic Imager (CMI, derived from the Solar Dynamics Observatory (SDO) Helioseismic and Magnetic Imager), the Naval Research Laboratory (NRL) Compact Coronagraph (CCOR), and in-situ solar wind and energetic particle instruments. Falcon Heavy launch vehicles will place the SPOC spacecraft into a Jupiter gravitational assist (JGA) heliocentric orbit, achieving an 88-degree ecliptic inclination, with the spacecraft passing over the solar poles within 4 years after launch. Ion engines will subsequently reduce the eccentricity of the orbits to below 0.05 at approximately 0.9 AU within 6 years after launch. Orbital phasing will place the spacecraft over alternate poles to enable continuous monitoring of the polar regions with operational-level redundancy of systems. The inclusion of CCOR will enable visualization and tracking of coronal mass ejections from above (or below) the ecliptic for the first time, greatly enhancing our ability to forecast CME arrival times at Earth and other planets such as Mars. SPOC combines polar region exploration, high-latitude helioseismology and magnetic imaging, and operational space weather monitoring in a single mission. Along with planned missions to the L1 and L5 Lagrangian points in the ecliptic, SPOC will enable an approach to the long-sought goal of continuous full-sphere measurements of the solar magnetic field, solar wind and CME outflow, and energetic particle flux - a goal that cannot be achieved with observations from the ecliptic plane alone. Title: Search for Light Dark Matter Interactions Enhanced by the Migdal Effect or Bremsstrahlung in XENON1T Authors: Aprile, E.; Aalbers, J.; Agostini, F.; Alfonsi, M.; Althueser, L.; Amaro, F. D.; Antochi, V. C.; Angelino, E.; Arneodo, F.; Barge, D.; Baudis, L.; Bauermeister, B.; Bellagamba, L.; Benabderrahmane, M. L.; Berger, T.; Breur, P. A.; Brown, A.; Brown, E.; Bruenner, S.; Bruno, G.; Budnik, R.; Capelli, C.; Cardoso, J. M. R.; Cichon, D.; Coderre, D.; Colijn, A. P.; Conrad, J.; Cussonneau, J. P.; Decowski, M. P.; de Perio, P.; Depoian, A.; di Gangi, P.; di Giovanni, A.; Diglio, S.; Elykov, A.; Eurin, G.; Fei, J.; Ferella, A. D.; Fieguth, A.; Fulgione, W.; Gaemers, P.; Gallo Rosso, A.; Galloway, M.; Gao, F.; Garbini, M.; Grandi, L.; Greene, Z.; Hasterok, C.; Hils, C.; Hogenbirk, E.; Howlett, J.; Iacovacci, M.; Itay, R.; Joerg, F.; Kazama, S.; Kish, A.; Kobayashi, M.; Koltman, G.; Kopec, A.; Landsman, H.; Lang, R. F.; Levinson, L.; Lin, Q.; Lindemann, S.; Lindner, M.; Lombardi, F.; Lopes, J. A. M.; López Fune, E.; Macolino, C.; Mahlstedt, J.; Manenti, M.; Manfredini, A.; Marignetti, F.; Marrodán Undagoitia, T.; Masbou, J.; Mastroianni, S.; Messina, M.; Micheneau, K.; Miller, K.; Molinario, A.; Morâ, K.; Mosbacher, Y.; Murra, M.; Naganoma, J.; Ni, K.; Oberlack, U.; Odgers, K.; Palacio, J.; Pelssers, B.; Peres, R.; Pienaar, J.; Pizzella, V.; Plante, G.; Podviianiuk, R.; Qin, J.; Qiu, H.; Ramírez García, D.; Reichard, S.; Riedel, B.; Rocchetti, A.; Rupp, N.; Dos Santos, J. M. F.; Sartorelli, G.; Šarčević, N.; Scheibelhut, M.; Schindler, S.; Schreiner, J.; Schulte, D.; Schumann, M.; Scotto Lavina, L.; Selvi, M.; Shagin, P.; Shockley, E.; Silva, M.; Simgen, H.; Therreau, C.; Thers, D.; Toschi, F.; Trinchero, G.; Tunnell, C.; Upole, N.; Vargas, M.; Volta, G.; Wack, O.; Wang, H.; Wei, Y.; Weinheimer, C.; Wenz, D.; Wittweg, C.; Wulf, J.; Ye, J.; Zhang, Y.; Zhu, T.; Zopounidis, J. P.; Xenon Collaboration Bibcode: 2019PhRvL.123x1803A Altcode: 2019arXiv190712771A Direct dark matter detection experiments based on a liquid xenon target are leading the search for dark matter particles with masses above ∼5 GeV /c2, but have limited sensitivity to lighter masses because of the small momentum transfer in dark matter-nucleus elastic scattering. However, there is an irreducible contribution from inelastic processes accompanying the elastic scattering, which leads to the excitation and ionization of the recoiling atom (the Migdal effect) or the emission of a bremsstrahlung photon. In this Letter, we report on a probe of low-mass dark matter with masses down to about 85 MeV /c2 by looking for electronic recoils induced by the Migdal effect and bremsstrahlung using data from the XENON1T experiment. Besides the approach of detecting both scintillation and ionization signals, we exploit an approach that uses ionization signals only, which allows for a lower detection threshold. This analysis significantly enhances the sensitivity of XENON1T to light dark matter previously beyond its reach. Title: The University of Colorado Space Weather Technology, Research, and Education Center's Space Weather Portal: A Tool for Easing Access to and Understanding of Datasets to Characterize Space Weather Events Authors: Baltzer, T.; Berger, T. E.; Knuth, J.; Lindholm, D. M.; Wilson, A.; Pankratz, C. K. Bibcode: 2019AGUFMSH33C3371B Altcode: In our work with researchers, we consistently hear that a significant hurdle they encounter is obtaining datasets from disparate providers in varying formats, needing to repeat processes to obtain new timeframes for those datasets and that having an idea of what is available (e.g. is there an instrument outage during the time of interest?) before downloading it is often unavailable. This is particularly challenging for space weather researchers attempting to characterize an event from the moment of occurrence on the Sun to the impacts it has on the Earth. As part of the University of Colorado's Space Weather Technology, Research and Education Center (SWx-TREC https://www.colorado.edu/spaceweather/), the Laboratory for Atmospheric and Space Physics (LASP) is developing a Space Weather Portal (http://lasp.colorado.edu/space-weather-portal) to provide unified access to disparate datasets to help close the Research to Operations (R2O) and Operations to Research (O2R) gap. This presentation will describe how this portal can be used to characterize an historical event (2015 St. Patrick's day storm) from available datasets, visualize them and download them for further use. It will also describe the underlying middleware (LaTiS) that enables the portal. Title: Light Dark Matter Search with Ionization Signals in XENON1T Authors: Aprile, E.; Aalbers, J.; Agostini, F.; Alfonsi, M.; Althueser, L.; Amaro, F. D.; Antochi, V. C.; Angelino, E.; Arneodo, F.; Barge, D.; Baudis, L.; Bauermeister, B.; Bellagamba, L.; Benabderrahmane, M. L.; Berger, T.; Breur, P. A.; Brown, A.; Brown, E.; Bruenner, S.; Bruno, G.; Budnik, R.; Capelli, C.; Cardoso, J. M. R.; Cichon, D.; Coderre, D.; Colijn, A. P.; Conrad, J.; Cussonneau, J. P.; Decowski, M. P.; de Perio, P.; Depoian, A.; di Gangi, P.; di Giovanni, A.; Diglio, S.; Elykov, A.; Eurin, G.; Fei, J.; Ferella, A. D.; Fieguth, A.; Fulgione, W.; Gaemers, P.; Gallo Rosso, A.; Galloway, M.; Gao, F.; Garbini, M.; Grandi, L.; Greene, Z.; Hasterok, C.; Hils, C.; Hogenbirk, E.; Howlett, J.; Iacovacci, M.; Itay, R.; Joerg, F.; Kazama, S.; Kish, A.; Kobayashi, M.; Koltman, G.; Kopec, A.; Landsman, H.; Lang, R. F.; Levinson, L.; Lin, Q.; Lindemann, S.; Lindner, M.; Lombardi, F.; Lopes, J. A. M.; López Fune, E.; Macolino, C.; Mahlstedt, J.; Manfredini, A.; Marignetti, F.; Marrodán Undagoitia, T.; Masbou, J.; Mastroianni, S.; Messina, M.; Micheneau, K.; Miller, K.; Molinario, A.; Morâ, K.; Mosbacher, Y.; Murra, M.; Naganoma, J.; Ni, K.; Oberlack, U.; Odgers, K.; Palacio, J.; Pelssers, B.; Peres, R.; Pienaar, J.; Pizzella, V.; Plante, G.; Podviianiuk, R.; Qin, J.; Qiu, H.; Ramírez García, D.; Reichard, S.; Riedel, B.; Rocchetti, A.; Rupp, N.; Dos Santos, J. M. F.; Sartorelli, G.; Šarčević, N.; Scheibelhut, M.; Schindler, S.; Schreiner, J.; Schulte, D.; Schumann, M.; Scotto Lavina, L.; Selvi, M.; Shagin, P.; Shockley, E.; Silva, M.; Simgen, H.; Therreau, C.; Thers, D.; Toschi, F.; Trinchero, G.; Tunnell, C.; Upole, N.; Vargas, M.; Volta, G.; Wack, O.; Wang, H.; Wei, Y.; Weinheimer, C.; Wenz, D.; Wittweg, C.; Wulf, J.; Ye, J.; Zhang, Y.; Zhu, T.; Zopounidis, J. P.; Xenon Collaboration Bibcode: 2019PhRvL.123y1801A Altcode: 2019arXiv190711485A We report constraints on light dark matter (DM) models using ionization signals in the XENON1T experiment. We mitigate backgrounds with strong event selections, rather than requiring a scintillation signal, leaving an effective exposure of (22 ±3 ) tonne day. Above ∼0.4 keVe e , we observe <1 event/(tonne day keVe e) , which is more than 1000 times lower than in similar searches with other detectors. Despite observing a higher rate at lower energies, no DM or CEvNS detection may be claimed because we cannot model all of our backgrounds. We thus exclude new regions in the parameter spaces for DM-nucleus scattering for DM masses mχ within 3 - 6 GeV /c2 , DM-electron scattering for mχ>30 MeV /c2 , and absorption of dark photons and axionlike particles for mχ within 0.186 - 1 keV /c2 . Title: Cooling Condensation at Coronal Null Points and Quasi-Separatrix Layers Involving Magnetic Reconnection Authors: Liu, W.; Sun, X.; Yu, S.; Luna Bennasar, M.; Antolin, P.; Titov, V. S.; Downs, C.; Berger, T. E. Bibcode: 2019AGUFMSH11C3394L Altcode: The solar corona, Sun's outer atmosphere, is million-degrees hot and tenuous. This hot plasma, under certain conditions, can enigmatically undergo a radiative cooling instability and condense into material of 100 times cooler in the form of prominences or coronal rain. Where, when, and how such cooling condensation takes place remain poorly understood. Answers to these questions are not only of scientific importance in their own right, but also bear implications for the fundamental question of coronal heating and the chromosphere-corona mass cycle. Magnetic fields in the magnetized corona undoubtedly play a crucial role (e.g., by trapping the plasma), but where and how? We report recent imaging and spectroscopic observations from SDO/AIA/HMI and IRIS that can shed light on these puzzles. Through a systematic survey, we found that a large fraction of quiet-Sun condensations preferentially occur at the dips of coronal loops or funnels. Such dips are located at/near magnetic topological features, such as null points and quasi-separatrix layers (QSLs), which are regions characterized by high values of the squashing factor. We also identified evidence of magnetic reconnection at such locations, which can produce favorable conditions, e.g., density enhancement by compression and/or mass trapping in plasmoids, that can trigger run-away radiative cooling. We present proof-of-concept MHD simulations that demonstrate the role of reconnection in transporting cooled mass from overlying, long loops to underlying, short loops where it slide down as coronal rain. We will discuss the significance and broader implications of these results beyond solar physics. Title: SWx TREC Testbed: Facilitating Model/Algorithm R2O and O2R Development within a Cloud Computing Environment Authors: Lucas, G.; Craft, J.; Pankratz, C. K.; Sutton, E. K.; Berger, T. E. Bibcode: 2019AGUFMSH33C3372L Altcode: The Space Weather Technology, Research and Education Center (SWx TREC) is an emerging national center of excellence in cross-disciplinary research, technology, innovation, and education, intended to facilitate evolving space weather research and forecasting needs. Within this center, we are developing a Space Weather Testbed environment to facilitate the research to operations (R2O) and operations to research (O2R) pipelines. The Testbed leverages cloud computing to provide a managed computational environment for independent science teams to deploy their processing software into an operational-like system. Using cloud computing for the environment enables traditional defined-cadence (daily, hourly) model runs to be scheduled while also providing the ability to submit on-demand runs during storm times with no additional bulk hardware purchases that would otherwise sit idle most of the time. In this poster, we will discuss the technologies that are being used in producing the Space Weather Testbed and demonstrate two ways that the testbed is currently being utilized. First, in the R2O pipeline, we have implemented code from the USGS to produce electric field maps at a set cadence to demonstrate that the code can be run in an operational mode. Second, in the O2R pipeline, we are taking an operational code, the NOAA Whole Atmosphere Model (WAM), and enabling researchers to investigate new data assimilation techniques that can supplement and enhance current operational code capabilities. The Space Weather TREC Testbed is utilizing modern computer architectures and software practices to facilitate researchers and forecasters bridge the R2O and O2R gaps. Title: VizieR Online Data Catalog: Revised radii of KIC stars & planets using Gaia DR2 (Berger+, 2018) Authors: Berger, T. A.; Huber, D.; Gaidos, E.; van Saders, J. L. Bibcode: 2019yCat..18660099B Altcode: First, we crossmatched the positions of all stars from the Kepler Stellar Properties Catalog (KSPC DR25; Mathur+ 2017, J/ApJS/229/30) with the Gaia Data Release 2 (DR2, I/345) by utilizing the X-match service of the Centre de Donnees astronomiques de Strasbourg (CDS). This provided a table of Gaia DR2 source matches within 3" of each Keplers tar. Excluding stars through a variety of cuts reduced our final sample to 177911 Kepler stars. See section 2.1 for further details. (2 data files). Title: Planetesimals around stars with TESS (PAST) - I. Transient dimming of a binary solar analogue at the end of the planet accretion era Authors: Gaidos, E.; Jacobs, T.; LaCourse, D.; Vanderburg, A.; Rappaport, S.; Berger, T.; Pearce, L.; Mann, A. W.; Weiss, L.; Fulton, B.; Behmard, A.; Howard, A. W.; Ansdell, M.; Ricker, G. R.; Vanderspek, R. K.; Latham, D. W.; Seager, S.; Winn, J. N.; Jenkins, J. M. Bibcode: 2019MNRAS.488.4465G Altcode: 2019arXiv190702476G; 2019MNRAS.tmp.1875G We report detection of quasi-periodic (1.5-d) dimming of HD 240779, the solar-mass primary in a 5 arcsec visual binary (also TIC 284730577), by the Transiting Exoplanet Survey Satellite. This dimming, as has been shown for other `dipper' stars, is likely due to occultation by circumstellar dust. The barycentric space motion, lithium abundance, rotation, and chromospheric emission of the stars in this system point to an age of ≈125 Myr, and possible membership in the AB Doradus moving group. As such it occupies an important but poorly explored intermediate regime of stars with transient dimming between young stellar objects in star-forming regions and main-sequence stars, and between UX Orionis-type Ae/Be stars and M-type `dippers'. HD 240779, but not its companion BD+10 714B, has Wide-field Infrared Survey Explorer (WISE)-detected excess infrared emission at 12 and 22 μm indicative of circumstellar dust. We propose that infrared emission is produced by collisions of planetesimals during clearing of a residual disc at the end of rocky planet formation, and that quasi-periodic dimming is produced by the rapid disintegration of a ≳100 km planetesimal near the silicate evaporation radius. Further studies of this and similar systems will illuminate a poorly understood final phase of rocky planet formation like that which produced the inner Solar system. Title: Phobos LIFE (Living Interplanetary Flight Experiment) Authors: Betts, Bruce H.; Warmflash, David; Fraze, Raymond E.; Friedman, Louis; Vorobyova, Elena; Lilburn, Timothy G.; Smith, Amy; Rettberg, Petra; Jönsson, K. Ingemar; Ciftcioglu, Neva; Fox, George E.; Svitek, Tomas; Kirschvinck, Joseph L.; Moeller, Ralf; Wassmann, Marko; Berger, Thomas Bibcode: 2019AsBio..19.1177B Altcode: The Planetary Society's Phobos Living Interplanetary Flight Experiment (Phobos LIFE) flew in the sample return capsule of the Russian Federal Space Agency's Phobos Grunt mission and was to have been a test of one aspect of the hypothesis that life can move between nearby planets within ejected rocks. Although the Phobos Grunt mission failed, we present here the scientific and engineering design and motivation of the Phobos LIFE experiment to assist with the scientific and engineering design of similar future experiments. Phobos LIFE flew selected organisms in a simulated meteoroid. The 34-month voyage would have been the first such test to occur in the high-radiation environment outside the protection of Earth's magnetosphere for more than a few days. The patented Phobos LIFE "biomodule" is an 88 g cylinder consisting of a titanium outer shell, several types of redundant seals, and 31 individual Delrin sample containers. Phobos LIFE contained 10 different organisms, representing all three domains of life, and one soil sample. The organisms are all very well characterized, most with sequenced genomes. Most are extremophiles, and most have flown in low Earth orbit. Upon return from space, the health and characteristics of organisms were to have been compared with controls that remained on Earth and have not yet been opened. Title: First Results from the Lunar Lander Neutron and Dosimetry Experiment (LND) on China's Chang'E 4 mission to the far side of the Moon Authors: Wimmer-Schweingruber, Robert F.; Zhang, Shenyi; Yu, Jia; Böttcher, Stephan I.; Burmeister, Sönke; Lohf, Henning; Guo, Jingnan; Xu, Zigong; Berger, Thomas; Hellweg, Christine; Matthiä, Daniel Bibcode: 2019EPSC...13.1289W Altcode: Chang'E 4 is the Chinese mission which landed on the far side of the Moon at 02:26 UTC on January 3, 2019. It consists of a lander, a rover, and an re- lay spacecraft. We will present first results from the Lunar Lander Neutron and Dosimetry (LND) Experi- ment aboard Chang'E 4. LND has obtained first active dosimetric measurements on the surface of the Moon, both of the charged as well as neutral radiation com- ponent. Title: Measurements of radiation quality factor on Mars with the Mars Science Laboratory Radiation Assessment Detector Authors: Zeitlin, C.; Hassler, D. M.; Ehresmann, B.; Rafkin, S. C. R.; Guo, J.; Wimmer-Schweingruber, R. F.; Berger, T.; Matthiä, D. Bibcode: 2019LSSR...22...89Z Altcode: We report the first long-term measurements of the radiation quality factor of energetic charged particles on the surface of Mars. The Radiation Assessment Detector (RAD) aboard the Mars Science Laboratory rover, also known as Curiosity, has been operating on Mars since 2012. RAD contains thin silicon detectors that record the ionization energy loss of energetic charged particles. The particles are dominantly galactic cosmic rays (GCRs) and the products of their interactions in the Martian atmosphere, with occasional contributions from solar energetic particles (SEPs). The quality factor on the surface of Mars is influenced by two factors: variations in the shielding provided by the atmosphere, and changes in the spectrum of the incident energetic particle flux due to the 11-year solar cycle. The two cannot be easily disentangled using the data alone, but insights can be gained from calculations and Monte Carlo simulations. Title: Photochemistry on the Space Station—Antibody Resistance to Space Conditions after Exposure Outside the International Space Station Authors: Coussot, Gaëlle; Le Postollec, Aurélie; Faye, Clément; Baqué, Mickaël; Vandenabeele-Trambouze, Odile; Incerti, Sébastien; Vigier, Flavie; Chaput, Didier; Cottin, Hervé; Przybyla, Bartos; Berger, Thomas; Dobrijevic, Michel Bibcode: 2019AsBio..19.1053C Altcode: Antibody-based analytical instruments are under development to detect signatures of life on planetary bodies. Antibodies are molecular recognition reagents able to detect their target at sub-nanomolar concentrations, with high affinity and specificity. Studying antibody binding performances under space conditions is mandatory to convince space agencies of the adequacy of this promising tool for planetary exploration. To complement previous ground-based experiments on antibody resistance to simulated irradiation, we evaluate in this paper the effects of antibody exposure to real space conditions during the EXPOSE-R2 mission outside the International Space Station. The absorbed dose of ionizing radiation recorded during the 588 days of this mission (220 mGy) corresponded to the absorbed dose expected during a mission to Mars. Moreover, samples faced, at the same time as irradiation, thermal cycles, launch constraints, and long-term storage. A model biochip was used in this study with antibodies in freeze-dried form and under two formats: free or covalently grafted to a solid surface. We found that antibody-binding performances were not significantly affected by cosmic radiation, and more than 40% of the exposed antibody, independent of its format, was still functional during all this experiment. We conclude that antibody-based instruments are well suited for in situ analysis on planetary bodies. Title: Photochemistry on the Space Station—Aptamer Resistance to Space Conditions: Particles Exposure from Irradiation Facilities and Real Exposure Outside the International Space Station Authors: Coussot, Gaëlle; Le Postollec, Aurélie; Incerti, Sébastien; Baqué, Mickaël; Faye, Clément; Vandenabeele-Trambouze, Odile; Cottin, Hervé; Ravelet, Corinne; Peyrin, Eric; Fiore, Emmanuelle; Vigier, Flavie; Caron, Jérôme; Chaput, Didier; Przybyla, Bartos; Berger, Thomas; Dobrijevic, Michel Bibcode: 2019AsBio..19.1063C Altcode: Some microarray-based instruments that use bioaffinity receptors such as antibodies or aptamers are under development to detect signatures of past or present life on planetary bodies. Studying the resistance of such instruments against space constraints and cosmic rays in particular is a prerequisite. We used several ground-based facilities to study the resistance of aptamers to various types of particles (protons, electrons, neutrons, and carbon ions) at different energies and fluences. We also tested the resistance of aptamers during the EXPOSE-R2 mission outside the International Space Station (ISS). The accumulated dose measured after the 588 days of this mission (220 mGy) corresponds to the accumulated dose that can be expected during a mission to Mars. We found that the recognition ability of fluorescently labeled aptamers was not significantly affected during short-term exposure experiments taking into account only one type of radiation at a time. However, we demonstrated that the same fluorescent dye was significantly affected by temperature variations (-21°C to +58°C) and storage throughout the entirety of the ISS experiment (60% of signal loss). This induced a large variability of aptamer signal in our analysis. However, we found that >50% of aptamers were still functional after the whole EXPOSE-R2 mission. We conclude that aptamer-based instruments are well suited for in situ analysis on planetary bodies, but the detection step requires additional investigations. Title: VizieR Online Data Catalog: Radial velocities and transit times for KOI 4 (Chontos+, 2019) Authors: Chontos, A.; Huber, D.; Latham, D. W.; Bieryla, A.; van Eylen, V.; Bedding, T. R.; Berger, T.; Buchhave, L. A.; Campante, T. L.; Chaplin, W. J.; Colman, I. L.; Coughlin, J. L.; Davies, G.; Hirano, T.; Howard, A. W.; Isaacson, H. Bibcode: 2019yCat..51570192C Altcode: Following the asteroseismic reclassification of the host star, we initiated an intensive radial velocity (RV) follow-up program using the Tillinghast Reflector Echelle Spectrograph (TRES), a fiber-fed echelle spectrograph spanning the spectral range of 3900-9100 Å with a resolving power of R~44000. We obtained 23 spectra with TRES between UT 2009 November 8 and 2017 September 13 using the medium 2.3" fiber. The spectra were reduced and extracted as outlined in Buchhave et al. (2010, J/ApJ/720/1118). The average exposure time of ~1800 s, corresponding to a mean signal-to-noise ratio (S/N) per resolution element of ~53 at the peak of the continuum near the Mg b triplet at 519 nm. We used the strongest S/N spectrum as a template to derive relative RVs by cross-correlating the remaining spectra order-by-order against the template, which is given a relative velocity of 0 km/s, by definition. (2 data files). Title: Coronal Condensation at Preferential Topological Locations: The Birth of Solar Prominences and Coronal Rain Authors: Liu, Wei; Sun, Xudong; Yu, Sijie; Antolin, Patrick; Titov, Viacheslav; Downs, Cooper; Berger, Thomas Bibcode: 2019AAS...23412502L Altcode: The million-degree hot and tenuous solar coronal plasma, under certain conditions, can enigmatically undergo a radiative cooling instability and condense into material of 100 times cooler in the form of prominences or coronal rain. Where, when, and how such cooling condensation takes place remain poorly understood. Answers to these questions are not only of scientific importance in their own right, but also bear implications for the fundamental question of coronal heating and the chromosphere-corona mass cycle. Magnetic fields in the magnetized corona undoubtedly play a crucial role (e.g., by trapping the plasma), but where and how? We report recent imaging and spectroscopic observations from SDO/AIA/HMI and IRIS that can shed light on these puzzles. Through a systematic survey, we found that a large fraction of quiet-Sun condensations preferentially occur at the dips of coronal loops or funnels. Such dips are located at/near magnetic topological features, such as null points and quasi-separatrix layers (QSLs), which are regions characterized by high values of the squashing factor. We also identified evidence of magnetic reconnection at such locations, which can produce favorable conditions, e.g., density enhancement by compression and/or mass trapping in plasmoids, that can trigger run-away radiative cooling. We will discuss the significance and broader implications of these novel observations. Title: Solar Polar Observing Constellation (SPOC): A New Age for Solar Observations Authors: Upton, Lisa; Berger, Thomas; Duncan, Nicole; Bosanac, Natasha Bibcode: 2019AAS...23410614U Altcode: Current observing platforms can only measure the solar magnetic field over a portion of the Earth-facing hemisphere, forcing us to rely on solar rotation to build up fictional "synoptic maps" of the full-Sun field over 27-days. The lack of magnetic field "boundary conditions" over the full Sun represents a fundamental gap in our ability to accurately model the solar coronal magnetic field and solar wind acceleration. Views restricted to the ecliptic plane cannot capture the Sun's polar regions. Observation of the poles from a high latitude vantage point are needed to advance helioseismology and constrain the Sun's polar fields and high latitude flows, which are crucial to understanding the solar activity cycle. Furthermore, sustained observation of the Sun's polar regions will enable helioseismology investigations of the polar subsurface flows, allowing us to probe deeper into the mechanisms of the solar cycle. We propose a novel constellation of small satellites called the Solar Polar Observing Constellation (SPOC) that will obtain magnetic field and doppler velocity measurements from a solar polar orbit, including nearly direct overhead measurements of the poles. The SPOC constellation consists of two identical satellites placed into 90-degree inclination heliocentric orbits using Jupiter gravitational assist (JGA) trajectories and ion electric propulsion to circularize the orbit at about 0.9 AU. Instrumentation includes a compact helioseismic magnetic imager, compact coronagraph, and in-situ solar wind plasma measuring instruments. The SPOC mission follows the model of "hybrid operational-research" missions developed by the CU Space Weather Technology, Research, and Education (SWx-TREC) to enhance utility and collaboration by developing critical operational data sources for space weather forecasting that can also produce exploratory science data. Title: Deep Learning and Feature Engineering for Solar Flare Prediction Authors: Carande, Wendy Hawley; Berger, Tom; Cai, Justin; Craft, James; Hartnett, Maxine; Jones, Andrew; Newman, William; Pankratz, Chris; Woods, Tom Bibcode: 2019shin.confE.156C Altcode: Space weather events can inflict chaos on our modern, technologically-dependent world, such as degradation, and sometimes even disruption, for our telecommunications, power grids, navigation systems, and satellite operations. Therefore, improving the accuracy in predicting such events is of the upmost importance. With this in mind, we built a deep learning system capable of predicting M and X class solar flares in a 24 hour time window, and we achieved a True Skill Score of 0.9. The inputs to our deep learning algorithm are magnetograms from the Solar Dynamics Observatory Helioseismic and Magnetic Imager (SDO/HMI), and the output is a binary classification indicating whether or not a solar flare will occur in the time window. The highest True Skill Scores were attained with the convolutional neural networks AlexNet and VGGNet. We are currently working to incorporate SDO Extreme ultraviolet Variability (EVE) time series data into our existing deep learning framework. As we add more data, we anticipate a richer model with increased predictive power. Using examples and results from our convolutional neural network and multilayer perceptron models, we’ll present how we approached challenges and sought to fix them and what methods we propose as we further develop our models. We’ll also present the importance of feature engineering as it relates to solar flare prediction, and the obstacles and rewards of creating our own in-house features, including polarity inversion lines. Title: Calibrating GONG Magnetograms Using MURaM as Ground Truth Authors: Plowman, Joseph; Petrie, Gordon; Berger, Tom Bibcode: 2019shin.confE.223P Altcode: Results of a GONG calibration based on an end-to-end simulation of its measurement process are presented. The calibration begins with a MuRAM 3D MHD simulation, models solar radiative transfer of the GONG nickel line, emulates the GONG measurement process, and inverts the resulting synthetic GONG observations to produce magnetograms. The theory of producing calibration curves from comparison of synthetic magnetograms with the corresponding ground truth is then considered, and the resulting calibration curves are shown. The implications of these results for space weather applications are discussed, and they also shed new light on the old question of the relative calibration of magnetographs. Title: SWx TREC: An Open Space Weather (SWx) R2O Development and Testbed Environment Authors: Craft, James; Pankratz, Chris; Berger, Thomas; Thayer, Jeffrey; Baltzer, Thomas; Baker, Daniel Bibcode: 2019EGUGA..2112073C Altcode: The Chancellor of the University of Colorado recently awarded a Grand Challenge grant to a group of departments and labs for the development of the Space Weather Technology, Research and Education Center (https://www.colorado.edu/spaceweather/). As part of this effort, the Laboratory for Atmospheric and Space Physics (LASP) is developing a Space Weather Testbed to provide a platform to explore research and development models side-by-side with operational standards. The Space Weather Testbed is being built using technologies employed by LASP Data Systems for the Magnetospheric Multiscale Mission Science Data Center and the Emirates Mars Mission Science Data Center. These data centers provide a managed computational environment for independent science teams to deploy their processing software into the operational system. This poster will discuss the technologies that will be used in producing the Space Weather Testbed and how the exploration between Operations to Research (O2R) and Research to Operations (R2O) will be supported. Title: Constraining the Spin-Dependent WIMP-Nucleon Cross Sections with XENON1T Authors: Aprile, E.; Aalbers, J.; Agostini, F.; Alfonsi, M.; Althueser, L.; Amaro, F. D.; Anthony, M.; Antochi, V. C.; Arneodo, F.; Baudis, L.; Bauermeister, B.; Benabderrahmane, M. L.; Berger, T.; Breur, P. A.; Brown, A.; Brown, A.; Brown, E.; Bruenner, S.; Bruno, G.; Budnik, R.; Capelli, C.; Cardoso, J. M. R.; Cichon, D.; Coderre, D.; Colijn, A. P.; Conrad, J.; Cussonneau, J. P.; Decowski, M. P.; de Perio, P.; di Gangi, P.; di Giovanni, A.; Diglio, S.; Elykov, A.; Eurin, G.; Fei, J.; Ferella, A. D.; Fieguth, A.; Fulgione, W.; Gallo Rosso, A.; Galloway, M.; Gao, F.; Garbini, M.; Grandi, L.; Greene, Z.; Hasterok, C.; Hogenbirk, E.; Howlett, J.; Iacovacci, M.; Itay, R.; Joerg, F.; Kazama, S.; Kish, A.; Koltman, G.; Kopec, A.; Landsman, H.; Lang, R. F.; Levinson, L.; Lin, Q.; Lindemann, S.; Lindner, M.; Lombardi, F.; Lopes, J. A. M.; López Fune, E.; Macolino, C.; Mahlstedt, J.; Manfredini, A.; Marignetti, F.; Marrodán Undagoitia, T.; Masbou, J.; Masson, D.; Mastroianni, S.; Messina, M.; Micheneau, K.; Miller, K.; Molinario, A.; Morâ, K.; Mosbacher, Y.; Murra, M.; Naganoma, J.; Ni, K.; Oberlack, U.; Odgers, K.; Pelssers, B.; Piastra, F.; Pienaar, J.; Pizzella, V.; Plante, G.; Podviianiuk, R.; Priel, N.; Qiu, H.; Ramírez García, D.; Reichard, S.; Riedel, B.; Rizzo, A.; Rocchetti, A.; Rupp, N.; Dos Santos, J. M. F.; Sartorelli, G.; Šarčević, N.; Scheibelhut, M.; Schindler, S.; Schreiner, J.; Schulte, D.; Schumann, M.; Scotto Lavina, L.; Selvi, M.; Shagin, P.; Shockley, E.; Silva, M.; Simgen, H.; Therreau, C.; Thers, D.; Toschi, F.; Trinchero, G.; Tunnell, C.; Upole, N.; Vargas, M.; Wack, O.; Wang, H.; Wang, Z.; Wei, Y.; Weinheimer, C.; Wenz, D.; Wittweg, C.; Wulf, J.; Xu, Z.; Ye, J.; Zhang, Y.; Zhu, T.; Zopounidis, J. P.; Xenon Collaboration Bibcode: 2019PhRvL.122n1301A Altcode: 2019arXiv190203234A We report the first experimental results on spin-dependent elastic weakly interacting massive particle (WIMP) nucleon scattering from the XENON1T dark matter search experiment. The analysis uses the full ton year exposure of XENON1T to constrain the spin-dependent proton-only and neutron-only cases. No significant signal excess is observed, and a profile likelihood ratio analysis is used to set exclusion limits on the WIMP-nucleon interactions. This includes the most stringent constraint to date on the WIMP-neutron cross section, with a minimum of 6.3 ×10-42 cm2 at 30 GeV /c2 and 90% confidence level. The results are compared with those from collider searches and used to exclude new parameter space in an isoscalar theory with an axial-vector mediator. Title: The Lunar Lander Neutron and Dosimetry (LND) Experiment on Chang'E4 Authors: Wimmer-Schweingruber, R. F.; Zhang, S.; Yu, J.; Hellweg, C. E.; Guo, J.; Lohf, H.; Berger, T.; Böttcher, S. I.; Burmeister, S.; Knappmann, A.; Knierim, V.; Schuster, B.; Seimetz, L.; Xu, Z.; Shen, G.; Yuan, B. Bibcode: 2019LPI....50.2348W Altcode: Chang'E4 was launched on December 8, 2018 and landed on January 3, 2019. We present first data from the Lunar Lander Neutron and Dosimetry (LND) Experiment. Title: Limits of Life and the Habitability of Mars: The ESA Space Experiment BIOMEX on the ISS Authors: de Vera, Jean-Pierre; Alawi, Mashal; Backhaus, Theresa; Baqué, Mickael; Billi, Daniela; Böttger, Ute; Berger, Thomas; Bohmeier, Maria; Cockell, Charles; Demets, René; de la Torre Noetzel, Rosa; Edwards, Howell; Elsaesser, Andreas; Fagliarone, Claudia; Fiedler, Annelie; Foing, Bernard; Foucher, Frédéric; Fritz, Jörg; Hanke, Franziska; Herzog, Thomas; Horneck, Gerda; Hübers, Heinz-Wilhelm; Huwe, Björn; Joshi, Jasmin; Kozyrovska, Natalia; Kruchten, Martha; Lasch, Peter; Lee, Natuschka; Leuko, Stefan; Leya, Thomas; Lorek, Andreas; Martínez-Frías, Jesús; Meessen, Joachim; Moritz, Sophie; Moeller, Ralf; Olsson-Francis, Karen; Onofri, Silvano; Ott, Sieglinde; Pacelli, Claudia; Podolich, Olga; Rabbow, Elke; Reitz, Günther; Rettberg, Petra; Reva, Oleg; Rothschild, Lynn; Garcia Sancho, Leo; Schulze-Makuch, Dirk; Selbmann, Laura; Serrano, Paloma; Szewzyk, Ulrich; Verseux, Cyprien; Wadsworth, Jennifer; Wagner, Dirk; Westall, Frances; Wolter, David; Zucconi, Laura Bibcode: 2019AsBio..19..145D Altcode: BIOMEX (BIOlogy and Mars EXperiment) is an ESA/Roscosmos space exposure experiment housed within the exposure facility EXPOSE-R2 outside the Zvezda module on the International Space Station (ISS). The design of the multiuser facility supports—among others—the BIOMEX investigations into the stability and level of degradation of space-exposed biosignatures such as pigments, secondary metabolites, and cell surfaces in contact with a terrestrial and Mars analog mineral environment. In parallel, analysis on the viability of the investigated organisms has provided relevant data for evaluation of the habitability of Mars, for the limits of life, and for the likelihood of an interplanetary transfer of life (theory of lithopanspermia). In this project, lichens, archaea, bacteria, cyanobacteria, snow/permafrost algae, meristematic black fungi, and bryophytes from alpine and polar habitats were embedded, grown, and cultured on a mixture of martian and lunar regolith analogs or other terrestrial minerals. The organisms and regolith analogs and terrestrial mineral mixtures were then exposed to space and to simulated Mars-like conditions by way of the EXPOSE-R2 facility. In this special issue, we present the first set of data obtained in reference to our investigation into the habitability of Mars and limits of life. This project was initiated and implemented by the BIOMEX group, an international and interdisciplinary consortium of 30 institutes in 12 countries on 3 continents. Preflight tests for sample selection, results from ground-based simulation experiments, and the space experiments themselves are presented and include a complete overview of the scientific processes required for this space experiment and postflight analysis. The presented BIOMEX concept could be scaled up to future exposure experiments on the Moon and will serve as a pretest in low Earth orbit. Title: First Results on the Scalar WIMP-Pion Coupling, Using the XENON1T Experiment Authors: Aprile, E.; Aalbers, J.; Agostini, F.; Alfonsi, M.; Althueser, L.; Amaro, F. D.; Anthony, M.; Antochi, V. C.; Arneodo, F.; Baudis, L.; Bauermeister, B.; Benabderrahmane, M. L.; Berger, T.; Breur, P. A.; Brown, A.; Brown, A.; Brown, E.; Bruenner, S.; Bruno, G.; Budnik, R.; Capelli, C.; Cardoso, J. M. R.; Cichon, D.; Coderre, D.; Colijn, A. P.; Conrad, J.; Cussonneau, J. P.; Decowski, M. P.; de Perio, P.; di Gangi, P.; di Giovanni, A.; Diglio, S.; Elykov, A.; Eurin, G.; Fei, J.; Ferella, A. D.; Fieguth, A.; Fulgione, W.; Gallo Rosso, A.; Galloway, M.; Gao, F.; Garbini, M.; Grandi, L.; Greene, Z.; Hasterok, C.; Hogenbirk, E.; Howlett, J.; Iacovacci, M.; Itay, R.; Joerg, F.; Kaminsky, B.; Kazama, S.; Kish, A.; Koltman, G.; Kopec, A.; Landsman, H.; Lang, R. F.; Levinson, L.; Lin, Q.; Lindemann, S.; Lindner, M.; Lombardi, F.; Lopes, J. A. M.; López Fune, E.; Macolino, C.; Mahlstedt, J.; Manfredini, A.; Marignetti, F.; Marrodán Undagoitia, T.; Masbou, J.; Masson, D.; Mastroianni, S.; Messina, M.; Micheneau, K.; Miller, K.; Molinario, A.; Morâ, K.; Murra, M.; Naganoma, J.; Ni, K.; Oberlack, U.; Odgers, K.; Pelssers, B.; Piastra, F.; Pienaar, J.; Pizzella, V.; Plante, G.; Podviianiuk, R.; Priel, N.; Qiu, H.; Ramírez García, D.; Reichard, S.; Riedel, B.; Rizzo, A.; Rocchetti, A.; Rupp, N.; Dos Santos, J. M. F.; Sartorelli, G.; Šarčević, N.; Scheibelhut, M.; Schindler, S.; Schreiner, J.; Schulte, D.; Schumann, M.; Scotto Lavina, L.; Selvi, M.; Shagin, P.; Shockley, E.; Silva, M.; Simgen, H.; Therreau, C.; Thers, D.; Toschi, F.; Trinchero, G.; Tunnell, C.; Upole, N.; Vargas, M.; Wack, O.; Wang, H.; Wang, Z.; Wei, Y.; Weinheimer, C.; Wenz, D.; Wittweg, C.; Wulf, J.; Ye, J.; Zhang, Y.; Zhu, T.; Zopounidis, J. P.; Hoferichter, M.; Klos, P.; Menéndez, J.; Schwenk, A.; Xenon Collaboration Bibcode: 2019PhRvL.122g1301A Altcode: 2018arXiv181112482A We present first results on the scalar coupling of weakly interacting massive particles (WIMPs) to pions from 1 t yr of exposure with the XENON1T experiment. This interaction is generated when the WIMP couples to a virtual pion exchanged between the nucleons in a nucleus. In contrast to most nonrelativistic operators, these pion-exchange currents can be coherently enhanced by the total number of nucleons and therefore may dominate in scenarios where spin-independent WIMP-nucleon interactions are suppressed. Moreover, for natural values of the couplings, they dominate over the spin-dependent channel due to their coherence in the nucleus. Using the signal model of this new WIMP-pion channel, no significant excess is found, leading to an upper limit cross section of 6.4 ×10-46 cm2 (90% confidence level) at 30 GeV /c2 WIMP mass. Title: VizieR Online Data Catalog: Lithium abundances of KOIs from CKS spectra (Berger+, 2018) Authors: Berger, T. A.; Howard, A. W.; Boesgaard, A. M. Bibcode: 2019yCat..18550115B Altcode: One key follow-up survey of Kepler-discovered exoplanets is the California Kepler Survey (CKS) (Petigura+ 2017, J/AJ/154/107), which was proposed to measure precise stellar parameters (Teff, logg, [Fe/H], vsini) by using local thermodynamic equilibrium (LTE) modeling of Keck-HIRES spectra of ~1000 Kepler FGK stars. Most spectra have signal-to-noise ratios (S/Ns) of ~45 per pixel, or ~90 per resolution element at 6700Å, with a resolution R=55000 and wavelength coverage from 3642-7990Å. S/N ranges from ~5 to ~200. (3 data files). Title: Skynet Algorithm for Single-dish Radio Mapping. I. Contaminant-cleaning, Mapping, and Photometering Small-scale Structures Authors: Martin, J. R.; Reichart, D. E.; Dutton, D. A.; Maples, M. P.; Berger, T. A.; Ghigo, F. D.; Haislip, J. B.; Shaban, O. H.; Trotter, A. S.; Barnes, L. M.; Paggen, M. L.; Gao, R. L.; Salemi, C. P.; Langston, G. I.; Bussa, S.; Duncan, J. A.; White, S.; Heatherly, S. A.; Karlik, J. B.; Johnson, E. M.; Reichart, J. E.; Foster, A. C.; Kouprianov, V. V.; Mazlin, S.; Harvey, J. Bibcode: 2019ApJS..240...12M Altcode: 2018arXiv180806128M We present a single-dish mapping algorithm with a number of advantages over traditional techniques. (1) Our algorithm makes use of weighted modeling, instead of weighted averaging, to interpolate between signal measurements. This smooths the data, but without blurring the data beyond instrumental resolution. Techniques that rely on weighted averaging blur point sources sometimes by as much as 40%. (2) Our algorithm makes use of local, instead of global, modeling to separate astronomical signal from instrumental and/or environmental signal drift along the telescope’s scans. Other techniques, such as basket weaving, model this drift with simple functional forms (linear, quadratic, etc.) across the entirety of scans, limiting their ability to remove such contaminants. (3) Our algorithm makes use of a similar, local modeling technique to separate astronomical signal from radio-frequency interference (RFI), even if only continuum data are available. (4) Unlike other techniques, our algorithm does not require data to be collected on a rectangular grid or regridded before processing. (5) Data from any number of observations, overlapping or not, may be appended and processed together. (6) Any pixel density may be selected for the final image. We present our algorithm and evaluate it using both simulated and real data. We are integrating it into the image-processing library of the Skynet Robotic Telescope Network, which includes optical telescopes spanning four continents, and now also Green Bank Observatory’s 20 m diameter radio telescope in West Virginia. Skynet serves hundreds of professional users, and additionally tens of thousands of students, of all ages. Default data products are generated on the fly, but will soon be customizable after the fact. Title: Roadmap for Reliable Ensemble Forecasting of the Sun-Earth System Authors: Nita, Gelu; Angryk, Rafal; Aydin, Berkay; Banda, Juan; Bastian, Tim; Berger, Tom; Bindi, Veronica; Boucheron, Laura; Cao, Wenda; Christian, Eric; de Nolfo, Georgia; DeLuca, Edward; DeRosa, Marc; Downs, Cooper; Fleishman, Gregory; Fuentes, Olac; Gary, Dale; Hill, Frank; Hoeksema, Todd; Hu, Qiang; Ilie, Raluca; Ireland, Jack; Kamalabadi, Farzad; Korreck, Kelly; Kosovichev, Alexander; Lin, Jessica; Lugaz, Noe; Mannucci, Anthony; Mansour, Nagi; Martens, Petrus; Mays, Leila; McAteer, James; McIntosh, Scott W.; Oria, Vincent; Pan, David; Panesi, Marco; Pesnell, W. Dean; Pevtsov, Alexei; Pillet, Valentin; Rachmeler, Laurel; Ridley, Aaron; Scherliess, Ludger; Toth, Gabor; Velli, Marco; White, Stephen; Zhang, Jie; Zou, Shasha Bibcode: 2018arXiv181008728N Altcode: The authors of this report met on 28-30 March 2018 at the New Jersey Institute of Technology, Newark, New Jersey, for a 3-day workshop that brought together a group of data providers, expert modelers, and computer and data scientists, in the solar discipline. Their objective was to identify challenges in the path towards building an effective framework to achieve transformative advances in the understanding and forecasting of the Sun-Earth system from the upper convection zone of the Sun to the Earth's magnetosphere. The workshop aimed to develop a research roadmap that targets the scientific challenge of coupling observations and modeling with emerging data-science research to extract knowledge from the large volumes of data (observed and simulated) while stimulating computer science with new research applications. The desire among the attendees was to promote future trans-disciplinary collaborations and identify areas of convergence across disciplines. The workshop combined a set of plenary sessions featuring invited introductory talks and workshop progress reports, interleaved with a set of breakout sessions focused on specific topics of interest. Each breakout group generated short documents, listing the challenges identified during their discussions in addition to possible ways of attacking them collectively. These documents were combined into this report-wherein a list of prioritized activities have been collated, shared and endorsed. Title: Robust Chauvenet Outlier Rejection Authors: Maples, M. P.; Reichart, D. E.; Konz, N. C.; Berger, T. A.; Trotter, A. S.; Martin, J. R.; Dutton, D. A.; Paggen, M. L.; Joyner, R. E.; Salemi, C. P. Bibcode: 2018ApJS..238....2M Altcode: 2018arXiv180705276M Sigma clipping is commonly used in astronomy for outlier rejection, but the number of standard deviations beyond which one should clip data from a sample ultimately depends on the size of the sample. Chauvenet rejection is one of the oldest, and simplest, ways to account for this, but, like sigma clipping, it depends on the sample’s mean and standard deviation, neither of which are robust quantities: both are easily contaminated by the very outliers they are being used to reject. Many, more robust measures of central tendency, and of sample deviation, exist, but each has a trade-off with precision. Here we demonstrate that outlier rejection can be both very robust and very precise if decreasingly robust but increasingly precise techniques are applied in sequence. To this end, we present a variation on Chauvenet rejection that we call “robust” Chauvenet rejection (RCR), which uses three decreasingly robust/increasingly precise measures of central tendency and four decreasingly robust/increasingly precise measures of sample deviation. We show this sequential approach to be very effective for a wide variety of contaminant types, even when a significant—even dominant—fraction of the sample is contaminated, and especially when the contaminants are strong. Furthermore, we have developed a bulk-rejection variant, to significantly decrease computing times, and RCR can be applied both to weighted data and when fitting parameterized models to data. We present aperture photometry in a contaminated, crowded field as an example. RCR may be used by anyone at https://skynet.unc.edu/rcr, and source code is available there as well. Title: Dark Matter Search Results from a One Ton-Year Exposure of XENON1T Authors: Aprile, E.; Aalbers, J.; Agostini, F.; Alfonsi, M.; Althueser, L.; Amaro, F. D.; Anthony, M.; Arneodo, F.; Baudis, L.; Bauermeister, B.; Benabderrahmane, M. L.; Berger, T.; Breur, P. A.; Brown, A.; Brown, A.; Brown, E.; Bruenner, S.; Bruno, G.; Budnik, R.; Capelli, C.; Cardoso, J. M. R.; Cichon, D.; Coderre, D.; Colijn, A. P.; Conrad, J.; Cussonneau, J. P.; Decowski, M. P.; de Perio, P.; di Gangi, P.; di Giovanni, A.; Diglio, S.; Elykov, A.; Eurin, G.; Fei, J.; Ferella, A. D.; Fieguth, A.; Fulgione, W.; Gallo Rosso, A.; Galloway, M.; Gao, F.; Garbini, M.; Geis, C.; Grandi, L.; Greene, Z.; Qiu, H.; Hasterok, C.; Hogenbirk, E.; Howlett, J.; Itay, R.; Joerg, F.; Kaminsky, B.; Kazama, S.; Kish, A.; Koltman, G.; Landsman, H.; Lang, R. F.; Levinson, L.; Lin, Q.; Lindemann, S.; Lindner, M.; Lombardi, F.; Lopes, J. A. M.; Mahlstedt, J.; Manfredini, A.; Marrodán Undagoitia, T.; Masbou, J.; Masson, D.; Messina, M.; Micheneau, K.; Miller, K.; Molinario, A.; Morâ, K.; Murra, M.; Naganoma, J.; Ni, K.; Oberlack, U.; Pelssers, B.; Piastra, F.; Pienaar, J.; Pizzella, V.; Plante, G.; Podviianiuk, R.; Priel, N.; Ramírez García, D.; Rauch, L.; Reichard, S.; Reuter, C.; Riedel, B.; Rizzo, A.; Rocchetti, A.; Rupp, N.; Dos Santos, J. M. F.; Sartorelli, G.; Scheibelhut, M.; Schindler, S.; Schreiner, J.; Schulte, D.; Schumann, M.; Scotto Lavina, L.; Selvi, M.; Shagin, P.; Shockley, E.; Silva, M.; Simgen, H.; Thers, D.; Toschi, F.; Trinchero, G.; Tunnell, C.; Upole, N.; Vargas, M.; Wack, O.; Wang, H.; Wang, Z.; Wei, Y.; Weinheimer, C.; Wittweg, C.; Wulf, J.; Ye, J.; Zhang, Y.; Zhu, T.; Xenon Collaboration Bibcode: 2018PhRvL.121k1302A Altcode: 2018arXiv180512562A We report on a search for weakly interacting massive particles (WIMPs) using 278.8 days of data collected with the XENON1T experiment at LNGS. XENON1T utilizes a liquid xenon time projection chamber with a fiducial mass of (1.30 ±0.01 ) t o n , resulting in a 1.0 ton yr exposure. The energy region of interest, [1.4 ,10.6 ] keVee ([4.9 ,40.9 ] keVnr ), exhibits an ultralow electron recoil background rate of [82-3+5(syst ) ±3 (stat ) ] events /(t o n yr keVee) . No significant excess over background is found, and a profile likelihood analysis parametrized in spatial and energy dimensions excludes new parameter space for the WIMP-nucleon spin-independent elastic scatter cross section for WIMP masses above 6 GeV /c2, with a minimum of 4.1 ×10-47 cm2 at 30 GeV /c2 and a 90% confidence level. Title: ESA Active Dosimeter a Technolgy Demonstration for ISS and beyond Authors: Straube, Ulrich; Berger, Thomas Bibcode: 2018cosp...42E3270S Altcode: Human presence in space has increased significantly over the last decade. Extended space flights supported by various international crews that lasted half a year and longer became a reality. Challenges to human health and well-being proofed to remain significant and increasing with mission-length and workload. Ongoing strong efforts did enable for such mission scenarios and shall do so for the future, the human journey to deep space that is intended. Several of the risks arising seem to have the potential to be mitigated and finally covered sufficiently. Despite health risks from ionizing radiation during extended exploratory deep space missions remain to be of significance and may strongly limit human presence and mission goals beyond Low Earth Orbit. The ESA Active Dosimeter [EAD] hardware enables for advanced personal dosimetry capabilities in real time. The system consists of several small portable Personal Active Dosimeters (MU = Mobile Unit's) as well as a surface attached docking station, called "Personal Storage Device (PSD)". The PSD provides data read-out data and advanced display capabilities as well as data storage and telemetry. The PSD contains a Tissue Equivalent Proportional Counter (TEPC) and an internal MU (iMU) for advanced analysis of the complex radiation environment in the space station and to ensure means of cross calibrations. The MU is applied for personal dosimetry as well as used for area monitoring purposes throughout the station. Verification of the system capabilities have been successfully executed in flight on ISS. Further utilization has been recommend by the ISS partner agencies. System developments and testing, including operations during a future flight of NASA's Orion program, is en-route. This presentation will give an overview of the relevant data from the first year of operations on ISS. Title: Round Table Discussion - Part 1: The Future of Space Radiation Research Authors: Hellweg, Christine; Ottolenghi, Andrea; Sun, Yeqing; Berger, Thomas Bibcode: 2018cosp...42E1428H Altcode: Space radiation is the "Number One Health Risk" (Chancellor et al., 2014) for long-term space missions beyond Low Earth Orbit (LEO). During space missions, astronauts are chronically exposed to galactic cosmic radiation (GCR) consisting of energetic protons, helium and heavier nuclei up to iron. This chronic exposure increases the risk for developing cancer and degenerative diseases (cataract of the eye lens, and possibly also decrements of the central nervous system (CNS) and other organ systems). The extents of these risks and the underlying mechanisms have to be further elucidated. In addition to the baseline exposure to GCR, Solar particle events (SPEs) bear the risk of acute high dose exposure, and might even provoke the acute radiation syndrome. Mitigation of the space radiation risks necessitates a multidisciplinary approach, from understanding the nature of the space radiation environment, the development of relevant radiation dosimeter systems, having the relevant tools to model the radiation environment, understanding the influence of shielding to the biological effects of space radiation, and being able to develop relevant countermeasures. The invited speakers of the cross discipline talks of the session F2.5 will discuss the upcoming challenges in the fields of space radiation physics, dosimetry, and modeling, biology and countermeasure development.References:Chancellor JC, Scott GBI,1, Sutton JP (2014) Space Radiation: The Number One Risk to Astronaut Health beyond Low Earth Orbit. Life (Basel). 2014 Sep; 4(3): 491-510. Title: The september 2017 solar energetic particle event observed by MSL/RAD on the surface of mars Authors: Ehresmann, Bent; Berger, Thomas; Reitz, Guenther; Burmeister, Soenke; Rafkin, Scot; Guo, Jingnan; Zeitlin, Cary; Wimmer-Schweingruber, Robert; Matthiä, Daniel; Lohf, Henning; Kristoffer Appel, Jan; Hassler, Donald M. Bibcode: 2018cosp...42E.966E Altcode: The Radiation Assessment Detector (RAD) has been continuously monitoring the Martian surface radiation environment in Gale crater as part of NASA's Mars Science Laboratory (MSL) mission since August 2012. On September 11 2017, RAD detected the strongest SEP event on the Martian surface to date. This event lead to the highest radiation levels since the beginning of the RAD operations in Gale crater. The SEPs associated with this solar storm increased the surface radiation dose by a factor of 3 over the course of a few hours, and the peak radiation dose was more than 50% higher than the previous maximum measured in October 2013.Here, we give an overview of the heliospheric conditions during the September 2017 solar storm, and present measurements of charged particle spectra during and before the event. RAD saw significant increases in the surface proton and helium fluxes, as well as in the neutral particles (neutrons and gamma-rays) created by interactions of the SEPs with the atmosphere and soil. Title: Scene-Setting talk: Solar Activity Forecasting in Practice Authors: Berger, Thomas Bibcode: 2018shin.confE.159B Altcode: We review the state-of-the-art in solar activity and resultant space weather event forecasting as well as some of the challenges, both Grand and mundane, as a scene-setting talk for Session 22 Title: Three-dimensional Velocity Measurements in Solar Prominence Bubbles and Combined Kelvin-Helmholtz/Rayleigh-Taylor Instability Authors: Berger, Thomas; Hillier, Andrew; Liu, Wei Bibcode: 2018cosp...42E.293B Altcode: We present measurements of flow velocities in solar prominences that display so-called "prominence bubble" events. Prominence bubbles are large-scale buoyant intrusions into prominences that rise from below and penetrate into the overlying plasma. They are believed to be due to magnetic flux emergence below prominences and can trigger Rayleigh-Taylor and Kelvin-Helmholtz instability flows as they interact with the overlying prominence. Prominence bubbles frequently result in the formation of plumes that rise into, or entirely through, the overlying prominence. This presents a mechanism for increasing magnetic flux and helicity in the associated coronal magnetic flux tubes, which are key for their eventual loss of equilibrium and eruptions as coronal mass ejections (CMEs). In this presentation, Hinode/Solar Optical Telescope (SOT) and Interface Region Imaging Spectrograph (IRIS) observations are analyzed to infer three-dimensional flow vectors in the "boundary layer" above several prominence bubble events. IRIS Doppler velocity measurements indicate flow speeds of 50-100 km/sec perpendicular to the sky plane, consistent with flow speeds inferred from combined Kelvin-Helmholtz/Rayleigh-Taylor instability analysis using typical quiescent prominence density and magnetic flux density values. With these typical values, flow speeds and magnetic flux densities within the bubbles can be inferred to be on the order of 100 km/sec and 10 Gauss, respectively. We discuss the implications of these novel results, and in particular, the potential for strong shear flows at the bubble boundary to trigger Kelvin-Helmholtz instability waves that develop into large-scale Rayleigh-Taylor instability plumes. Title: Radiation measurements and dosimetry for deep-space exploration Authors: Ehresmann, Bent; Berger, Thomas; Reitz, Guenther; Burmeister, Soenke; Rafkin, Scot; Guo, Jingnan; Zeitlin, Cary; Wimmer-Schweingruber, Robert; Matthiä, Daniel; Lohf, Henning; Kristoffer Appel, Jan; Hassler, Donald M. Bibcode: 2018cosp...42E.965E Altcode: Dosimetry and radiation monitoring are key factors for the planning of future human exploration on deep-space missions outside of Low-Earth Orbit (LEO), as radiation exposure poses one of the major health risks for astronauts in deep space. The amount of radiation dose astronauts would accumulate during typical mission scenarios and durations can potentially exceed currently allowable exposure limits within months.In space radiation monitoring the three main areas of concern are: 1) high-energy and deeply-penetrating Galactic Cosmic Rays (GCRs); 2) impulsive Solar Energetic Particle (SEP) events with high flux intensities up to a few hundred MeVs; and 3) secondary neutrons created by interactions of primary radiation with spacecraft material or planetary atmospheres and soils. Furthermore, in-situ radiation measurements provide invaluable input for radiation transport models that are used to calculate expected radiation exposures and shielding effectiveness, and subsequently potential health risks for future deep-space mission scenarios.Here, we present an overview of dosimetry in LEO, lunar orbit, and in deep space, and place the findings from years of measurements in context of what our current state of knowledge of space radiation implies for future exploration missions. Because the planet Mars is a prime goal for future exploration, we will focus in more detail on measurements conducted on the Martian surface with the Radiation Assessment Detector (RAD) as part of the Mars Science Laboratory (MSL) mission. Since Mars lacks a global magnetic field and its atmosphere is very thin, the surface is only weakly protected from impacts of GCRs and SEPs. This makes understanding and assessing the Martian surface radiation environment a key goal for future exploration. MSL/RAD has been characterizing in detail the charged and neutral particle environment induced by GCRs, as well as during short-term radiation enhancements from SEP events arriving at Mars.We will discuss the capabilities of the existing space dosimetry instrumentation, as well as highlight areas outside the current scope where we need to improve our understanding of the space radiation environment. Title: The Lunar Lander Neutron & Dosimetry (LND) Experiment on Chang'E4 Authors: Wimmer-Schweingruber, Robert; Hellweg, Christine; Berger, Thomas; Boettcher, Stephan; Burmeister, Soenke; Seimetz, Lars; Schuster, Bjoern; Guo, Jingnan; Zhang, Shenyi; Lohf, Henning; Yu, Jia; Knierim, Violetta; Shen, G.; Yuan, B. Bibcode: 2018cosp...42E3672W Altcode: Chang'E4, the next Chinese mission to the Moon, is planned to launch in December 2018 and to land on the far side of the Moon in the South Pole Aitken Basin. The mission consists of a lander, a rover, and a communication relay around the Earth-Moon L2 libration point. Here we describe the Lunar Lander Neutron & Dosimetry experiment (LND) on the lander. It consists of a stack of 10 segmented Si solid-state detectors (SSDs) which forms a particle telescope to measure charged particles (electrons 150-500 keV, protons 12-30 MeV, and heavier nuclei 15-30 MeV/nuc). A special geometrical arrangement allows observations of fast neutrons (and g-rays) which are also important for dosimetry and cosmic-ray exposure of lunar soils. Thermal neutrons are measured using a very thin Gd conversion foil which is sandwiched between two SSDs. Thermal neutrons are sensitive to subsurface water and important to understand lunar surface mixing processes. Despite the aim of landing humans on the Moon in the not too distant future, radiation measurements in the vicinity of the Moon are remarkably scarce. Fairly recent measurements in lunar orbit were provided by the Radiation Dose Monitor (RADOM) on board Chandrayaan-1. The spacecraft reached its operational 100 km circular orbit on November 12, 2008. Measurements showed a dose rate of 0.23 mGy per day averaged over 3545 hours of measurement time (20/11/2008 to 18/5/2009). Newer measurements have been provided by the Cosmic Ray Telescope for the Effects of Radiation (CRaTER) instrument on board the Lunar Reconnaissance Orbiter (LRO). CRaTER measured a radiation exposure of about 0.22 _ 0.27 mGy per day in its 50 km orbit. In comparison with these meager orbital data, there is a real dearth of data on the lunar surface. The current knowledge about the radiation environment on the surface of the Moon is based exclusively on calculations using radiation transport models with input parameters from models for the galactic cosmic ray spectra and for solar particle events. This is highly questionable, especially since we know that these models are fraught with uncertainties. Thus LND will provide the first active dosimetry measurements on the surface of the Moon.In this presentation we will discuss the science, implementation, and status of LND on China's Chang'E4 mission. Title: Are "Solar Tornadoes" Really Rotating? Authors: Liu, Wei; Chye Low, Boon; Okamoto, Joten; Berger, Thomas Bibcode: 2018cosp...42E2053L Altcode: Solar "tornadoes" have been proposed to explain certain vertical structures in prominences that exhibit apparent rotations. Yet, it remains highly controversial whether such motions are real rotations or transverse oscillations. We present a statistical study of IRIS observations that reveal no clear evidence of systematic or coherent rotations, which would otherwise result in opposite Doppler shifts, i.e., blueshifts on the one side of the vertical structure and redshifts on the other, which were not found in our sample of "tornadoes". In addition, we find in one particular case observed by SDO/AIA that the "tornado" disappeared upon the impact of an eruption that pushed its mass away along a primarily horizontal trajectory (presumably along magnetic field lines). This "tornado" shortly reformed with the replenishment of material from the return flow of some of the displaced mass back to its original location, at the dips of local magnetic field lines, followed by back and forth transverse oscillations around the dips. Such observations from both IRIS and AIA suggest that, at least for the cases being analyzed here, the apparent oscillatory motions of "tornadoes" are a result of longitudinal oscillations (like a pendulum) of dense and heavy prominence material about the local minimum of gravitational potential at the magnetic dips, an interpretation proposed and supported by a number of authors. Title: Cool Material in the Hot Solar Corona and the Chromosphere-Corona Mass Cycle Authors: Liu, Wei; Vial, Jean-Claude; Antolin, Patrick; Sun, Xudong; Berger, Thomas Bibcode: 2018cosp...42E2052L Altcode: In the million-degree hot and tenuous solar corona, under favorable conditions, some mass can undergo a radiative cooling instability and condense into material of 100 times cooler in two distinct forms - prominences and coronal rain. Being at similar temperatures, they exhibit contrasting morphologies and behaviors: a quiescent prominence usually consists of numerous long-lasting, filamentary downflow threads, while coronal rain consists of transient mass blobs falling at comparably higher speeds along well-defined, curved paths (e.g., guided by coronal loops). We report recent imaging and spectroscopic observations from SDO/AIA and IRIS of a hybrid prominence-coronal rain complex structure that suggest different magnetic environments being responsible for such distinctions. We also present an ensemble of observations of the so-called funnel prominences that reside near the dips of magnetic funnels. Regardless of their morphological and behavioral differences, a large fraction of prominence and coronal rain material eventually falls back to the chromosphere and serves as the return flow of the so-called chromosphere-corona mass cycle (the other half of this cycle is the upward transport of heated mass from the chromosphere to the corona). We estimate the downflow mass fluxes in prominences and coronal rain, and compare them with the coronal mass budget in this cycle and with the mass loss to the solar wind and coronal mass ejections (CMEs). We will discuss the broad physical implications of these observations for fundamental questions, such as coronal heating and beyond. Title: Predicting Solar Eruptive Events Using Artificial Neural Networks Authors: Poduval, Bala; Berger, Tom Bibcode: 2018shin.confE.157P Altcode: Solar eruptive events, such as coronal mass ejections (CMEs), are the major sources of space weather events, causing disruptions and damages to our technological infrastructure, and endangering humans in space. Prediction of such eruptive events is highly challenging mainly because of lack of a single physics-based model adequately representing the complex solar dynamo and the magnetized, turbulent plasma. Methods of artificial intelligence (AI) can develop algorithms to identify patterns in long-stretches of data and make effective predictions with reasonable accuracy. Making use of deep neural networks (DNNs), we make an attempt to predict a few events in the SHARP catalog. Presented here are the results and accuracies of our prediction. Title: Facilitating Advancements in Space Weather Data Availability Through a Space Weather Testbed and Data Portal Authors: Pankratz, Christopher; Baker, Daniel N.; Elkington, Scot; Berger, Thomas; Jaynes, Allison; Craft, James; Baltzer, Thomas; Sanchez, Fernando Bibcode: 2018cosp...42E2572P Altcode: Society has grown reliant on complex and highly interconnected technological systems, which makes us increasingly vulnerable to the effects of space weather events. An extreme space weather event today could conceivably impact many of the crucial systems we rely on, including disrupting operating earth-orbiting satellites, potential collapse of electrical grids, and impairing navigation, communication, and remote sensing capabilities. Thus, it is imperative that the scientific community address the question of just how severe events might become and to ensure stakeholders have access to the essential data needed for research and decision making. Stakeholders include policy makers and public safety officials who need to be informed by the facts on what might happen during extreme conditions. This requires essentially extremely timely up-to-the-minute alerts, warnings, and also forecasts of severe space weather events, which in turn demands measurements, models, and associated data products to be available via the most effective data discovery and access methods possible. Similarly, advancement in the fundamental scientific understanding of space weather processes is also vital, requiring that researchers have convenient and effective access to a wide variety of data sets and models from multiple sources. The space weather research community, as with many scientific communities, must access data from dispersed and often uncoordinated data repositories to acquire the data necessary for the analysis and modeling efforts that advance our understanding of solar influences and space physics on the Earth's environment. The University of Colorado (CU) is a leading institution in both producing data products and advancing the state of scientific understanding of space weather processes, is well positioned to address many of these issues. CU is inaugurating a dedicated Space Weather Technology, Research, and Education Center (SWx TREC) that will serve many of these needs, including implementation of an interoperable data portal intended to more effectively serve the needs of the Space Weather research community, as well as facilitating the advancement of models into production/operational use. In this presentation, we will outline the motivating factors for effective space weather data access and present plans and methods for meeting model testing/incubation needs, as well as the data management and access needs of the disparate communities who require space weather data and information. Title: Towards Space Exploration of Moon, Mars & Neos: Radiation Biological Basis Authors: Hellweg, Christine; Baumstark-Khan, Christa; Berger, Thomas Bibcode: 2018cosp...42E1427H Altcode: Radiation has emerged as the most critical issue to be resolved for long-term missions both orbital and interplanetary. Astronauts are constantly exposed to galactic cosmic radiation (GCR) of various energies at a low dose rate. Primarily late tissue sequels like genetic alterations, cancer and non-cancer effects, i.e. cataracts and degenerative diseases of e.g. the central nervous system or the cardiovascular system, are the potential risks. Cataracts were observed to occur earlier and more often in astronauts exposed to higher proportions of galactic ions (Cucinotta et al., 2001). Predictions of cancer risk and acceptable radiation exposure in space are subject to many uncertainties including the relative biological effectiveness (RBE) of space radiation especially heavy ions, dose-rate effects and possible interaction with microgravity and other spaceflight environmental factors. The initial cellular response to radiation exposure paves the way to late sequelae and starts with damage to the DNA which complexity depends on the linear energy transfer (LET) of the radiation. Repair of such complex DNA damage is more challenging and requires more time than the repair of simple DNA double strand breaks (DSB) which can be visualized by immunofluorescence staining of the phosphorylated histone 2AX (γH2AX) and might explain the observed prolonged cell cycle arrests induced by high-LET in comparison to low-LET irradiation. Unrepaired or mis-repaired DNA DSB are proposed to be responsible for cell death, mutations, chromosomal aberrations and oncogenic cell transformation. Cell killing and mutation induction are most efficient in an LET range of 90-200 keV/μm. Also the activation of transcription factors such as Nuclear Factor κB (NF-κB) and gene expression shaping the cellular radiation response depend on the LET with a peak RBE between 90 and 300 keV/μm. Such LET-RBE relationships were observed for cataract and cancer induction by heavy ions in laboratory animals, with varying maximal efficiencies. Furthermore, there is always the added risk of acute exposure to high proton fluxes during a solar particle event (SPE), which can threaten immediate survival of the astronauts in case of insufficient shielding by eliciting the acute radiation syndrome. Its symptoms depend on absorbed total radiation dose, type of radiation, the dose distribution in the body and the individual radiation sensitivity. After the prodromal stage with nausea and vomiting and a subsequent symptom-free phase, depending on dose, the hematopoietic syndrome with suppression of the acquired immune system and thrombocytopenia (0.7-4 Sv), the gastrointestinal tract syndrome (5-12 Sv) or the central nervous system syndrome (> 20 Sv) develop and they are accompanied by exacerbated innate immune responses. Exposure to large SPE has to be avoided by warning systems and stay inside a radiation shelter during the event. Treatment options encompass e.g. the administration of colony-stimulating factors (CSF), growth factors and blood transfusions to overcome the hematopoietic syndrome and the administration of antibiotics against secondary infections. A concerted action of ground-based studies and space experiments is required to improve the radiobiological basis of space radiation risk assessment and countermeasure development.Reference:Cucinotta FA, Manuel FK, Jones J, Iszard G, Murrey J, Djojonegro B and Wear M (2001) Space Radiation and Cataracts in Astronauts. Rad Res 156, 460-466 Title: The DOSIS 3D Project Onboard the International Space Station - Analysis of the Solar Particle Event in September 2017 Authors: Burmeister, Soenke; Berger, Thomas; Matthiä, Daniel; Bruedern, Maximilian Bibcode: 2018cosp...42E.473B Altcode: Besides the effects of the microgravity environment, and the psychological and psychosocial problems encountered in confined spaces, radiation is the main health detriment for long duration human space missions. The radiation environment encountered in space differs in nature from that on earth, consisting mostly of high energetic ions from protons up to iron, resulting in radiation levels far exceeding the ones encountered on earth for occupational radiation workers. Accurate knowledge of the physical characteristics of the space radiation field in dependence on the solar activity, the orbital parameters and the different shielding configurations of the International Space Station ISS is therefore needed. As a follow up to the DOSIS experiment (2009 - 2011) DOSIS 3D measures since May 2012 the spatial and temporal variations of the radiation field in Columbus. The active part the DOSIS MAIN BOX thereby consist of two active radiation detectors (Dosimetry Telescopes = DOSTELs) with a DDPU (DOSTEL Data and Power Unit) is mounted in a Nomex pouch at a fixed location in the bottom area of the European Physiology Module rack (EPM).The temporal variation in dependence of ISS altitude and solar cycle has been measured with the DOSTEL instruments since May 2012 covering thereby already 6 years of continuous measurements in the frame of DOSIS 3D. Of special interest was the first Solar Particle Event (SPE) (GLE 72) measured inside the Space Station within the DOSIS 3D project in September 2017. This was the first event measured since 2012 inside the ISS and in terms of exploration missions extremely important, since it was also measured in Moon orbit and at the surface of Mars. The presentation will focus on the timeline of the event observed inside Columbus and provide data for dose and relevant energy deposition spectra and also show first comparisons with GEANT4 simulations. It will also provide comparison with events observed with DOSTEL like instruments on space station MIR (1997) and on ISS (2001).The CAU contributions to DOSIS and DOSIS 3D are financially supported by BMWi under Grants 50WB0826, 50WB1026, 50WB1232 and 50WB1533. Title: The 2015 - Present Rise of the GCR as observed by RAD on Mars Authors: Wimmer-Schweingruber, Robert; Berger, Thomas; Reitz, Guenther; Burmeister, Soenke; Guo, Jingnan; Ehresmann, Bent; Zeitlin, Cary; Matthiä, Daniel; Lohf, Henning; Hassler, Donald M.; von Forstner, Johan Lauritz Freiherr; Khaksari, Salman; Thorben Lundt, Niklas Bibcode: 2018cosp...42E3670W Altcode: The radiation exposure due to galactic cosmic rays has been rising since early 2015 and is reaching some of the highest levels observed in the space age. This observation is not limited to the near-Earth space environment, but is also seen at Mars in measurements performed by the highly capable Radiation Assessment Detector (RAD) on NASA's Curiosity rover. We will discuss the increased radiation exposure at Mars and elsewhere, put into the larger heliospheric context and discuss implications for human exploration. Title: Space Radiation and Human Exploration on the Moon, Mars and Neos - Dosimetry, Models and Challenges Authors: Berger, Thomas; Hellweg, Christine; Uchihori, Yukio; Matthiä, Daniel Bibcode: 2018cosp...42E.294B Altcode: Space programs are shifting towards planetary exploration and, in particular, towards missions by human beings to the Moon and to Mars. Radiation is considered to be one of the major hazards for human long-term missions beyond Low Earth Orbit (LEO). During transit to these far away destinations and during relevant extravehicular activities (EVA) on their surface, complete shielding of the highly energetic particles is impracticable. The two sources of radiation that can impact a mission outside the Earth's magnetic field are Solar Energetic Particles (SEP) and Galactic Cosmic Rays (GCR). The main goal for exploration missions is therefore the quantification and reduction of space radiation health hazards, with the goal of maximizing the number of days that may be spent in space. The research to be carried out has to support all phases of exploration including mission planning, component design, operation and post-flight studies. Having this in mind this calls for novel and improved radiation detector assemblies as well as extended calibrations, detector intercomparisons and analysis algorithms. New measurements are a prerequisite for reliable risk assessment, a crucial input for radiation source modelling, and are also needed for real-time calibration of the detectors thereby allowing for a detailed understanding of the radiation environment the astronauts are going to live in. For exploration missions, radiation risk assessment will predominately rely on simulation models. The reliability of these models needs to be optimized through a series of tests against a wide set of measurements at sites/conditions where instruments are available or can be made available. More and more radiation details are needed to correctly assess radiation risks, and this requires detailed model outputs to be tested against proper measurements. In the last years various radiation detector systems have been send either to the Moon (circulating in Moon orbit) or are already on the surface of Mars, providing thereby a tremendously needed data set for model validation and benchmarking and input data to face the challenges ahead of us. Title: Space Weather - Technology, Research, and Education Center (SWx-TREC) Authors: Baker, Daniel N.; Thayer, Jeffrey; Berger, Thomas Bibcode: 2018cosp...42E.164B Altcode: SWx-TREC is a new Center at the University of Colorado - Boulder initiated under a grant intended to create a center of gravity for the many units at CU working on space weather topics. TREC will be in the College of Engineering and Applied Science and the Laboratory for Atmospheric and Space Physics (LASP). It will be able to work across the usual academic boundaries to better develop and integrate space weather models, missions, and data that will have a direct benefit to the operational forecasting offices. TREC will also be the focal point for creating undergraduate, graduate, and professional courses in space weather. TREC is currently making strategic investments in research-to-operations (R2O) projects such as an improved full-physics model of Low-Earth-Orbit satellite and debris drag, as well as operations-to-research (O2R) projects including improvements to solar magnetic field measurements and models that form the basis of operational solar wind forecasting models. In addition, TREC will host a "space weather data portal" and a forecast center "test bed", enabling close interaction between operational forecasters and researchers from around the nation and the world. In short, TREC is a new academic research and technology center dedicated to helping bridge the gap between space weather research and operations, and to educating the space science workforce, from undergraduates to industry professionals. TREC will work with national and international operational forecast centers, industry, other academic groups, and NSF and NASA centers such as the NASA/NSF CCMC, to develop and transition new models and tools that improve space weather forecasting and nowcasting. TREC will also be focusing significant effort on its educational mission in alignment with CU's mission as a leading space science university. Title: Implications of the September 2017 Solar Particle Event for Human Exploration of Mars Authors: Hassler, Donald M.; Berger, Thomas; Reitz, Guenther; Burmeister, Soenke; Guo, Jingnan; Ehresmann, Bent; Zeitlin, Cary; Wimmer-Schweingruber, Robert; Matthiä, Daniel Bibcode: 2018cosp...42E1393H Altcode: Although the Sun is approaching solar minimum, a series of large solar particle events (SPEs) occurred in September 2017 that impacted both Earth and Mars. In particular, the event of 10 September 2017 was the largest event that RAD has seen on the surface of Mars since it landed in 2012. Due to the modulating effect of the Martian atmosphere, the shape and intensity of these SEP spectra will differ significantly between interplanetary space and the Martian surface. Understanding how these SEP events influence the surface radiation field is crucial to assessing associated health risks for potential human missions to Mars. We will discuss in this talk the dosimetric quantities measured by MSL RAD before, during and after the Sept. 10 event, and their implications for potential human missions to Mars.MSL RAD is supported by NASA (HEOMD) under JPL subcontract #1273039 to SwRI, and by DLR in Germany under contract with Christian-Albrechts-Universitat (CAU). Title: Round Table Discussion - Part 2: The Future of Space Radiation Research Authors: Hellweg, Christine; Ottolenghi, Andrea; Sun, Yeqing; Berger, Thomas Bibcode: 2018cosp...42E1429H Altcode: Space radiation is the "Number One Health Risk" (Chancellor et al., 2014) for long-term space missions beyond Low Earth Orbit (LEO). During space missions, astronauts are chronically exposed to galactic cosmic radiation (GCR) consisting of energetic protons, helium and heavier nuclei up to iron. This chronic exposure increases the risk for developing cancer and degenerative diseases (cataract of the eye lens, and possibly also decrements of the central nervous system (CNS) and other organ systems). The extents of these risks and the underlying mechanisms have to be further elucidated. In addition to the baseline exposure to GCR, Solar particle events (SPEs) bear the risk of acute high dose exposure, and might even provoke the acute radiation syndrome. Mitigation of the space radiation risks necessitates a multidisciplinary approach, from understanding the nature of the space radiation environment, the development of relevant radiation dosimeter systems, having the relevant tools to model the radiation environment, understanding the influence of shielding to the biological effects of space radiation, and being able to develop relevant countermeasures. The invited speakers of the cross discipline talks of the session F2.5 will discuss the upcoming challenges in the fields of space radiation physics, dosimetry, and modeling, biology and countermeasure development.References:Chancellor JC, Scott GBI,1, Sutton JP (2014) Space Radiation: The Number One Risk to Astronaut Health beyond Low Earth Orbit. Life (Basel). 2014 Sep; 4(3): 491-510. Title: The DOSIS 3D Project Onboard the International Space Station - Status and Science Overview of 6 years of measurements (2012 - 2018) Authors: Berger, Thomas Bibcode: 2018cosp...42E.295B Altcode: The radiation environment encountered in space differs in nature from that on Earth, consisting mostly of highly energetic ions from protons up to iron, resulting in radiation levels far exceeding the ones present on Earth for occupational radiation workers. Since the beginning of the space era the radiation exposure during space missions has been monitored with various passive and active radiation instruments. Also on-board the International Space Station (ISS) a number of area monitoring devices provide data related to the spatial and temporal variation of the radiation field in - and outside the ISS. The aim of the DOSIS 3D (2012 - ongoing) experiment is the measurement of the radiation environment within the European Columbus Laboratory of the ISS. These measurements are, on the one hand, performed with passive radiation detectors mounted at eleven locations within Columbus for the determination of the spatial distribution of the radiation field parameters and, on the other hand, with two active radiation detectors (DOSTEL) mounted at a fixed position inside Columbus for the determination of the temporal variation of the radiation field parameters. The talk will give an overview of the current results of the data evaluation performed for the passive and active radiation detectors for DOSIS 3D in the years 2012 to 2018 and further focus on the work in progress for data comparison with other passive and active radiation detector systems measuring on-board the ISS. Acknowledgments: The participation of the Technische Universität Wien, Atominstitut (ATI), Vienna, Austria in the DOSIS-1 and -2 experiments was supported by the Austrian Space Applications Programme (ASAP) under contract no. 819643. The Polish contribution for the Institute of Nuclear Physics (IFJ), Krakow, Poland was supported by the National Science Center (project No DEC-2012/06/M/ST9/00423). MTA EK greatly acknowledges the possibility to participate in the project to DLR and to the ESA PECS for the financial grant No. PECS4000108464. The participation of the Nuclear Physics Institute of the Czech Academy of Sciences has been supported by the grant of Czech Science Foundation (GACR) No. 15-16622Y. The CAU, University of Kiel was supported by DLR under grants 50WB0826, 50WB1026, 50WB1232 and 50WB1533. Title: On the Nature of Funnel Prominences Authors: Liu, Wei; Chye Low, Boon; Berger, Thomas Bibcode: 2018cosp...42E2054L Altcode: It has been proposed that prominences are manifestations of a magneto-thermal convection process that involves ever-present dynamic descents of cool material threads and upflows of hot bubbles and plumes (Berger et al. 2011 Nature). On global scales, prominences may play an important role as the return flows of the chromosphere-corona mass cycle. A critical step in this cycle is the condensation of million-degree coronal plasma into T<10,000 K prominence material by radiative cooling instability. Direct observational evidence has been lacking for decades, a situation that has recently changed, especially with the advent of the SDO mission. We present here SDO/AIA observations of runaway cooling in coronal loops leading to condensation at magnetic dips and formation of funnel-shaped prominences (e.g., Liu et al. 2012, 2014; Berger et al. 2012 ApJL). We find that a macroscopically quiescent prominence is microscopically dynamic, involving the passage (through condensation and drainage) of a significant mass of typically 10^{15} gram/day (comparable to the mass of a typical CME). This picture is further supported by the theoretical development on spontaneous formation of current sheets and condensations (Low et al. 2012a, b, ApJ). Such funnel prominences, usually small in size, can constitute a new type of prominences. We suggest that similar processes could produce elementary building blocks of large-scale quiescent prominences in filament channels. Title: Energetic Particle Radiation Environment Observed by RAD on the Surface of Mars During the September 2017 Event Authors: Ehresmann, B.; Hassler, D. M.; Zeitlin, C.; Guo, J.; Wimmer-Schweingruber, R. F.; Matthiä, D.; Lohf, H.; Burmeister, S.; Rafkin, S. C. R.; Berger, T.; Reitz, G. Bibcode: 2018GeoRL..45.5305E Altcode: The 10-12 September Solar Energetic Particle event produced the strongest increase of the radiation environment measured by the Radiation Assessment Detector on the surface of Mars since landing in August 2012. We report the details of the measurements of the energetic particle environment from Radiation Assessment Detector in Gale crater during this event. The Solar Energetic Particle event increased the low-energy proton flux (below 100 MeV) by a factor of 30, and the higher-energy proton flux by a factor of 4, above preevent levels. The 4He flux (below 100 MeV/nuc) rose by factors up to 10, and neutral particles by a factor of 2 above background. The increase started on 10 September around 19:50 UTC, peak-level fluxes were reached on the morning of 11 September and prevailed for about 10 hr before decreasing toward background levels. The onset of a Forbush decrease on 13 September decreased the proton flux below preevent intensities. Title: Analysis of the Radiation Hazard Observed by RAD on the Surface of Mars During the September 2017 Solar Particle Event Authors: Zeitlin, C.; Hassler, D. M.; Guo, J.; Ehresmann, B.; Wimmer-Schweingruber, R. F.; Rafkin, S. C. R.; Freiherr von Forstner, J. L.; Lohf, H.; Berger, T.; Matthiae, D.; Reitz, G. Bibcode: 2018GeoRL..45.5845Z Altcode: We report dosimetric quantities measured by the Mars Science Laboratory Radiation Assessment Detector (RAD) on the surface of Mars during the 10-12 September 2017 solar particle event. Despite 23 g/cm2 of CO2 shielding provided by the atmosphere above RAD, dose rates rose above background galactic cosmic ray levels by factors of 2 to 3 over the course of several hours and leveled off at sustained peak rates for about 12 hr before declining over the following 36 hr. As the solar particle event flux was gradually declining, a shock front reached Mars and caused a sudden drop of about 15% in instantaneous dose rates. No solar particles followed the shock arrival, and the magnetic shielding of galactic cosmic rays by the shock reduced their intensity to levels below those seen before the start of the event. This event is the largest seen to date by RAD on Mars. Title: Signal yields of keV electronic recoils and their discrimination from nuclear recoils in liquid xenon Authors: Aprile, E.; Aalbers, J.; Agostini, F.; Alfonsi, M.; Amaro, F. D.; Anthony, M.; Arneodo, F.; Barrow, P.; Baudis, L.; Bauermeister, B.; Benabderrahmane, M. L.; Berger, T.; Breur, P. A.; Brown, A.; Brown, E.; Bruenner, S.; Bruno, G.; Budnik, R.; Bütikofer, L.; Calvén, J.; Cardoso, J. M. R.; Cervantes, M.; Cichon, D.; Coderre, D.; Colijn, A. P.; Conrad, J.; Cussonneau, J. P.; Decowski, M. P.; de Perio, P.; di Gangi, P.; di Giovanni, A.; Diglio, S.; Eurin, G.; Fei, J.; Ferella, A. D.; Fieguth, A.; Fulgione, W.; Gallo Rosso, A.; Galloway, M.; Gao, F.; Garbini, M.; Geis, C.; Goetzke, L. W.; Grandi, L.; Greene, Z.; Grignon, C.; Hasterok, C.; Hogenbirk, E.; Howlett, J.; Itay, R.; Kaminsky, B.; Kazama, S.; Kessler, G.; Kish, A.; Landsman, H.; Lang, R. F.; Lellouch, D.; Levinson, L.; Lin, Q.; Lindemann, S.; Lindner, M.; Lombardi, F.; Lopes, J. A. M.; Mahlstedt, J.; Manfredini, A.; Maris, I.; Marrodán Undagoitia, T.; Masbou, J.; Massoli, F. V.; Masson, D.; Mayani, D.; Messina, M.; Micheneau, K.; Molinario, A.; Morâ, K.; Murra, M.; Naganoma, J.; Ni, K.; Oberlack, U.; Pakarha, P.; Pelssers, B.; Persiani, R.; Piastra, F.; Pienaar, J.; Pizzella, V.; Piro, M. -C.; Plante, G.; Priel, N.; Ramírez García, D.; Rauch, L.; Reichard, S.; Reuter, C.; Rizzo, A.; Rupp, N.; Saldanha, R.; Dos Santos, J. M. F.; Sartorelli, G.; Scheibelhut, M.; Schindler, S.; Schreiner, J.; Schumann, M.; Scotto Lavina, L.; Selvi, M.; Shagin, P.; Shockley, E.; Silva, M.; Simgen, H.; Sivers, M. V.; Stein, A.; Thers, D.; Tiseni, A.; Trinchero, G.; Tunnell, C.; Vargas, M.; Wang, H.; Wang, Z.; Wei, Y.; Weinheimer, C.; Wittweg, C.; Wulf, J.; Ye, J.; Zhang, Y.; Zhu, T.; Xenon Collaboration Bibcode: 2018PhRvD..97i2007A Altcode: 2017arXiv170910149A We report on the response of liquid xenon to low energy electronic recoils below 15 keV from beta decays of tritium at drift fields of 92 V /cm , 154 V /cm and 366 V /cm using the XENON100 detector. A data-to-simulation fitting method based on Markov Chain Monte Carlo is used to extract the photon yields and recombination fluctuations from the experimental data. The photon yields measured at the two lower fields are in agreement with those from literature; additional measurements at a higher field of 366 V /cm are presented. The electronic and nuclear recoil discrimination as well as its dependence on the drift field and photon detection efficiency are investigated at these low energies. The results provide new measurements in the energy region of interest for dark matter searches using liquid xenon. Title: The Lunar Lander Neutron and Dosimetry (LND) Experiment on Chang'e4 Authors: Wimmer-Schweingruber, R. F.; Zhang, S.; Hellweg, C. E.; Yu, J.; Guo, J.; Lohf, H.; Berger, T.; Böttcher, S. I.; Burmeister, S.; Knappmann, A. C.; Knierim, V.; Schuster, B.; Seimetz, L.; Shen, G.; Yuan, B. Bibcode: 2018LPI....49.1413W Altcode: Chang'e4 is scheduled to launch to the far side of the Moon in December 2018. LND will measure the radiation environment in preparation of human exploration. Title: Low-Energy Cosmic Rays: Radiation Environment Studies and Astrophysics on the Deep Space Gateway Authors: Losekamm, M. J.; Berger, T. Bibcode: 2018LPICo2063.3108L Altcode: The Deep Space Gateway will be ideally located to investigate the cosmic radiation that astronauts are subjected to in deep space and to help shed light on one of the most intriguing astrophysical mysteries of today: What is the universe made of? Title: Matroshka AstroRad Radiation Experiment (MARE) on the Deep Space Gateway Authors: Gaza, R.; Hussein, H.; Murrow, D.; Hopkins, J.; Waterman, G.; Milstein, O.; Berger, T.; Przybyla, B.; Aeckerlein, J.; Marsalek, K.; Matthiae, D.; Rutczynska, A. Bibcode: 2018LPICo2063.3042G Altcode: The Matroshka AstroRad Radiation Experiment is a science payload on Orion EM-1 flight. A research platform derived from MARE is proposed for the Deep Space Gateway. Feedback is invited on desired Deep Space Gateway design features to maximize its science potential. Title: Space Weather Research and Operational Observing from a Cis-Lunar Deep Space Gateway Authors: Berger, T. E.; Baker, D. N.; Woods, T. N. Bibcode: 2018LPICo2063.3147B Altcode: We review the status of observational architectures for space weather research and operational forecasting and suggest ways in which the Deep Space Gateway may act as an ideal supplement to current and future space weather observing platforms. Title: Alamos: An International Collaboration to Provide a Space Based Environmental Monitoring Solution for the Deep Space Network Authors: Kennedy, S. O.; Dunn, A.; Lecomte, J.; Buchheim, K.; Johansson, E.; Berger, T. Bibcode: 2018LPICo2063.3069K Altcode: This abstract proposes the advantages of an externally mounted instrument in support of the human physiology, space biology, and human health and performance key science area. Alamos provides Space-Based Environmental Monitoring capabilities. Title: Results from Field Testing the RIMFAX GPR on Svalbard. Authors: Hamran, S. E.; Amundsen, H. E. F.; Berger, T.; Carter, L. M.; Dypvik, H.; Ghent, R. R.; Kohler, J.; Mellon, M. T.; Nunes, D. C.; Paige, D. A.; Plettemeier, D.; Russell, P. Bibcode: 2017AGUFM.P23G..07H Altcode: The Radar Imager for Mars' Subsurface Experiment - RIMFAX is a Ground Penetrating Radar being developed for NASÁs MARS 2020 rover mission. The principal goals of the RIMFAX investigation are to image subsurface structures, provide context for sample sites, derive information regarding subsurface composition, and search for ice or brines. In meeting these goals, RIMFAX will provide a view of the stratigraphic section and a window into the geological and environmental history of Mars. To verify the design an Engineering Model (EM) of the radar was tested in the field in the spring 2017. Different sounding modes on the EM were tested in different types of subsurface geology on Svalbard. Deep soundings were performed on polythermal glaciers down to a couple of hundred meters. Shallow soundings were used to map a ground water table in the firn area of a glacier. A combination of deep and shallow soundings was used to image buried ice under a sedimentary layer of a couple of meters. Subsurface sedimentary layers were imaged down to more than 20 meters in sand stone permafrost. This presentation will give an overview of the RIMFAX investigation, describe the development of the radar system, and show results from field tests of the radar. Title: Search for bosonic super-WIMP interactions with the XENON100 experiment Authors: Aprile, E.; Aalbers, J.; Agostini, F.; Alfonsi, M.; Althueser, L.; Amaro, F. D.; Anthony, M.; Arneodo, F.; Barrow, P.; Baudis, L.; Bauermeister, B.; Benabderrahmane, M. L.; Berger, T.; Breur, P. A.; Brown, A.; Brown, A.; Brown, E.; Bruenner, S.; Bruno, G.; Budnik, R.; Bütikofer, L.; Calvén, J.; Capelli, C.; Cardoso, J. M. R.; Cichon, D.; Coderre, D.; Colijn, A. P.; Conrad, J.; Cussonneau, J. P.; Decowski, M. P.; de Perio, P.; di Gangi, P.; di Giovanni, A.; Diglio, S.; Eurin, G.; Fei, J.; Ferella, A. D.; Fieguth, A.; Fulgione, W.; Gallo Rosso, A.; Galloway, M.; Gao, F.; Garbini, M.; Geis, C.; Goetzke, L. W.; Greene, Z.; Grignon, C.; Hasterok, C.; Hogenbirk, E.; Howlett, J.; Itay, R.; Kaminsky, B.; Kazama, S.; Kessler, G.; Kish, A.; Landsman, H.; Lang, R. F.; Lellouch, D.; Levinson, L.; Lin, Q.; Lindemann, S.; Lindner, M.; Lombardi, F.; Lopes, J. A. M.; Manfredini, A.; Maris, I.; Marrodán Undagoitia, T.; Masbou, J.; Massoli, F. V.; Masson, D.; Mayani, D.; Messina, M.; Micheneau, K.; Molinario, A.; Morâ, K.; Murra, M.; Naganoma, J.; Ni, K.; Oberlack, U.; Pakarha, P.; Pelssers, B.; Persiani, R.; Piastra, F.; Pienaar, J.; Pizzella, V.; Piro, M. -C.; Plante, G.; Priel, N.; Ramírez García, D.; Rauch, L.; Reichard, S.; Reuter, C.; Rizzo, A.; Rupp, N.; Dos Santos, J. M. F.; Sartorelli, G.; Scheibelhut, M.; Schindler, S.; Schreiner, J.; Schumann, M.; Scotto Lavina, L.; Selvi, M.; Shagin, P.; Silva, M.; Simgen, H.; Sivers, M. V.; Stein, A.; Thers, D.; Tiseni, A.; Trinchero, G.; Tunnell, C.; Vargas, M.; Wang, H.; Wang, Z.; Wei, Y.; Weinheimer, C.; Wittweg, C.; Wulf, J.; Ye, J.; Zhang, Y.; Zhu, T.; Xenon Collaboration Bibcode: 2017PhRvD..96l2002A Altcode: 2017arXiv170902222X We present results of searches for vector and pseudoscalar bosonic super-weakly interacting massive particles (WIMPs), which are dark matter candidates with masses at the keV-scale, with the XENON100 experiment. XENON100 is a dual-phase xenon time projection chamber operated at the Laboratori Nazionali del Gran Sasso. A profile likelihood analysis of data with an exposure of 224.6 live days ×34 kg showed no evidence for a signal above the expected background. We thus obtain new and stringent upper limits in the (8 - 125 ) keV /c2 mass range, excluding couplings to electrons with coupling constants of ga e>3 ×10-13 for pseudo-scalar and α'/α >2 ×10-28 for vector super-WIMPs, respectively. These limits are derived under the assumption that super-WIMPs constitute all of the dark matter in our galaxy. Title: The XENON1T dark matter experiment Authors: Aprile, E.; Aalbers, J.; Agostini, F.; Alfonsi, M.; Amaro, F. D.; Anthony, M.; Antunes, B.; Arneodo, F.; Balata, M.; Barrow, P.; Baudis, L.; Bauermeister, B.; Benabderrahmane, M. L.; Berger, T.; Breskin, A.; Breur, P. A.; Brown, A.; Brown, E.; Bruenner, S.; Bruno, G.; Budnik, R.; Bütikofer, L.; Calvén, J.; Cardoso, J. M. R.; Cervantes, M.; Chiarini, A.; Cichon, D.; Coderre, D.; Colijn, A. P.; Conrad, J.; Corrieri, R.; Cussonneau, J. P.; Decowski, M. P.; de Perio, P.; Gangi, P. Di; Giovanni, A. Di; Diglio, S.; Disdier, J. -M.; Doets, M.; Duchovni, E.; Eurin, G.; Fei, J.; Ferella, A. D.; Fieguth, A.; Franco, D.; Front, D.; Fulgione, W.; Rosso, A. Gallo; Galloway, M.; Gao, F.; Garbini, M.; Geis, C.; Giboni, K. -L.; Goetzke, L. W.; Grandi, L.; Greene, Z.; Grignon, C.; Hasterok, C.; Hogenbirk, E.; Huhmann, C.; Itay, R.; James, A.; Kaminsky, B.; Kazama, S.; Kessler, G.; Kish, A.; Landsman, H.; Lang, R. F.; Lellouch, D.; Levinson, L.; Lin, Q.; Lindemann, S.; Lindner, M.; Lombardi, F.; Lopes, J. A. M.; Maier, R.; Manfredini, A.; Maris, I.; Undagoitia, T. Marrodán; Masbou, J.; Massoli, F. V.; Masson, D.; Mayani, D.; Messina, M.; Micheneau, K.; Molinario, A.; Morå, K.; Murra, M.; Naganoma, J.; Ni, K.; Oberlack, U.; Orlandi, D.; Othegraven, R.; Pakarha, P.; Parlati, S.; Pelssers, B.; Persiani, R.; Piastra, F.; Pienaar, J.; Pizzella, V.; Piro, M. -C.; Plante, G.; Priel, N.; García, D. Ramírez; Rauch, L.; Reichard, S.; Reuter, C.; Rizzo, A.; Rosendahl, S.; Rupp, N.; Santos, J. M. F. dos; Saldanha, R.; Sartorelli, G.; Scheibelhut, M.; Schindler, S.; Schreiner, J.; Schumann, M.; Lavina, L. Scotto; Selvi, M.; Shagin, P.; Shockley, E.; Silva, M.; Simgen, H.; Sivers, M. v.; Stern, M.; Stein, A.; Tatananni, D.; Tatananni, L.; Thers, D.; Tiseni, A.; Trinchero, G.; Tunnell, C.; Upole, N.; Vargas, M.; Wack, O.; Walet, R.; Wang, H.; Wang, Z.; Wei, Y.; Weinheimer, C.; Wittweg, C.; Wulf, J.; Ye, J.; Zhang, Y. Bibcode: 2017EPJC...77..881A Altcode: 2017arXiv170807051X The XENON1T experiment at the Laboratori Nazionali del Gran Sasso (LNGS) is the first WIMP dark matter detector operating with a liquid xenon target mass above the ton-scale. Out of its 3.2 t liquid xenon inventory, 2.0 t constitute the active target of the dual-phase time projection chamber. The scintillation and ionization signals from particle interactions are detected with low-background photomultipliers. This article describes the XENON1T instrument and its subsystems as well as strategies to achieve an unprecedented low background level. First results on the detector response and the performance of the subsystems are also presented. Title: First Dark Matter Search Results from the XENON1T Experiment Authors: Aprile, E.; Aalbers, J.; Agostini, F.; Alfonsi, M.; Amaro, F. D.; Anthony, M.; Arneodo, F.; Barrow, P.; Baudis, L.; Bauermeister, B.; Benabderrahmane, M. L.; Berger, T.; Breur, P. A.; Brown, A.; Brown, A.; Brown, E.; Bruenner, S.; Bruno, G.; Budnik, R.; Bütikofer, L.; Calvén, J.; Cardoso, J. M. R.; Cervantes, M.; Cichon, D.; Coderre, D.; Colijn, A. P.; Conrad, J.; Cussonneau, J. P.; Decowski, M. P.; de Perio, P.; di Gangi, P.; di Giovanni, A.; Diglio, S.; Eurin, G.; Fei, J.; Ferella, A. D.; Fieguth, A.; Fulgione, W.; Gallo Rosso, A.; Galloway, M.; Gao, F.; Garbini, M.; Gardner, R.; Geis, C.; Goetzke, L. W.; Grandi, L.; Greene, Z.; Grignon, C.; Hasterok, C.; Hogenbirk, E.; Howlett, J.; Itay, R.; Kaminsky, B.; Kazama, S.; Kessler, G.; Kish, A.; Landsman, H.; Lang, R. F.; Lellouch, D.; Levinson, L.; Lin, Q.; Lindemann, S.; Lindner, M.; Lombardi, F.; Lopes, J. A. M.; Manfredini, A.; Mariş, I.; Marrodán Undagoitia, T.; Masbou, J.; Massoli, F. V.; Masson, D.; Mayani, D.; Messina, M.; Micheneau, K.; Molinario, A.; Morâ, K.; Murra, M.; Naganoma, J.; Ni, K.; Oberlack, U.; Pakarha, P.; Pelssers, B.; Persiani, R.; Piastra, F.; Pienaar, J.; Pizzella, V.; Piro, M. -C.; Plante, G.; Priel, N.; Rauch, L.; Reichard, S.; Reuter, C.; Riedel, B.; Rizzo, A.; Rosendahl, S.; Rupp, N.; Saldanha, R.; Dos Santos, J. M. F.; Sartorelli, G.; Scheibelhut, M.; Schindler, S.; Schreiner, J.; Schumann, M.; Scotto Lavina, L.; Selvi, M.; Shagin, P.; Shockley, E.; Silva, M.; Simgen, H.; Sivers, M. V.; Stein, A.; Thapa, S.; Thers, D.; Tiseni, A.; Trinchero, G.; Tunnell, C.; Vargas, M.; Upole, N.; Wang, H.; Wang, Z.; Wei, Y.; Weinheimer, C.; Wulf, J.; Ye, J.; Zhang, Y.; Zhu, T.; Xenon Collaboration Bibcode: 2017PhRvL.119r1301A Altcode: 2017arXiv170506655A We report the first dark matter search results from XENON1T, a ∼2000 -kg -target-mass dual-phase (liquid-gas) xenon time projection chamber in operation at the Laboratori Nazionali del Gran Sasso in Italy and the first ton-scale detector of this kind. The blinded search used 34.2 live days of data acquired between November 2016 and January 2017. Inside the (1042 ±12 )-kg fiducial mass and in the [5 ,40 ] keVnr energy range of interest for weakly interacting massive particle (WIMP) dark matter searches, the electronic recoil background was (1.93 ±0.25 )×10-4 events /(kg ×day ×keVee) , the lowest ever achieved in such a dark matter detector. A profile likelihood analysis shows that the data are consistent with the background-only hypothesis. We derive the most stringent exclusion limits on the spin-independent WIMP-nucleon interaction cross section for WIMP masses above 10 GeV /c2 , with a minimum of 7.7 ×10-47 cm2 for 35 -GeV /c2 WIMPs at 90% C.L. Title: Quiescent Prominence Dynamics Observed with the Hinode Solar Optical Telescope. II. Prominence Bubble Boundary Layer Characteristics and the Onset of a Coupled Kelvin-Helmholtz Rayleigh-Taylor Instability Authors: Berger, Thomas; Hillier, Andrew; Liu, Wei Bibcode: 2017ApJ...850...60B Altcode: 2017arXiv170705265B We analyze solar quiescent prominence bubble characteristics and instability dynamics using Hinode/Solar Optical Telescope data. We measure the bubble expansion rate, prominence downflows, and the profile of the boundary layer brightness and thickness as a function of time. The largest bubble analyzed rises into the prominence with a speed of about 1.3 {km} {{{s}}}-1 until it is destabilized by a localized shear flow on the boundary. Boundary layer thickness grows gradually as prominence downflows deposit plasma onto the bubble with characteristic speeds of 20{--}35 {km} {{{s}}}-1. Lateral downflows initiate from the thickened boundary layer with characteristic speeds of 25{--}50 {km} {{{s}}}-1, “draining” the layer of plasma. Strong shear flow across one bubble boundary leads to an apparent coupled Kelvin-Helmholtz Rayleigh-Taylor (KH-RT) instability. We measure shear flow speeds above the bubble of 10 {km} {{{s}}}-1 and infer interior bubble flow speeds on the order of 100 {km} {{{s}}}-1. Comparing the measured growth rate of the instability to analytic expressions, we infer a magnetic flux density across the bubble boundary of ∼10-3 T (10 Gauss) at an angle of ∼ 70^\circ to the prominence plane. The results are consistent with the hypothesis that prominence bubbles are caused by magnetic flux that emerges below a prominence, setting up the conditions for RT, or combined KH-RT, instability flows that transport flux, helicity, and hot plasma upward into the overlying coronal magnetic flux rope. Title: Search for magnetic inelastic dark matter with XENON100 Authors: Aprile, E.; Aalbers, J.; Agostini, F.; Alfonsi, M.; Amaro, F. D.; Anthony, M.; Arneodo, F.; Barrow, P.; Baudis, L.; Bauermeister, B.; Benabderrahmane, M. L.; Berger, T.; Breur, P. A.; Brown, A.; Brown, E.; Bruenner, S.; Bruno, G.; Budnik, R.; Bütikofer, L.; Calvén, J.; Cardoso, J. M. R.; Cervantes, M.; Cichon, D.; Coderre, D.; Colijn, A. P.; Conrad, J.; Cussonneau, J. P.; Decowski, M. P.; de Perio, P.; Di Gangi, P.; Di Giovanni, A.; Diglio, S.; Eurin, G.; Fei, J.; Ferella, A. D.; Fieguth, A.; Franco, D.; Fulgione, W.; Gallo Rosso, A.; Galloway, M.; Gao, F.; Garbini, M.; Geis, C.; Goetzke, L. W.; Greene, Z.; Grignon, C.; Hasterok, C.; Hogenbirk, E.; Itay, R.; Kaminsky, B.; Kessler, G.; Kish, A.; Landsman, H.; Lang, R. F.; Lellouch, D.; Levinson, L.; Lin, Q.; Lindemann, S.; Lindner, M.; Lombardi, F.; Lopes, J. A. M.; Manfredini, A.; Maris, I.; Marrodán Undagoitia, T.; Masbou, J.; Massoli, F. V.; Masson, D.; Mayani, D.; Messina, M.; Micheneau, K.; Molinario, A.; Murra, M.; Naganoma, J.; Ni, K.; Oberlack, U.; Pakarha, P.; Pelssers, B.; Persiani, R.; Piastra, F.; Pienaar, J.; Pizzella, V.; Piro, M. -C.; Plante, G.; Priel, N.; Rauch, L.; Reichard, S.; Reuter, C.; Rizzo, A.; Rosendahl, S.; Rupp, N.; dos Santos, J. M. F.; Sartorelli, G.; Scheibelhut, M.; Schindler, S.; Schreiner, J.; Schumann, M.; Scotto Lavina, L.; Selvi, M.; Shagin, P.; Silva, M.; Simgen, H.; Sivers, M. v.; Stein, A.; Thers, D.; Tiseni, A.; Trinchero, G.; Tunnell, C.; Vargas, M.; Wang, H.; Wei, Y.; Weinheimer, C.; Wulf, J.; Ye, J.; Zhang, Y. Bibcode: 2017JCAP...10..039A Altcode: 2017arXiv170405804X We present the first search for dark matter-induced delayed coincidence signals in a dual-phase xenon time projection chamber, using the 224.6 live days of the XENON100 science run II. This very distinct signature is predicted in the framework of magnetic inelastic dark matter which has been proposed to reconcile the modulation signal reported by the DAMA/LIBRA collaboration with the null results from other direct detection experiments. No candidate event has been found in the region of interest and upper limits on the WIMP's magnetic dipole moment are derived. The scenarios proposed to explain the DAMA/LIBRA modulation signal by magnetic inelastic dark matter interactions of WIMPs with masses of 58.0 GeV/c2 and 122.7 GeV/c2 are excluded at 3.3 σ and 9.3 σ, respectively. Title: Modelling the radiation on the Martian surface Authors: Matthiä, D.; Berger, T. Bibcode: 2017EPSC...11..655M Altcode: Radiation caused by galactic cosmic radiation can be harmful to electronics and is of interest for future manned missions. A model of the radiation exposure caused by galactic cosmic radiation on the Martian surface is presented and the results are compared to measurements by the Radiation Assessment (RAD) detector of the Mars Science Laboratory (MSL). Title: Exploiting different active silicon detectors in the International Space Station: ALTEA and DOSTEL galactic cosmic radiation (GCR) measurements Authors: Narici, Livo; Berger, Thomas; Burmeister, Sönke; Di Fino, Luca; Rizzo, Alessandro; Matthiä, Daniel; Reitz, Günther Bibcode: 2017JSWSC...7A..18N Altcode: The solar system exploration by humans requires to successfully deal with the radiation exposition issue. The scientific aspect of this issue is twofold: knowing the radiation environment the astronauts are going to face and linking radiation exposure to health risks. Here we focus on the first issue. It is generally agreed that the final tool to describe the radiation environment in a space habitat will be a model featuring the needed amount of details to perform a meaningful risk assessment. The model should also take into account the shield changes due to the movement of materials inside the habitat, which in turn produce changes in the radiation environment. This model will have to undergo a final validation with a radiation field of similar complexity. The International Space Station (ISS) is a space habitat that features a radiation environment inside which is similar to what will be found in habitats in deep space, if we use measurements acquired only during high latitude passages (where the effects of the Earth magnetic field are reduced). Active detectors, providing time information, that can easily select data from different orbital sections, are the ones best fulfilling the requirements for these kinds of measurements. The exploitation of the radiation measurements performed in the ISS by all the available instruments is therefore mandatory to provide the largest possible database to the scientific community, to be merged with detailed Computer Aided Design (CAD) models, in the quest for a full model validation. While some efforts in comparing results from multiple active detectors have been attempted, a thorough study of a procedure to merge data in a single data matrix in order to provide the best validation set for radiation environment models has never been attempted. The aim of this paper is to provide such a procedure, to apply it to two of the most performing active detector systems in the ISS: the Anomalous Long Term Effects in Astronauts (ALTEA) instrument and the DOSimetry TELescope (DOSTEL) detectors, applied in the frame of the DOSIS and DOSIS 3D project onboard the ISS and to present combined results exploiting the features of each of the two apparatuses. Title: The Fate of Cool Material in the Hot Corona: Solar Prominences and Coronal Rain Authors: Liu, Wei; Antolin, Patrick; Sun, Xudong; Vial, Jean-Claude; Berger, Thomas Bibcode: 2017SPD....4810501L Altcode: As an important chain of the chromosphere-corona mass cycle, some of the million-degree hot coronal mass undergoes a radiative cooling instability and condenses into material at chromospheric or transition-region temperatures in two distinct forms - prominences and coronal rain (some of which eventually falls back to the chromosphere). A quiescent prominence usually consists of numerous long-lasting, filamentary downflow threads, while coronal rain consists of transient mass blobs falling at comparably higher speeds along well-defined paths. It remains puzzling why such material of similar temperatures exhibit contrasting morphologies and behaviors. We report recent SDO/AIA and IRIS observations that suggest different magnetic environments being responsible for such distinctions. Specifically, in a hybrid prominence-coronal rain complex structure, we found that the prominence material is formed and resides near magnetic null points that favor the radiative cooling process and provide possibly a high plasma-beta environment suitable for the existence of meandering prominence threads. As the cool material descends, it turns into coronal rain tied onto low-lying coronal loops in a likely low-beta environment. Such structures resemble to certain extent the so-called coronal spiders or cloud prominences, but the observations reported here provide critical new insights. We will discuss the broad physical implications of these observations for fundamental questions, such as coronal heating and beyond (e.g., in astrophysical and/or laboratory plasma environments). Title: Intrinsic backgrounds from Rn and Kr in the XENON100 experiment Authors: XENON Collaboration; Aprile, E.; Aalbers, J.; Agostini, F.; Alfonsi, M.; Amaro, F. D.; Anthony, M.; Arneodo, F.; Barrow, P.; Baudis, L.; Bauermeister, B.; Benabderrahmane, M. L.; Berger, T.; Breur, P. A.; Brown, A.; Brown, E.; Bruenner, S.; Bruno, G.; Budnik, R.; Bütikofer, L.; Calvén, J.; Cardoso, J. M. R.; Cervantes, M.; Cichon, D.; Coderre, D.; Colijn, A. P.; Conrad, J.; Cussonneau, J. P.; Decowski, M. P.; de Perio, P.; Di Gangi, P.; Di Giovanni, A.; Diglio, S.; Eurin, G.; Fei, J.; Ferella, A. D.; Fieguth, A.; Fulgione, W.; Gallo Rosso, A.; Galloway, M.; Gao, F.; Garbini, M.; Geis, C.; Goetzke, L. W.; Greene, Z.; Grignon, C.; Hasterok, C.; Hogenbirk, E.; Itay, R.; Kaminsky, B.; Kazama, S.; Kessler, G.; Kish, A.; Landsman, H.; Lang, R. F.; Lellouch, D.; Levinson, L.; Lin, Q.; Lindemann, S.; Lindner, M.; Lombardi, F.; Lopes, J. A. M.; Manfredini, A.; Maris, I.; Marrodán Undagoitia, T.; Masbou, J.; Massoli, F. V.; Masson, D.; Mayani, D.; Messina, M.; Micheneau, K.; Molinario, A.; Morå, K.; Murra, M.; Naganoma, J.; Ni, K.; Oberlack, U.; Pakarha, P.; Pelssers, B.; Persiani, R.; Piastra, F.; Pienaar, J.; Piro, M. -C.; Pizzella, V.; Plante, G.; Priel, N.; Ramírez García, D.; Rauch, L.; Reichard, S.; Reuter, C.; Rizzo, A.; Rupp, N.; dos Santos, J. M. F.; Sartorelli, G.; Scheibelhut, M.; Schindler, S.; Schreiner, J.; Schumann, M.; Scotto Lavina, L.; Selvi, M.; Shagin, P.; Silva, M.; Simgen, H.; Sivers, M. v.; Stein, A.; Thers, D.; Tiseni, A.; Trinchero, G.; Tunnell, C.; Vargas, M.; Wang, H.; Wang, Z.; Weber, M.; Wei, Y.; Weinheimer, C.; Wulf, J.; Ye, J.; Zhang, Y. Bibcode: 2017arXiv170803617X Altcode: In this paper, we describe the XENON100 data analyses used to assess the target-intrinsic background sources radon ($^{222}$Rn), thoron ($^{220}$Rn) and krypton ($^{85}$Kr). We detail the event selections of high-energy alpha particles and decay-specific delayed coincidences. We derive distributions of the individual radionuclides inside the detector and quantify their abundances during the main three science runs of the experiment over a period of $\sim$ 4 years, from January 2010 to January 2014. We compare our results to external measurements of radon emanation and krypton concentrations where we find good agreement. We report an observed reduction in concentrations of radon daughters that we attribute to the plating-out of charged ions on the negatively biased cathode. Title: The fading of Cassiopeia A, and improved models for the absolute spectrum of primary radio calibration sources Authors: Trotter, A. S.; Reichart, D. E.; Egger, R. E.; Stýblová, J.; Paggen, M. L.; Martin, J. R.; Dutton, D. A.; Reichart, J. E.; Kumar, N. D.; Maples, M. P.; Barlow, B. N.; Berger, T. A.; Foster, A. C.; Frank, N. R.; Ghigo, F. D.; Haislip, J. B.; Heatherly, S. A.; Kouprianov, V. V.; LaCluyzé, A. P.; Moffett, D. A.; Moore, J. P.; Stanley, J. L.; White, S. Bibcode: 2017MNRAS.469.1299T Altcode: 2017arXiv170400002T Based on 5 yr of observations with the 40-foot telescope at Green Bank Observatory (GBO), Reichart & Stephens found that the radio source Cassiopeia A had either faded more slowly between the mid-1970s and late 1990s than Baars et al. had found it to be fading between the late 1940s and mid-1970s, or that it had rebrightened and then resumed fading sometime between the mid-1970s and mid-1990s, in the L band (1.4 GHz). Here, we present 15 additional years of observations of Cas A and Cyg A with the 40-foot in the L band, and three and a half additional years of observations of Cas A, Cyg A, Tau A and Vir A with GBO's recently refurbished 20-m telescope in the L and X (9 GHz) bands. We also present a more sophisticated analysis of the 40-foot data, and a reanalysis of the Baars et al. data, which reveals small, but non-negligible differences. We find that overall, between the late 1950s and late 2010s, Cas A faded at an average rate of 0.670 ± 0.019 per cent yr-1 in the L band, consistent with Reichart & Stephens. However, we also find, at the 6.3σ credible level, that it did not fade at a constant rate. Rather, Cas A faded at a faster rate through at least the late 1960s, rebrightened (or at least faded at a much slower rate), and then resumed fading at a similarly fast rate by, at most, the late 1990s. Given these differences from the original Baars et al. analysis, and given the importance of their fitted spectral and temporal models for flux-density calibration in radio astronomy, we update and improve on these models for all four of these radio sources. In doing so, we additionally find that Tau A is fading at a rate of 0.102^{+0.042}_{-0.043} per cent yr-1 in the L band. Title: The radiation environment on the surface of Mars - Numerical calculations of the galactic component with GEANT4/PLANETOCOSMICS Authors: Matthiä, Daniel; Berger, Thomas Bibcode: 2017LSSR...14...57M Altcode: Galactic cosmic radiation and secondary particles produced in the interaction with the atmosphere lead to a complex radiation field on the Martian surface. A workshop (;1st Mars Space Radiation Modeling Workshop;) organized by the MSL-RAD science team was held in June 2016 in Boulder with the goal to compare models capable to predict this radiation field with each other and measurements from the RAD instrument onboard the curiosity rover taken between November 15, 2015 and January 15, 2016. In this work the results of PLANETOCOSMICS/GEANT4 contributed to the workshop are presented. Calculated secondary particle spectra on the Martian surface are investigated and the radiation field's directionality of the different particles in dependence on the energy is discussed. Omnidirectional particle fluxes are used in combination with fluence to dose conversion factors to calculate absorbed dose rates and dose equivalent rates in a slab of tissue. Title: Effective field theory search for high-energy nuclear recoils using the XENON100 dark matter detector Authors: Aprile, E.; Aalbers, J.; Agostini, F.; Alfonsi, M.; Amaro, F. D.; Anthony, M.; Arneodo, F.; Barrow, P.; Baudis, L.; Bauermeister, B.; Benabderrahmane, M. L.; Berger, T.; Breur, P. A.; Brown, A.; Brown, E.; Bruenner, S.; Bruno, G.; Budnik, R.; Bütikofer, L.; Calvén, J.; Cardoso, J. M. R.; Cervantes, M.; Cichon, D.; Coderre, D.; Colijn, A. P.; Conrad, J.; Cussonneau, J. P.; Decowski, M. P.; de Perio, P.; di Gangi, P.; di Giovanni, A.; Diglio, S.; Eurin, G.; Fei, J.; Ferella, A. D.; Fieguth, A.; Fulgione, W.; Gallo Rosso, A.; Galloway, M.; Gao, F.; Garbini, M.; Geis, C.; Goetzke, L. W.; Greene, Z.; Grignon, C.; Hasterok, C.; Hogenbirk, E.; Itay, R.; Kaminsky, B.; Kazama, S.; Kessler, G.; Kish, A.; Landsman, H.; Lang, R. F.; Lellouch, D.; Levinson, L.; Lin, Q.; Lindemann, S.; Lindner, M.; Lombardi, F.; Lopes, J. A. M.; Manfredini, A.; Maris, I.; Marrodán Undagoitia, T.; Masbou, J.; Massoli, F. V.; Masson, D.; Mayani, D.; Messina, M.; Micheneau, K.; Molinario, A.; Morâ, K.; Murra, M.; Naganoma, J.; Ni, K.; Oberlack, U.; Pakarha, P.; Pelssers, B.; Persiani, R.; Piastra, F.; Pienaar, J.; Pizzella, V.; Piro, M. -C.; Plante, G.; Priel, N.; Rauch, L.; Reichard, S.; Reuter, C.; Rizzo, A.; Rosendahl, S.; Rupp, N.; Dos Santos, J. M. F.; Sartorelli, G.; Scheibelhut, M.; Schindler, S.; Schreiner, J.; Schumann, M.; Scotto Lavina, L.; Selvi, M.; Shagin, P.; Silva, M.; Simgen, H.; Sivers, M. V.; Stein, A.; Thers, D.; Tiseni, A.; Trinchero, G.; Tunnell, C.; Vargas, M.; Wang, H.; Wang, Z.; Wei, Y.; Weinheimer, C.; Wulf, J.; Ye, J.; Zhang., Y.; Farmer, B.; Xenon Collaboration Bibcode: 2017PhRvD..96d2004A Altcode: 2017arXiv170502614A We report on weakly interacting massive particles (WIMPs) search results in the XENON100 detector using a nonrelativistic effective field theory approach. The data from science run II (34 kg ×224.6 live days) were reanalyzed, with an increased recoil energy interval compared to previous analyses, ranging from (6.6 -240 ) keVnr . The data are found to be compatible with the background-only hypothesis. We present 90% confidence level exclusion limits on the coupling constants of WIMP-nucleon effective operators using a binned profile likelihood method. We also consider the case of inelastic WIMP scattering, where incident WIMPs may up-scatter to a higher mass state, and set exclusion limits on this model as well. Title: Prominence Bubble Shear Flows and the Coupled Kelvin-Helmholtz — Rayleigh-Taylor Instability Authors: Berger, Thomas; Hillier, Andrew Bibcode: 2017SPD....4820103B Altcode: Prominence bubbles are large arched structures that rise from below into quiescent prominences, often growing to heights on the order of 10 Mm before going unstable and generating plume upflows. While there is general agreement that emerging flux below pre-existing prominences causes the structures, there is lack of agreement on the nature of the bubbles and the cause of the instability flows. One hypothesis is that the bubbles contain coronal temperature plasma and rise into the prominence above due to both magnetic and thermal buoyancy, eventually breaking down via a magnetic Rayleigh-Taylor (RT) instability to release hot plasma and magnetic flux and helicity into the overlying coronal flux rope. Another posits that the bubbles are actually just “arcades” in the prominence indicating a magnetic separator line between the bipole and the prominence fields with the observed upflows and downflows caused by reconnection along the separator. We analyze Hinode/SOT, SDO/AIA, and IRIS observations of prominence bubbles, focusing on characteristics of the bubble boundary layers that may discriminate between the two hypotheses. We find speeds on the order of 10 km/s in prominence plasma downflows and lateral shear flows along the bubble boundary. Inflows to the boundary gradually increase the thickness and brightness of the layer until plasma drains from there, apparently around the dome-like bubble domain. In one case, shear flow across the bubble boundary develops Kelvin-Helmholtz (KH) vortices that we use to infer flow speeds in the low-density bubble on the order of 100 km/sec. IRIS spectra indicate that plasma flows on the bubble boundary at transition region temperatures achieve Doppler speeds on the order of 50 km/s, consistent with this inference. Combined magnetic KH-RT instability analysis leads to flux density estimates of 10 G with a field angle of 30° to the prominence, consistent with vector magnetic field measurements. In contrast, we find no evidence of the impulsive brightening or bi-directional jets that are expected from reconnection driven flows at bubble boundaries. We conclude that observations to date are consistent with the hot bubble/Rayleigh-Taylor instability hypothesis. Title: The radiation environment on the surface of Mars - Summary of model calculations and comparison to RAD data Authors: Matthiä, Daniel; Hassler, Donald M.; de Wet, Wouter; Ehresmann, Bent; Firan, Ana; Flores-McLaughlin, John; Guo, Jingnan; Heilbronn, Lawrence H.; Lee, Kerry; Ratliff, Hunter; Rios, Ryan R.; Slaba, Tony C.; Smith, Michael; Stoffle, Nicholas N.; Townsend, Lawrence W.; Berger, Thomas; Reitz, Günther; Wimmer-Schweingruber, Robert F.; Zeitlin, Cary Bibcode: 2017LSSR...14...18M Altcode: The radiation environment at the Martian surface is, apart from occasional solar energetic particle events, dominated by galactic cosmic radiation, secondary particles produced in their interaction with the Martian atmosphere and albedo particles from the Martian regolith. The highly energetic primary cosmic radiation consists mainly of fully ionized nuclei creating a complex radiation field at the Martian surface. This complex field, its formation and its potential health risk posed to astronauts on future manned missions to Mars can only be fully understood using a combination of measurements and model calculations. In this work the outcome of a workshop held in June 2016 in Boulder, CO, USA is presented: experimental results from the Radiation Assessment Detector of the Mars Science Laboratory are compared to model results from GEANT4, HETC-HEDS, HZETRN, MCNP6, and PHITS. Charged and neutral particle spectra and dose rates measured between 15 November 2015 and 15 January 2016 and model results calculated for this time period are investigated. Title: Search for WIMP inelastic scattering off xenon nuclei with XENON100 Authors: Aprile, E.; Aalbers, J.; Agostini, F.; Alfonsi, M.; Amaro, F. D.; Anthony, M.; Arneodo, F.; Barrow, P.; Baudis, L.; Bauermeister, B.; Benabderrahmane, M. L.; Berger, T.; Breur, P. A.; Brown, A.; Brown, E.; Bruenner, S.; Bruno, G.; Budnik, R.; Bütikofer, L.; Calvén, J.; Cardoso, J. M. R.; Cervantes, M.; Cichon, D.; Coderre, D.; Colijn, A. P.; Conrad, J.; Cussonneau, J. P.; Decowski, M. P.; de Perio, P.; di Gangi, P.; di Giovanni, A.; Diglio, S.; Eurin, G.; Fei, J.; Ferella, A. D.; Fieguth, A.; Fulgione, W.; Gallo Rosso, A.; Galloway, M.; Gao, F.; Garbini, M.; Geis, C.; Goetzke, L. W.; Greene, Z.; Grignon, C.; Hasterok, C.; Hogenbirk, E.; Itay, R.; Kaminsky, B.; Kazama, S.; Kessler, G.; Kish, A.; Landsman, H.; Lang, R. F.; Lellouch, D.; Levinson, L.; Lin, Q.; Lindemann, S.; Lindner, M.; Lombardi, F.; Lopes, J. A. M.; Manfredini, A.; Maris, I.; Marrodán Undagoitia, T.; Masbou, J.; Massoli, F. V.; Masson, D.; Mayani, D.; Messina, M.; Micheneau, K.; Molinario, A.; Mora, K.; Murra, M.; Naganoma, J.; Ni, K.; Oberlack, U.; Pakarha, P.; Pelssers, B.; Persiani, R.; Piastra, F.; Pienaar, J.; Pizzella, V.; Piro, M. -C.; Plante, G.; Priel, N.; Rauch, L.; Reichard, S.; Reuter, C.; Rizzo, A.; Rosendahl, S.; Rupp, N.; Dos Santos, J. M. F.; Sartorelli, G.; Scheibelhut, M.; Schindler, S.; Schreiner, J.; Schumann, M.; Scotto Lavina, L.; Selvi, M.; Shagin, P.; Silva, M.; Simgen, H.; Sivers, M. V.; Stein, A.; Thers, D.; Tiseni, A.; Trinchero, G.; Tunnell, C.; Vargas, M.; Wang, H.; Wang, Z.; Wei, Y.; Weinheimer, C.; Wulf, J.; Ye, J.; Zhang, Y.; Xenon Collaboration Bibcode: 2017PhRvD..96b2008A Altcode: 2017arXiv170505830A We present the first constraints on the spin-dependent, inelastic scattering cross section of weakly interacting massive particles (WIMPs) on nucleons from XENON100 data with an exposure of 7.64 ×103 kg .days . XENON100 is a dual-phase xenon time projection chamber with 62 kg of active mass, operated at the Laboratori Nazionali del Gran Sasso (LNGS) in Italy and designed to search for nuclear recoils from WIMP-nucleus interactions. Here we explore inelastic scattering, where a transition to a low-lying excited nuclear state of <mml:mmultiscripts>Xe 129 </mml:mmultiscripts> is induced. The experimental signature is a nuclear recoil observed together with the prompt deexcitation photon. We see no evidence for such inelastic WIMP-<mml:mmultiscripts>Xe 129 </mml:mmultiscripts> interactions. A profile likelihood analysis allows us to set a 90% C.L. upper limit on the inelastic, spin-dependent WIMP-nucleon cross section of 3.3 ×10-38 cm2 at 100 GeV /c2 . This is the most constraining result to date, and sets the pathway for an analysis of this interaction channel in upcoming, larger dual-phase xenon detectors. Title: DOSIS & DOSIS 3D: radiation measurements with the DOSTEL instruments onboard the Columbus Laboratory of the ISS in the years 2009-2016 Authors: Berger, Thomas; Burmeister, Sönke; Matthiä, Daniel; Przybyla, Bartos; Reitz, Günther; Bilski, Pawel; Hajek, Michael; Sihver, Lembit; Szabo, Julianna; Ambrozova, Iva; Vanhavere, Filip; Gaza, Ramona; Semones, Edward; Yukihara, Eduardo G.; Benton, Eric R.; Uchihori, Yukio; Kodaira, Satoshi; Kitamura, Hisashi; Boehme, Matthias Bibcode: 2017JSWSC...7A...8B Altcode: The natural radiation environment in Low Earth Orbit (LEO) differs significantly in composition and energy from that found on Earth. The space radiation field consists of high energetic protons and heavier ions from Galactic Cosmic Radiation (GCR), as well as of protons and electrons trapped in the Earth's radiation belts (Van Allen belts). Protons and some heavier particles ejected in occasional Solar Particle Events (SPEs) might in addition contribute to the radiation exposure in LEO. All sources of radiation are modulated by the solar cycle. During solar maximum conditions SPEs occur more frequently with higher particle intensities. Since the radiation exposure in LEO exceeds exposure limits for radiation workers on Earth, the radiation exposure in space has been recognized as a main health concern for humans in space missions from the beginning of the space age on. Monitoring of the radiation environment is therefore an inevitable task in human spaceflight. Since mission profiles are always different and each spacecraft provides different shielding distributions, modifying the radiation environment measurements needs to be done for each mission. The experiments "Dose Distribution within the ISS (DOSIS)" (2009-2011) and "Dose Distribution within the ISS 3D (DOSIS 3D)" (2012-onwards) onboard the Columbus Laboratory of the International Space Station (ISS) use a detector suite consisting of two silicon detector telescopes (DOSimetry TELescope = DOSTEL) and passive radiation detector packages (PDP) and are designed for the determination of the temporal and spatial variation of the radiation environment. With the DOSTEL instruments' changes of the radiation composition and the related exposure levels in dependence of the solar cycle, the altitude of the ISS and the influence of attitude changes of the ISS during Space Shuttle dockings inside the Columbus Laboratory have been monitored. The absorbed doses measured at the end of May 2016 reached up to 286 μGy/day with dose equivalent values of 647 μSv/day. Title: The Lunar Lander Neutron and Dosimetry (LND) Experiment on Chang'e4 Authors: Wimmer-Schweingruber, R. F.; Zhang, S.; Hellweg, C. E.; Yu, J.; Guo, J.; Lohf, H.; Berger, T.; Böttcher, S. I.; Burmeister, S.; Jüngling, M.; Knappmann, A.; Knierim, V.; Schuster, B.; Seimetz, L.; Shen, G.; Steinhagen, J.; Yuan, B. Bibcode: 2017LPI....48.1320W Altcode: The Lunar Lander Neutron and Dosimetry (LND) experiment on China's lunar mission Chang'e4 will measure the neutral and charged radiation on the lunar surface. Title: STARLIFE - An International Campaign to Study the Role of Galactic Cosmic Radiation in Astrobiological Model Systems Authors: Moeller, Ralf; Raguse, Marina; Leuko, Stefan; Berger, Thomas; Hellweg, Christine Elisabeth; Fujimori, Akira; Okayasu, Ryuichi; Horneck, Gerda Bibcode: 2017AsBio..17..101M Altcode: In-depth knowledge regarding the biological effects of the radiation field in space is required for assessing the radiation risks in space. To obtain this knowledge, a set of different astrobiological model systems has been studied within the STARLIFE radiation campaign during six irradiation campaigns (2013-2015). The STARLIFE group is an international consortium with the aim to investigate the responses of different astrobiological model systems to the different types of ionizing radiation (X-rays, γ rays, heavy ions) representing major parts of the galactic cosmic radiation spectrum. Low- and high-energy charged particle radiation experiments have been conducted at the Heavy Ion Medical Accelerator in Chiba (HIMAC) facility at the National Institute of Radiological Sciences (NIRS) in Chiba, Japan. X-rays or γ rays were used as reference radiation at the German Aerospace Center (DLR, Cologne, Germany) or Beta-Gamma-Service GmbH (BGS, Wiehl, Germany) to derive the biological efficiency of different radiation qualities. All samples were exposed under identical conditions to the same dose and qualities of ionizing radiation (i) allowing a direct comparison between the tested specimens and (ii) providing information on the impact of the space radiation environment on currently used astrobiological model organisms. Title: Search for Electronic Recoil Event Rate Modulation with 4 Years of XENON100 Data Authors: The XENON collaboration; Aprile, E.; Aalbers, J.; Agostini, F.; Alfonsi, M.; Amaro, F. D.; Anthony, M.; Arneodo, F.; Barrow, P.; Baudis, L.; Bauermeister, B.; Benabderrahmane, M. L.; Berger, T.; Breur, P. A.; Brown, A.; Brown, E.; Bruenner, S.; Bruno, G.; Budnik, R.; Butikofer, L.; Calven, J.; Cardoso, J. M. R.; Cervantes, M.; Cichon, D.; Coderre, D.; Colijn, A. P.; Conrad, J.; Cussonneau, J. P.; Decowski, M. P.; de Perio, P.; Di Gangi, P.; Di Giovanni, A.; Diglio, S.; Eurin, G.; Fei, J.; Ferella, A. D.; Fieguth, A.; Franco, D.; Fulgione, W.; Gallo Rosso, A.; Galloway, M.; Gao, F.; Garbini, M.; Geis, C.; Goetzke, L. W.; Greene, Z.; Grignon, C.; Hasterok, C.; Hogenbirk, E.; Itay, R.; Kaminsky, B.; Kessler, G.; Kish, A.; Landsman, H.; Lang, R. F.; Lellouch, D.; Levinson, L.; Lin, Q.; Lindemann, S.; Lindner, M.; Lopes, J. A. M.; Manfredini, A.; Maris, I.; Marrodan Undagoitia, T.; Masbou, J.; Massoli, F. V.; Masson, D.; Mayani, D.; Messina, M.; Micheneau, K.; Miguez, B.; Molinario, A.; Murra, M.; Naganoma, J.; Ni, K.; Oberlack, U.; Pakarha, P.; Pelssers, B.; Persiani, R.; Piastra, F.; Pienaar, J.; Pizzella, V.; Piro, M. -C.; Plante, G.; Priel, N.; Rauch, L.; Reichard, S.; Reuter, C.; Rizzo, A.; Rosendahl, S.; Rupp, N.; dos Santos, J. M. F.; Sartorelli, G.; Scheibelhut, M.; Schindler, S.; Schreiner, J.; Schumann, M.; Scotto Lavina, L.; Selvi, M.; Shagin, P.; Silva, M.; Simgen, H.; Sivers, M. v.; Stein, A.; Thers, D.; Tiseni, A.; Trinchero, G.; Tunnell, C.; Wang, H.; Wei, Y.; Weinheimer, C.; Wulf, J.; Ye, J.; Zhang, Y. Bibcode: 2017arXiv170100769T Altcode: We report on a search for electronic recoil event rate modulation signatures in the XENON100 data accumulated over a period of 4 years, from January 2010 to January 2014. A profile likelihood method, which incorporates the stability of the XENON100 detector and the known electronic recoil background model, is used to quantify the significance of periodicity in the time distribution of events. There is a weak modulation signature at a period of $431^{+16}_{-14}$ days in the low energy region of $(2.0-5.8)$ keV in the single scatter event sample, with a global significance of $1.9\,\sigma$, however no other more significant modulation is observed. The expected annual modulation of a dark matter signal is not compatible with this result. Single scatter events in the low energy region are thus used to exclude the DAMA/LIBRA annual modulation as being due to dark matter electron interactions via axial vector coupling at $5.7\,\sigma$. Title: XENON100 dark matter results from a combination of 477 live days Authors: Aprile, E.; Aalbers, J.; Agostini, F.; Alfonsi, M.; Amaro, F. D.; Anthony, M.; Arneodo, F.; Barrow, P.; Baudis, L.; Bauermeister, B.; Benabderrahmane, M. L.; Berger, T.; Breur, P. A.; Brown, A.; Brown, E.; Bruenner, S.; Bruno, G.; Budnik, R.; Bütikofer, L.; Calvén, J.; Cardoso, J. M. R.; Cervantes, M.; Cichon, D.; Coderre, D.; Colijn, A. P.; Conrad, J.; Cussonneau, J. P.; Decowski, M. P.; de Perio, P.; di Gangi, P.; di Giovanni, A.; Diglio, S.; Duchovni, E.; Fei, J.; Ferella, A. D.; Fieguth, A.; Franco, D.; Fulgione, W.; Gallo Rosso, A.; Galloway, M.; Gao, F.; Garbini, M.; Geis, C.; Goetzke, L. W.; Greene, Z.; Grignon, C.; Hasterok, C.; Hogenbirk, E.; Itay, R.; Kaminsky, B.; Kessler, G.; Kish, A.; Landsman, H.; Lang, R. F.; Lellouch, D.; Levinson, L.; Le Calloch, M.; Levy, C.; Lin, Q.; Lindemann, S.; Lindner, M.; Lopes, J. A. M.; Manfredini, A.; Marrodán Undagoitia, T.; Masbou, J.; Massoli, F. V.; Masson, D.; Mayani, D.; Meng, Y.; Messina, M.; Micheneau, K.; Miguez, B.; Molinario, A.; Murra, M.; Naganoma, J.; Ni, K.; Oberlack, U.; Orrigo, S. E. A.; Pakarha, P.; Pelssers, B.; Persiani, R.; Piastra, F.; Pienaar, J.; Piro, M. -C.; Plante, G.; Priel, N.; Rauch, L.; Reichard, S.; Reuter, C.; Rizzo, A.; Rosendahl, S.; Rupp, N.; Dos Santos, J. M. F.; Sartorelli, G.; Scheibelhut, M.; Schindler, S.; Schreiner, J.; Schumann, M.; Scotto Lavina, L.; Selvi, M.; Shagin, P.; Silva, M.; Simgen, H.; Sivers, M. V.; Stein, A.; Thers, D.; Tiseni, A.; Trinchero, G.; Tunnell, C. D.; Wall, R.; Wang, H.; Weber, M.; Wei, Y.; Weinheimer, C.; Wulf, J.; Zhang, Y.; Xenon Collaboration Bibcode: 2016PhRvD..94l2001A Altcode: 2016arXiv160906154X We report on WIMP search results of the XENON100 experiment, combining three runs summing up to 477 live days from January 2010 to January 2014. Data from the first two runs were already published. A blind analysis was applied to the last run recorded between April 2013 and January 2014 prior to combining the results. The ultralow electromagnetic background of the experiment, ∼5 ×10-3 events /(keVee×kg ×day ) ) before electronic recoil rejection, together with the increased exposure of 48 kg ×yr , improves the sensitivity. A profile likelihood analysis using an energy range of (6.6 - 43.3 ) keVnr sets a limit on the elastic, spin-independent WIMP-nucleon scattering cross section for WIMP masses above 8 GeV /c2 , with a minimum of 1.1 ×10-45 cm2 at 50 GeV /c2 and 90% confidence level. We also report updated constraints on the elastic, spin-dependent WIMP-nucleon cross sections obtained with the same data. We set upper limits on the WIMP-neutron (proton) cross section with a minimum of 2.0 ×10-40 cm2 (52 ×10-40 cm2 ) at a WIMP mass of 50 GeV /c2 , at 90% confidence level. Title: Probing the Physical Connection between Solar Prominences and Coronal Rain Authors: Liu, W.; Antolin, P.; Sun, X.; Vial, J. C.; Guo, L.; Gibson, S. E.; Berger, T. E.; Okamoto, J.; De Pontieu, B. Bibcode: 2016AGUFMSH43C2587L Altcode: Solar prominences and coronal rain are intimately related phenomena, both involving cool material at chromospheric temperatures within the hot corona and both playing important roles as part of the return flow of the chromosphere-corona mass cycle. At the same time, they exhibit distinct morphologies and dynamics not yet well understood. Quiescent prominences consist of numerous long-lasting, filamentary downflow threads, while coronal rain is more transient and falls comparably faster along well-defined curved paths. We report here a novel, hybrid prominence-coronal rain complex in an arcade-fan geometry observed by SDO/AIA and IRIS, which provides new insights to the underlying physics of such contrasting behaviors. We found that the supra-arcade fan region hosts a prominence sheet consisting of meandering threads with broad line widths. As the prominence material descends to the arcade, it turns into coronal rain sliding down coronal loops with line widths 2-3 times narrower. This contrast suggests that distinct local plasma and magnetic conditions determine the fate of the cool material, a scenario supported by our magnetic field extrapolations from SDO/HMI. Specifically, the supra-arcade fan (similar to those in solar flares) is likely situated in a current sheet, where the magnetic field is weak and the plasma-beta could be close to unity, thus favoring turbulent flows like those prominence threads. In contrast, the underlying arcade has a stronger magnetic field and most likely a low-beta environment, such that the material is guided along magnetic field lines to appear as coronal rain. We will discuss the physical implications of these observations beyond the phenomena of prominences and coronal rain. Title: LND for Chang'E 4 Mission Authors: Wimmer-Schweingruber, R. F.; Yu, J.; Hellweg, C.; Berger, T.; Zhang, S.; Burmeister, S.; Seimetz, L.; Schuster, B.; Boettcher, S. I.; Woyciechowski, H.; Guo, J.; Lohf, H.; Knierim, V. Bibcode: 2016AGUFMSM51A2465W Altcode: The Lunar Lander Neutrons & Dosimetry experiment (LND) is part of the payload of the next Chinese lunar mission, Chang'E 4, which is planned to land on the far side of the Moon. The University of Kiel in Germany is responsible for the design, development, and build of LND. This instrument will be accommodated on the Chang'E 4 Lander and has two major science objectives: dosimetry for human exploration of the Moon and contribution to heliospheric science. To achieve the first objective, LND is designed to determine the time series of dose rate and of linear energy transfer (LET) spectra in the complex radiation field of the lunar surface. For the second objective, LND is capable to measure the particle fluxes and their temporal variations, which can contribute to the understanding of particle propagation and transport in the heliosphere. With a stack of 10 silicon solid-state detectors, LND can measure fast neutrons in the energy rang from 2 - 20 MeV, protons from 10 - 30 MeV, electrons from 60 - 500 keV, alpha particles from 10 - 20 MeV/n and heavy ions from 15 - 40 MeV/n. Using two Gd-sandwich detectors, LND can in addition measure fluxes of thermal neutrons, which are sensitive to subsurface water and important to understand lunar surface mixing processes. Here we present the current development status of LND including the test results of the engineering model, together with plans for future activities. Title: Blending of Ground- and Space-Based Magnetograms: Application to L1-L5 Solar Wind and Coronal Hole Predictions Authors: Berger, T. E.; Pevtsov, A. A.; Martinez-Pillet, V.; Bertello, L.; Petrie, G. J. D.; Arge, C. N.; Henney, C. J.; Biesecker, D. A. Bibcode: 2016AGUFMSH11C2241B Altcode: We examine the effect of blending ground-based Global Oscillations Network Group (GONG) line-of-sight solar magnetic flux maps ("magnetograms") with space-based magnetograms from the Solar Dynamics Observatory (SDO) Helioseismic and Magnetic Imager (HMI) instrument on solar wind and coronal hole model-based forecasts. The longitudinally blended maps are used to "reforecast" solar wind conditions using the Wang-Sheeley-Arge (WSA) solar wind model during historical periods of coronal hole High Speed Streams (HSS) and Corotating Interaction Regions (CIRs) and compared to Advanced Composition Explorer (ACE) data at the L1 Lagrangian point. The same WSA runs are repeated using GONG and HMI data alone to determine the effect of data blending. The blended maps are also used to create Potential Field Source Surface (PFSS) maps of open coronal field lines and compared with historical coronal hole data from SDO Atmospheric Imaging Assembly (AIA) images. The study addresses the feasibility of combining ground- and space-based data from instruments with widely disparate and varying spatiotemporal resolution and flux sensitivity levels for use as inputs to solar wind and coronal hole forecasting models. The results are relevant to mission studies considering blended data inputs from, e.g., L5 Lagrangian point satellite instruments with ground-based measurements on the Sun-Earth line, as well as to expected magnetogram data from the Solar Orbiter Polarimetric and Helioseismic Imager (PHI) instrument. This study complements others that examine the utility of having multiple viewpoint (e.g. L1 and L5) magnetogram inputs to solar wind models by exploring data blending from disparate instruments. Title: DARWIN: towards the ultimate dark matter detector Authors: Aalbers, J.; Agostini, F.; Alfonsi, M.; Amaro, F. D.; Amsler, C.; Aprile, E.; Arazi, L.; Arneodo, F.; Barrow, P.; Baudis, L.; Benabderrahmane, M. L.; Berger, T.; Beskers, B.; Breskin, A.; Breur, P. A.; Brown, A.; Brown, E.; Bruenner, S.; Bruno, G.; Budnik, R.; Bütikofer, L.; Calvén, J.; Cardoso, J. M. R.; Cichon, D.; Coderre, D.; Colijn, A. P.; Conrad, J.; Cussonneau, J. P.; Decowski, M. P.; Diglio, S.; Drexlin, G.; Duchovni, E.; Erdal, E.; Eurin, G.; Ferella, A.; Fieguth, A.; Fulgione, W.; Gallo Rosso, A.; Di Gangi, P.; Di Giovanni, A.; Galloway, M.; Garbini, M.; Geis, C.; Glueck, F.; Grandi, L.; Greene, Z.; Grignon, C.; Hasterok, C.; Hannen, V.; Hogenbirk, E.; Howlett, J.; Hilk, D.; Hils, C.; James, A.; Kaminsky, B.; Kazama, S.; Kilminster, B.; Kish, A.; Krauss, L. M.; Landsman, H.; Lang, R. F.; Lin, Q.; Linde, F. L.; Lindemann, S.; Lindner, M.; Lopes, J. A. M.; Marrodán Undagoitia, T.; Masbou, J.; Massoli, F. V.; Mayani, D.; Messina, M.; Micheneau, K.; Molinario, A.; Morå, K. D.; Morteau, E.; Murra, M.; Naganoma, J.; Newstead, J. L.; Ni, K.; Oberlack, U.; Pakarha, P.; Pelssers, B.; de Perio, P.; Persiani, R.; Piastra, F.; Piro, M. C.; Plante, G.; Rauch, L.; Reichard, S.; Rizzo, A.; Rupp, N.; Dos Santos, J. M. F.; Sartorelli, G.; Scheibelhut, M.; Schindler, S.; Schumann, M.; Schreiner, J.; Scotto Lavina, L.; Selvi, M.; Shagin, P.; Silva, M. C.; Simgen, H.; Sissol, P.; von Sivers, M.; Thers, D.; Thurn, J.; Tiseni, A.; Trotta, R.; Tunnell, C. D.; Valerius, K.; Vargas, M. A.; Wang, H.; Wei, Y.; Weinheimer, C.; Wester, T.; Wulf, J.; Zhang, Y.; Zhu, T.; Zuber, K. Bibcode: 2016JCAP...11..017A Altcode: 2016arXiv160607001A DARk matter WImp search with liquid xenoN (DARWIN) will be an experiment for the direct detection of dark matter using a multi-ton liquid xenon time projection chamber at its core. Its primary goal will be to explore the experimentally accessible parameter space for Weakly Interacting Massive Particles (WIMPs) in a wide mass-range, until neutrino interactions with the target become an irreducible background. The prompt scintillation light and the charge signals induced by particle interactions in the xenon will be observed by VUV sensitive, ultra-low background photosensors. Besides its excellent sensitivity to WIMPs above a mass of 5 GeV/c2, such a detector with its large mass, low-energy threshold and ultra-low background level will also be sensitive to other rare interactions. It will search for solar axions, galactic axion-like particles and the neutrinoless double-beta decay of 136Xe, as well as measure the low-energy solar neutrino flux with < 1% precision, observe coherent neutrino-nucleus interactions, and detect galactic supernovae. We present the concept of the DARWIN detector and discuss its physics reach, the main sources of backgrounds and the ongoing detector design and R&D efforts. Title: Low-mass dark matter search using ionization signals in XENON100 Authors: Aprile, E.; Aalbers, J.; Agostini, F.; Alfonsi, M.; Amaro, F. D.; Anthony, M.; Arneodo, F.; Barrow, P.; Baudis, L.; Bauermeister, B.; Benabderrahmane, M. L.; Berger, T.; Breur, P. A.; Brown, A.; Brown, E.; Bruenner, S.; Bruno, G.; Budnik, R.; Buss, A.; Bütikofer, L.; Cardoso, J. M. R.; Cervantes, M.; Cichon, D.; Coderre, D.; Colijn, A. P.; Conrad, J.; Cussonneau, J. P.; Decowski, M. P.; de Perio, P.; di Gangi, P.; di Giovanni, A.; Duchovni, E.; Ferella, A. D.; Fieguth, A.; Franco, D.; Fulgione, W.; Galloway, M.; Garbini, M.; Geis, C.; Goetzke, L. W.; Greene, Z.; Grignon, C.; Gross, E.; Hasterok, C.; Hogenbirk, E.; Itay, R.; Kaminsky, B.; Kessler, G.; Kish, A.; Landsman, H.; Lang, R. F.; Levinson, L.; Le Calloch, M.; Levy, C.; Linde, F.; Lindemann, S.; Lindner, M.; Lopes, J. A. M.; Lyashenko, A.; Manfredini, A.; Marrodán Undagoitia, T.; Masbou, J.; Massoli, F. V.; Masson, D.; Mayani, D.; Melgarejo Fernandez, A. J.; Meng, Y.; Messina, M.; Micheneau, K.; Miguez, B.; Molinario, A.; Murra, M.; Naganoma, J.; Oberlack, U.; Orrigo, S. E. A.; Pakarha, P.; Pelssers, B.; Persiani, R.; Piastra, F.; Pienaar, J.; Plante, G.; Priel, N.; Rauch, L.; Reichard, S.; Reuter, C.; Rizzo, A.; Rosendahl, S.; Rupp, N.; Dos Santos, J. M. F.; Sartorelli, G.; Scheibelhut, M.; Schindler, S.; Schreiner, J.; Schumann, M.; Scotto Lavina, L.; Selvi, M.; Shagin, P.; Simgen, H.; Stein, A.; Thers, D.; Tiseni, A.; Trinchero, G.; Tunnell, C. D.; von Sivers, M.; Wall, R.; Wang, H.; Weber, M.; Wei, Y.; Weinheimer, C.; Wulf, J.; Zhang, Y.; Xenon Collaboration Bibcode: 2016PhRvD..94i2001A Altcode: 2016arXiv160506262X We perform a low-mass dark matter search using an exposure of 30 kg ×yr with the XENON100 detector. By dropping the requirement of a scintillation signal and using only the ionization signal to determine the interaction energy, we lowered the energy threshold for detection to 0.7 keV for nuclear recoils. No dark matter detection can be claimed because a complete background model cannot be constructed without a primary scintillation signal. Instead, we compute an upper limit on the WIMP-nucleon scattering cross section under the assumption that every event passing our selection criteria could be a signal event. Using an energy interval from 0.7 keV to 9.1 keV, we derive a limit on the spin-independent WIMP-nucleon cross section that excludes WIMPs with a mass of 6 GeV /c2 above 1.4 ×10-41 cm2 at 90% confidence level. Title: DOSIS & DOSIS 3D: long-term dose monitoring onboard the Columbus Laboratory of the International Space Station (ISS) Authors: Berger, Thomas; Przybyla, Bartos; Matthiä, Daniel; Reitz, Günther; Burmeister, Sönke; Labrenz, Johannes; Bilski, Pawel; Horwacik, Tomasz; Twardak, Anna; Hajek, Michael; Fugger, Manfred; Hofstätter, Christina; Sihver, Lembit; Palfalvi, Jozsef K.; Szabo, Julianna; Stradi, Andrea; Ambrozova, Iva; Kubancak, Jan; Brabcova, Katerina Pachnerova; Vanhavere, Filip; Cauwels, Vanessa; Van Hoey, Olivier; Schoonjans, Werner; Parisi, Alessio; Gaza, Ramona; Semones, Edward; Yukihara, Eduardo G.; Benton, Eric R.; Doull, Brandon A.; Uchihori, Yukio; Kodaira, Satoshi; Kitamura, Hisashi; Boehme, Matthias Bibcode: 2016JSWSC...6A..39B Altcode: The radiation environment encountered in space differs in nature from that on Earth, consisting mostly of highly energetic ions from protons up to iron, resulting in radiation levels far exceeding the ones present on Earth for occupational radiation workers. Since the beginning of the space era, the radiation exposure during space missions has been monitored with various active and passive radiation instruments. Also onboard the International Space Station (ISS), a number of area monitoring devices provide data related to the spatial and temporal variation of the radiation field in and outside the ISS. The aim of the DOSIS (2009-2011) and the DOSIS 3D (2012-ongoing) experiments was and is to measure the radiation environment within the European Columbus Laboratory of the ISS. These measurements are, on the one hand, performed with passive radiation detectors mounted at 11 locations within Columbus for the determination of the spatial distribution of the radiation field parameters and, on the other, with two active radiation detectors mounted at a fixed position inside Columbus for the determination of the temporal variation of the radiation field parameters. Data measured with passive radiation detectors showed that the absorbed dose values inside the Columbus Laboratory follow a pattern, based on the local shielding configuration of the radiation detectors, with minimum dose values observed in the year 2010 of 195-270 μGy/day and maximum values observed in the year 2012 with values ranging from 260 to 360 μGy/day. The absorbed dose is modulated by (a) the variation in solar activity and (b) the changes in ISS altitude. Title: The RIMFAX GPR Instrument Development for the Mars 2020 Rover Mission Authors: Hamran, S. -E.; Amundsen, H. E. F.; Asak, L.; Berger, T.; Brovoll, S.; Buskenes, J. I.; Carter, L.; Damsgård, L.; Diaz, C.; Ghent, R.; Helleren, Ø.; Kohler, J.; Mellon, M.; Nunez, D.; Paige, D.; Plettemeier, D.; Rowe, K.; Russell, P.; Sagsveen, B.; Ødegaard, N.; Øyan, M. J. Bibcode: 2016LPICo1980.4031H Altcode: The Radar Imager for Mars' subsurface eXperiment (RIMFAX) ground penetrating radar (GPR) experiment for the Mars 2020 Rover will add a new dimension to the rover's toolset by providing the capability to image the shallow subsurface beneath the rover. Title: Joint SDO and IRIS Observations of a Novel, Hybrid Prominence-Coronal Rain Complex Authors: Liu, Wei; Antolin, Patrick; Sun, Xudong; Gao, Lijia; Vial, Jean-Claude; Gibson, Sarah; Okamoto, Takenori; Berger, Thomas; Uitenbroek, Han; De Pontieu, Bart Bibcode: 2016usc..confE..99L Altcode: Solar prominences and coronal rain are intimately related phenomena, both involving cool material at chromospheric temperatures within the hot corona and both playing important roles as part of the return flow of the chromosphere-corona mass cycle. At the same time, they exhibit distinct morphologies and dynamics not yet well understood. Quiescent prominences consist of numerous long-lasting, filamentary downflow threads, while coronal rain is more transient and falls comparably faster along well-defined curved paths. We report here a novel, hybrid prominence-coronal rain complex in an arcade-fan geometry observed by SDO/AIA and IRIS, which provides new insights to the underlying physics of such contrasting behaviors. We found that the supra-arcade fan region hosts a prominence sheet consisting of meandering threads with broad line widths. As the prominence material descends to the arcade, it turns into coronal rain sliding down coronal loops with line widths 2-3 times narrower. This contrast suggests that distinct local plasma and magnetic conditions determine the fate of the cool material, a scenario supported by our magnetic field extrapolations from SDO/HMI. Specifically, the supra-arcade fan (similar to those in solar flares; e.g., McKenzie 2013) is likely situated in a current sheet, where the magnetic field is weak and the plasma-beta could be close to unity, thus favoring turbulent flows like those prominence threads. In contrast, the underlying arcade has a stronger magnetic field and most likely a low-beta environment, such that the material is guided along magnetic field lines to appear as coronal rain. We will discuss the physical implications of these observations beyond prominence and coronal rain. Title: Transitioning GONG data processing to NOAA SWPC operations Authors: Reinard, Alysha; Berger, Thomas; Marble, Andrew; Hill, Frank Bibcode: 2016shin.confE..26R Altcode: The NOAA Space Weather Prediction Center (SWPC) is the nation's official source of space weather watches, warnings, and alerts, providing 24x7 forecasting and support to critical infrastructure operators around the world. Observations of the conditions on the Sun are crucial for determining when and if a warning is needed. The Global Oscillation Network Group (GONG) operated by the National Solar Observatory (NSO) consists of six ground stations, allowing continuous observations of the Sun. Of particular interest for space weather purposes are the H-alpha images and magnetograms. H-alpha data is used to identify filaments and their eruptions, to assess active region evolution and plage extent, and to help localize flare locations. Magnetograms are used to identify neutral lines, examine potential shearing areas and characterize the magnetic structure of active regions. GONG magnetograms also provide the initial condition for models of solar wind expansion such as the WSA-Enlil model. GONG helioseismology products, in particular far-side imaging, are being examined for operational use in the near future. NSO has operated GONG as a science facility since 1995 and has provided processed space weather data products to NOAA via public internet connections for the past several years. In 2014 the White House Office of Management and Budget (OMB) requested that NOAA transition the GONG network to an operational space weather asset in order to ensure the continued flow of critical magnetogram data for solar wind models. NSO will continue to operate and manage the instruments and sites, but the H-alpha images and 10 minute averaged magnetogram data will be sent directly to SWPC for processing and use in space weather modeling. SWPC will make these data available to NSO and the public via the new NOAA Integrated Dissemination Program (IDP) network. We discuss the progress and details of this change. Title: Towards Space Exploration of Moon, Mars Neos: Radiation Biological Basis Authors: Hellweg, Christine; Baumstark-Khan, Christa; Berger, Thomas; Reitz, Guenther Bibcode: 2016cosp...41E.825H Altcode: Radiation has emerged as the most critical issue to be resolved for long-term missions both orbital and interplanetary. Astronauts are constantly exposed to galactic cosmic radiation (GCR) of various energies with a low dose rate. Primarily late tissue sequels like genetic alterations, cancer and non-cancer effects, i.e. cataracts and degenerative diseases of e.g. the central nervous system or the cardiovascular system, are the potential risks. Cataracts were observed to occur earlier and more often in astronauts exposed to higher proportions of galactic ions (Cucinotta et al., 2001). Predictions of cancer risk and acceptable radiation exposure in space are subject to many uncertainties including the relative biological effectiveness (RBE) of space radiation especially heavy ions, dose-rate effects and possible interaction with microgravity and other spaceflight environmental factors. The initial cellular response to radiation exposure paves the way to late sequelae and starts with damage to the DNA which complexity depends on the linear energy transfer (LET) of the radiation. Repair of such complex DNA damage is more challenging and requires more time than the repair of simple DNA double strand breaks (DSB) which can be visualized by immunofluorescence staining of the phosphorylated histone 2AX (γH2AX) and might explain the observed prolonged cell cycle arrests induced by high-LET in comparison to low-LET irradiation. Unrepaired or mis-repaired DNA DSB are proposed to be responsible for cell death, mutations, chromosomal aberrations and oncogenic cell transformation. Cell killing and mutation induction are most efficient in an LET range of 90-200 keV/µm. Also the activation of transcription factors such as Nuclear Factor κB (NF-κB) and gene expression shaping the cellular radiation response depend on the LET with a peak RBE between 90 and 300 keV/µm. Such LET-RBE relationships were observed for cataract and cancer induction by heavy ions in laboratory animals, with varying maximal efficiencies. Furthermore, there is always the added risk of acute exposure to high proton fluxes during a solar particle event (SPE), which can threaten immediate survival of the astronauts in case of insufficient shielding by eliciting the acute radiation syndrome. Its symptoms depend on absorbed total radiation dose, type of radiation, the dose distribution in the body and the individual radiation sensitivity. After the prodromal stage with nausea and vomiting and a subsequent symptom-free phase, depending on dose, the hematopoietic syndrome with suppression of the acquired immune system and thrombocytopenia (0.7-4 Sv), the gastrointestinal tract syndrome (5-12 Sv) or the central nervous system syndrome (> 20 Sv) develop and they are accompanied by exacerbated innate immune responses. Exposure to large SPE has to be avoided by warning systems and stay inside a radiation shelter during the event. Treatment options encompass e.g. the administration of colony-stimulating factors (CSF), growth factors and blood transfusions to overcome the hematopoietic syndrome and the administration of antibiotics against secondary infections. A concerted action of ground-based studies and space experiments is required to improve the radiobiological basis of space radiation risk assessment and countermeasure development. References: Cucinotta FA, Manuel FK, Jones J, Iszard G, Murrey J, Djojonegro B and Wear M (2001) Space Radiation and Cataracts in Astronauts. Rad Res 156, 460-466 Title: Operational Space Weather Activities in the US Authors: Berger, Thomas; Singer, Howard; Onsager, Terrance; Viereck, Rodney; Murtagh, William; Rutledge, Robert Bibcode: 2016cosp...41E.180B Altcode: We review the current activities in the civil operational space weather forecasting enterprise of the United States. The NOAA/Space Weather Prediction Center is the nation's official source of space weather watches, warnings, and alerts, working with partners in the Air Force as well as international operational forecast services to provide predictions, data, and products on a large variety of space weather phenomena and impacts. In October 2015, the White House Office of Science and Technology Policy released the National Space Weather Strategy (NSWS) and associated Space Weather Action Plan (SWAP) that define how the nation will better forecast, mitigate, and respond to an extreme space weather event. The SWAP defines actions involving multiple federal agencies and mandates coordination and collaboration with academia, the private sector, and international bodies to, among other things, develop and sustain an operational space weather observing system; develop and deploy new models of space weather impacts to critical infrastructure systems; define new mechanisms for the transition of research models to operations and to ensure that the research community is supported for, and has access to, operational model upgrade paths; and to enhance fundamental understanding of space weather through support of research models and observations. The SWAP will guide significant aspects of space weather operational and research activities for the next decade, with opportunities to revisit the strategy in the coming years through the auspices of the National Science and Technology Council. Title: Data and Models Needed to Support Civil Aviation Authors: Onsager, Terrance; Biesecker, D. A.; Berger, Thomas; Rutledge, Robert Bibcode: 2016cosp...41E1469O Altcode: The effective utilization of existing data and models is an important element in advancing the goals of the COSPAR/ILWS space weather roadmap. This is recommended to be done through innovative approaches to data utilization, including data driving, data assimilation, and ensemble modeling. This presentation will focus on observations and models needed to support space weather services for civil aviation and commercial space transportation. The service needs for aviation will be discussed, and an overview will be given of some of the existing data and models that can provide these services. Efforts underway to define the requirements for real-time data and to assess current modeling capabilities will be described. Recommendations will be offered for internationally coordinated activities that could identify priorities and further the roadmap goals. Title: Experience Transitioning Models and Data at the NOAA Space Weather Prediction Center Authors: Berger, Thomas Bibcode: 2016cosp...41E.181B Altcode: The NOAA Space Weather Prediction Center has a long history of transitioning research data and models into operations and with the validation activities required. The first stage in this process involves demonstrating that the capability has sufficient value to customers to justify the cost needed to transition it and to run it continuously and reliably in operations. Once the overall value is demonstrated, a substantial effort is then required to develop the operational software from the research codes. The next stage is to implement and test the software and product generation on the operational computers. Finally, effort must be devoted to establishing long-term measures of performance, maintaining the software, and working with forecasters, customers, and researchers to improve over time the operational capabilities. This multi-stage process of identifying, transitioning, and improving operational space weather capabilities will be discussed using recent examples. Plans for future activities will also be described. Title: Transitioning GONG data processing to NOAA SWPC operations Authors: Reinard, Alysha; Marble, Andrew R.; Berger, Thomas Bibcode: 2016SPD....47.0205R Altcode: The NOAA Space Weather Prediction Center (SWPC) is the nation's official source of space weather watches, warnings, and alerts, providing 24x7 forecasting and support to critical infrastructure operators around the world. Observations of the conditions on the Sun are crucial for determining when and if a warning is needed. The Global Oscillation Network Group (GONG) operated by the National Solar Observatory (NSO) consists of six ground stations, allowing continuous observations of the Sun. Of particular interest for space weather purposes are the H-alpha images and magnetograms. The H-alpha data are used to identify filaments and their eruptions, to assess active region evolution and plage extent, and to help localize flare locations. The magnetograms are used to identify neutral lines, to examine potential shearing areas and to characterize the magnetic structure of active regions. GONG magnetograms also provide the initial condition for models of solar wind expansion through the heliosphere such as the WSA-Enlil model. Although beyond the scope of current space weather applications, GONG helioseismology products can be used to assess active region emergence on the far side of the Sun and to indicate the flaring potential of a front-side active region. These products are being examined as future tools in flare prediction.NSO has operated GONG as a science facility since 1995 and has provided processed space weather data products to NOAA via for the past several years. In 2014 the White House Office of Management and Budget (OMB) requested that NOAA transition the GONG network to an operational space weather asset in order to ensure the continued flow of critical data for solar wind models. NSO will continue to operate and manage the instruments and sites, but the H-alpha images and 10 minute averaged magnetogram data will be sent directly to SWPC for processing and use in space weather modeling. SWPC will make these data available to NSO and the public via the new NOAA Integrated Dissemination Program (IDP) network. We discuss the progress and details of this change. Title: Physics reach of the XENON1T dark matter experiment. Authors: Aprile, E.; Aalbers, J.; Agostini, F.; Alfonsi, M.; Amaro, F. D.; Anthony, M.; Arazi, L.; Arneodo, F.; Balan, C.; Barrow, P.; Baudis, L.; Bauermeister, B.; Berger, T.; Breur, P.; Breskin, A.; Brown, A.; Brown, E.; Bruenner, S.; Bruno, G.; Budnik, R.; Bütikofer, L.; Cardoso, J. M. R.; Cervantes, M.; Cichon, D.; Coderre, D.; Colijn, A. P.; Conrad, J.; Contreras, H.; Cussonneau, J. P.; Decowski, M. P.; de Perio, P.; Di Gangi, P.; Di Giovanni, A.; Duchovni, E.; Fattori, S.; Ferella, A. D.; Fieguth, A.; Franco, D.; Fulgione, W.; Galloway, M.; Garbini, M.; Geis, C.; Goetzke, L. W.; Greene, Z.; Grignon, C.; Gross, E.; Hampel, W.; Hasterok, C.; Itay, R.; Kaether, F.; Kaminsky, B.; Kessler, G.; Kish, A.; Landsman, H.; Lang, R. F.; Lellouch, D.; Levinson, L.; Le Calloch, M.; Levy, C.; Lindemann, S.; Lindner, M.; Lopes, J. A. M.; Lyashenko, A.; Macmullin, S.; Manfredini, A.; Marrodán Undagoitia, T.; Masbou, J.; Massoli, F. V.; Mayani, D.; Melgarejo Fernandez, A. J.; Meng, Y.; Messina, M.; Micheneau, K.; Miguez, B.; Molinario, A.; Murra, M.; Naganoma, J.; Oberlack, U.; Orrigo, S. E. A.; Pakarha, P.; Pelssers, B.; Persiani, R.; Piastra, F.; Pienaar, J.; Plante, G.; Priel, N.; Rauch, L.; Reichard, S.; Reuter, C.; Rizzo, A.; Rosendahl, S.; Rupp, N.; dos Santos, J. M. F.; Sartorelli, G.; Scheibelhut, M.; Schindler, S.; Schreiner, J.; Schumann, M.; Scotto Lavina, L.; Selvi, M.; Shagin, P.; Simgen, H.; Stein, A.; Thers, D.; Tiseni, A.; Trinchero, G.; Tunnell, C.; von Sivers, M.; Wall, R.; Wang, H.; Weber, M.; Wei, Y.; Weinheimer, C.; Wulf, J.; Zhang, Y. Bibcode: 2016JCAP...04..027A Altcode: 2015arXiv151207501T The XENON1T experiment is currently in the commissioning phase at the Laboratori Nazionali del Gran Sasso, Italy. In this article we study the experiment's expected sensitivity to the spin-independent WIMP-nucleon interaction cross section, based on Monte Carlo predictions of the electronic and nuclear recoil backgrounds. The total electronic recoil background in 1 tonne fiducial volume and (1, 12) keV electronic recoil equivalent energy region, before applying any selection to discriminate between electronic and nuclear recoils, is (1.80 ± 0.15) · 10-4 (kg·day·keV)-1, mainly due to the decay of 222Rn daughters inside the xenon target. The nuclear recoil background in the corresponding nuclear recoil equivalent energy region (4, 50) keV, is composed of (0.6 ± 0.1) (t·y)-1 from radiogenic neutrons, (1.8 ± 0.3) · 10-2 (t·y)-1 from coherent scattering of neutrinos, and less than 0.01 (t·y)-1 from muon-induced neutrons. The sensitivity of XENON1T is calculated with the Profile Likelihood Ratio method, after converting the deposited energy of electronic and nuclear recoils into the scintillation and ionization signals seen in the detector. We take into account the systematic uncertainties on the photon and electron emission model, and on the estimation of the backgrounds, treated as nuisance parameters. The main contribution comes from the relative scintillation efficiency Script Leff, which affects both the signal from WIMPs and the nuclear recoil backgrounds. After a 2 y measurement in 1 t fiducial volume, the sensitivity reaches a minimum cross section of 1.6 · 10-47 cm2 at mχ = 50 GeV/c2. Title: The Martian surface radiation environment - a comparison of models and MSL/RAD measurements Authors: Matthiä, Daniel; Ehresmann, Bent; Lohf, Henning; Köhler, Jan; Zeitlin, Cary; Appel, Jan; Sato, Tatsuhiko; Slaba, Tony; Martin, Cesar; Berger, Thomas; Boehm, Eckart; Boettcher, Stephan; Brinza, David E.; Burmeister, Soenke; Guo, Jingnan; Hassler, Donald M.; Posner, Arik; Rafkin, Scot C. R.; Reitz, Günther; Wilson, John W.; Wimmer-Schweingruber, Robert F. Bibcode: 2016JSWSC...6A..13M Altcode: Context: The Radiation Assessment Detector (RAD) on the Mars Science Laboratory (MSL) has been measuring the radiation environment on the surface of Mars since August 6th 2012. MSL-RAD is the first instrument to provide detailed information about charged and neutral particle spectra and dose rates on the Martian surface, and one of the primary objectives of the RAD investigation is to help improve and validate current radiation transport models. Aims: Applying different numerical transport models with boundary conditions derived from the MSL-RAD environment the goal of this work was to both provide predictions for the particle spectra and the radiation exposure on the Martian surface complementing the RAD sensitive range and, at the same time, validate the results with the experimental data, where applicable. Such validated models can be used to predict dose rates for future manned missions as well as for performing shield optimization studies. Methods: Several particle transport models (GEANT4, PHITS, HZETRN/OLTARIS) were used to predict the particle flux and the corresponding radiation environment caused by galactic cosmic radiation on Mars. From the calculated particle spectra the dose rates on the surface are estimated. Results: Calculations of particle spectra and dose rates induced by galactic cosmic radiation on the Martian surface are presented. Although good agreement is found in many cases for the different transport codes, GEANT4, PHITS, and HZETRN/OLTARIS, some models still show large, sometimes order of magnitude discrepancies in certain particle spectra. We have found that RAD data is helping to make better choices of input parameters and physical models. Elements of these validated models can be applied to more detailed studies on how the radiation environment is influenced by solar modulation, Martian atmosphere and soil, and changes due to the Martian seasonal pressure cycle. By extending the range of the calculated particle spectra with respect to the experimental data additional information about the radiation environment is gained, and the contribution of different particle species to the dose is estimated. Title: Matroshka DOSTEL measurements onboard the International Space Station (ISS) Authors: Labrenz, Johannes; Burmeister, Soenke; Berger, Thomas; Heber, Bernd; Reitz, Guenther Bibcode: 2015JSWSC...5A..38L Altcode: This paper presents the absorbed dose and dose equivalent rate measurements achieved with the DOSimetry TElescope (DOSTEL) during the two Matroshka (MTR) experiment campaigns in 2004/2005 (MTR-1) and 2007/2008 (MTR-2B). The comparison between the inside (MTR-2B) and outside (MTR-1) mission has shown that the shielding thickness provided by the International Space Station (ISS) spacecraft hull has a minor effect on the radiation exposure caused by Galactic Cosmic Rays (GCR). The exposure varies with the solar modulation of the GCR, too. Particles from Earth's radiation belts are effectively shielded by the spacecraft hull, and thus the contribution to the radiation exposure is lower for the inside measurement during MTR-2B. While the MTR-DOSTEL absorbed dose rate shows a good agreement with passive detectors of the MTR experiment for the MTR-2B mission phase, the MTR-1 absorbed dose rates from MTR-DOSTEL measurements are much lower than those obtained by a nearby passive detector. Observed discrepancies between the MTR-DOSTEL measurements and the passive detectors located nearby could be explained by the additional exposure to an enhanced flux of electrons trapped between L-parameter 2.5 and 3.5 caused by solar storms in July 2004. Title: Transitioning GONG data processing to NOAA SWPC operations Authors: Reinard, A.; Marble, A.; Hill, F.; Berger, T. E. Bibcode: 2015AGUFMSH21B2394R Altcode: The NOAA Space Weather Prediction Center (SWPC) is the nation's official source of space weather watches, warnings, and alerts, providing 24x7 forecasting and support to critical infrastructure operators around the world. Observations of the conditions on the Sun are crucial for determining when and if a warning is needed. The Global Oscillation Network Group (GONG) operated by the National Solar Observatory (NSO) consists of six ground stations, allowing continuous observations of the Sun. Of particular interest for space weather purposes are the H-alpha images and magnetograms. The H-alpha data are used to identify filaments and their eruptions, to assess active region evolution and plage extent, and to help localize flare locations. The magnetograms are used to identify neutral lines, to examine potential shearing areas and to characterize the magnetic structure of active regions. GONG magnetograms also provide the initial condition for models of solar wind expansion through the heliosphere such as the WSA-Enlil model. Although beyond the scope of current space weather applications, GONG helioseismology products can be used to assess active region emergence on the far side of the Sun and to indicate the flaring potential of a front-side active region. These products are being examined as future tools in flare prediction. NSO has operated GONG as a science facility since 1995 and has provided processed space weather data products to NOAA via public internet connections for the past several years. In 2014 the White House Office of Management and Budget (OMB) requested that NOAA transition the GONG network to an operational space weather asset in order to ensure the continued flow of critical magnetogram data for solar wind models. NSO will continue to operate and manage the instruments and sites, but the H-alpha images and 10 minute averaged magnetogram data will be sent directly to SWPC for processing and use in space weather modeling. SWPC will make these data available to NSO and the public via the new NOAA Integrated Dissemination Program (IDP) network. We discuss the progress and details of this change. Title: Fifty Years of Space Weather Forecasting from Boulder Authors: Berger, T. E. Bibcode: 2015AGUFMSM13F..01B Altcode: The first official space weather forecast was issued by the Space Disturbances Laboratory in Boulder, Colorado, in 1965, ushering in an era of operational prediction that continues to this day. Today, the National Oceanic and Atmospheric Administration (NOAA) charters the Space Weather Prediction Center (SWPC) as one of the nine National Centers for Environmental Prediction (NCEP) to provide the nation's official watches, warnings, and alerts of space weather phenomena. SWPC is now integral to national and international efforts to predict space weather events, from the common and mild, to the rare and extreme, that can impact critical technological infrastructure. In 2012, the Strategic National Risk Assessment included extreme space weather events as low-to-medium probability phenomena that could, unlike any other meteorogical phenomena, have an impact on the government's ability to function. Recognizing this, the White House chartered the Office of Science and Technology Policy (OSTP) to produce the first comprehensive national strategy for the prediction, mitigation, and response to an extreme space weather event. The implementation of the National Strategy is ongoing with NOAA, its partners, and stakeholders concentrating on the goal of improving our ability to observe, model, and predict the onset and severity of space weather events. In addition, work continues with the research community to improve our understanding of the physical mechanisms - on the Sun, in the heliosphere, and in the Earth's magnetic field and upper atmosphere - of space weather as well as the effects on critical infrastructure such as electrical power transmission systems. In fifty years, people will hopefully look back at the history of operational space weather prediction and credit our efforts today with solidifying the necessary developments in observational systems, full-physics models of the entire Sun-Earth system, and tools for predicting the impacts to infrastructure to protect against any and all forms of space weather. Title: The Future of Operational Space Weather Observations Authors: Berger, T. E. Bibcode: 2015AGUFMSH12A..03B Altcode: We review the current state of operational space weather observations, the requirements for new or evolved space weather forecasting capablities, and the relevant sections of the new National strategy for space weather developed by the Space Weather Operations, Research, and Mitigation (SWORM) Task Force chartered by the Office of Science and Technology Policy of the White House. Based on this foundation, we discuss future space missions such as the NOAA space weather mission to the L1 Lagrangian point planned for the 2021 time frame and its synergy with an L5 mission planned for the same period; the space weather capabilities of the upcoming GOES-R mission, as well as GOES-Next possiblities; and the upcoming COSMIC-2 mission for ionospheric observations. We also discuss the needs for ground-based operational networks to supply mission critical and/or backup space weather observations including the NSF GONG solar optical observing network, the USAF SEON solar radio observing network, the USGS real-time magnetometer network, the USCG CORS network of GPS receivers, and the possibility of operationalizing the world-wide network of neutron monitors for real-time alerts of ground-level radiation events. Title: Space experiment "Cellular Responses to Radiation in Space (CELLRAD)": Hardware and biological system tests Authors: Hellweg, Christine E.; Dilruba, Shahana; Adrian, Astrid; Feles, Sebastian; Schmitz, Claudia; Berger, Thomas; Przybyla, Bartos; Briganti, Luca; Franz, Markus; Segerer, Jürgen; Spitta, Luis F.; Henschenmacher, Bernd; Konda, Bikash; Diegeler, Sebastian; Baumstark-Khan, Christa; Panitz, Corinna; Reitz, Günther Bibcode: 2015LSSR....7...73H Altcode: One factor contributing to the high uncertainty in radiation risk assessment for long-term space missions is the insufficient knowledge about possible interactions of radiation with other spaceflight environmental factors. Such factors, e.g. microgravity, have to be considered as possibly additive or even synergistic factors in cancerogenesis. Regarding the effects of microgravity on signal transduction, it cannot be excluded that microgravity alters the cellular response to cosmic radiation, which comprises a complex network of signaling pathways. The purpose of the experiment ;Cellular Responses to Radiation in Space; (CELLRAD, formerly CERASP) is to study the effects of combined exposure to microgravity, radiation and general space flight conditions on mammalian cells, in particular Human Embryonic Kidney (HEK) cells that are stably transfected with different plasmids allowing monitoring of proliferation and the Nuclear Factor κB (NF-κB) pathway by means of fluorescent proteins. The cells will be seeded on ground in multiwell plate units (MPUs), transported to the ISS, and irradiated by an artificial radiation source after an adaptation period at 0 × g and 1 × g. After different incubation periods, the cells will be fixed by pumping a formaldehyde solution into the MPUs. Ground control samples will be treated in the same way. For implementation of CELLRAD in the Biolab on the International Space Station (ISS), tests of the hardware and the biological systems were performed. The sequence of different steps in MPU fabrication (cutting, drilling, cleaning, growth surface coating, and sterilization) was optimized in order to reach full biocompatibility. Different coatings of the foil used as growth surface revealed that coating with 0.1 mg/ml poly-D-lysine supports cell attachment better than collagen type I. The tests of prototype hardware (Science Model) proved its full functionality for automated medium change, irradiation and fixation of cells. Exposure of HEK cells to the β-rays emitted by the radiation source dose-dependently decreased cell growth and increased NF-κB activation. The signal of the fluorescent proteins after formaldehyde fixation was stable for at least six months after fixation, allowing storage of the MPUs after fixation for several months before the transport back to Earth and evaluation of the fluorescence intensity. In conclusion, these tests show the feasibility of CELLRAD on the ISS with the currently available transport mechanisms. Title: First High-resolution Spectroscopic Observations of an Erupting Prominence Within a Coronal Mass Ejection by the Interface Region Imaging Spectrograph (IRIS) Authors: Liu, Wei; De Pontieu, Bart; Vial, Jean-Claude; Title, Alan M.; Carlsson, Mats; Uitenbroek, Han; Okamoto, Takenori J.; Berger, Thomas E.; Antolin, Patrick Bibcode: 2015ApJ...803...85L Altcode: 2015arXiv150204738L Spectroscopic observations of prominence eruptions associated with coronal mass ejections (CMEs), although relatively rare, can provide valuable plasma and three-dimensional geometry diagnostics. We report the first observations by the Interface Region Imaging Spectrograph mission of a spectacular fast CME/prominence eruption associated with an equivalent X1.6 flare on 2014 May 9. The maximum plane-of-sky and Doppler velocities of the eruption are 1200 and 460 km s-1, respectively. There are two eruption components separated by ∼200 km s-1 in Doppler velocity: a primary, bright component and a secondary, faint component, suggesting a hollow, rather than solid, cone-shaped distribution of material. The eruption involves a left-handed helical structure undergoing counterclockwise (viewed top-down) unwinding motion. There is a temporal evolution from upward eruption to downward fallback with less-than-free-fall speeds and decreasing nonthermal line widths. We find a wide range of Mg ii k/h line intensity ratios (less than ∼2 expected for optically-thin thermal emission): the lowest ever reported median value of 1.17 found in the fallback material, a comparably high value of 1.63 in nearby coronal rain, and intermediate values of 1.53 and 1.41 in the two eruption components. The fallback material exhibits a strong (\gt 5σ ) linear correlation between the k/h ratio and the Doppler velocity as well as the line intensity. We demonstrate that Doppler dimming of scattered chromospheric emission by the erupted material can potentially explain such characteristics. Title: Characteristics of Operational Space Weather Forecasting: Observations and Models Authors: Berger, Thomas; Viereck, Rodney; Singer, Howard; Onsager, Terry; Biesecker, Doug; Rutledge, Robert; Hill, Steven; Akmaev, Rashid; Milward, George; Fuller-Rowell, Tim Bibcode: 2015TESS....111204B Altcode: In contrast to research observations, models and ground support systems, operational systems are characterized by real-time data streams and run schedules, with redundant backup systems for most elements of the system. We review the characteristics of operational space weather forecasting, concentrating on the key aspects of ground- and space-based observations that feed models of the coupled Sun-Earth system at the NOAA/Space Weather Prediction Center (SWPC). Building on the infrastructure of the National Weather Service, SWPC is working toward a fully operational system based on the GOES weather satellite system (constant real-time operation with back-up satellites), the newly launched DSCOVR satellite at L1 (constant real-time data network with AFSCN backup), and operational models of the heliosphere, magnetosphere, and ionosphere/thermosphere/mesophere systems run on the Weather and Climate Operational Super-computing System (WCOSS), one of the worlds largest and fastest operational computer systems that will be upgraded to a dual 2.5 Pflop system in 2016. We review plans for further operational space weather observing platforms being developed in the context of the Space Weather Operations Research and Mitigation (SWORM) task force in the Office of Science and Technology Policy (OSTP) at the White House. We also review the current operational model developments at SWPC, concentrating on the differences between the research codes and the modified real-time versions that must run with zero fault tolerance on the WCOSS systems. Understanding the characteristics and needs of the operational forecasting community is key to producing research into the coupled Sun-Earth system with maximal societal benefit. Title: Constitutive expression of tdTomato protein as a cytotoxicity and proliferation marker for space radiation biology Authors: Chishti, Arif A.; Hellweg, Christine E.; Berger, Thomas; Baumstark-Khan, Christa; Feles, Sebastian; Kätzel, Thorben; Reitz, Günther Bibcode: 2015LSSR....4...35C Altcode: The radiation risk assessment for long-term space missions requires knowledge on the biological effectiveness of different space radiation components, e.g. heavy ions, on the interaction of radiation and other space environmental factors such as microgravity, and on the physical and biological dose distribution in the human body. Space experiments and ground-based experiments at heavy ion accelerators require fast and reliable test systems with an easy readout for different endpoints. In order to determine the effect of different radiation qualities on cellular proliferation and the biological depth dose distribution after heavy ion exposure, a stable human cell line expressing a novel fluorescent protein was established and characterized. tdTomato, a red fluorescent protein of the new generation with fast maturation and high fluorescence intensity, was selected as reporter of cell proliferation. Human embryonic kidney (HEK/293) cells were stably transfected with a plasmid encoding tdTomato under the control of the constitutively active cytomegalovirus (CMV) promoter (ptdTomato-N1). The stably transfected cell line was named HEK-ptdTomato-N1 8. This cytotoxicity biosensor was tested by ionizing radiation (X-rays and accelerated heavy ions) exposure. As biological endpoints, the proliferation kinetics and the cell density reached 100 h after irradiation reflected by constitutive expression of the tdTomato were investigated. Both were reduced dose-dependently after radiation exposure. Finally, the cell line was used for biological weighting of heavy ions of different linear energy transfer (LET) as space-relevant radiation quality. The relative biological effectiveness of accelerated heavy ions in reducing cellular proliferation peaked at an LET of 91 keV/μm. The results of this study demonstrate that the HEK-ptdTomato-N1 reporter cell line can be used as a fast and reliable biosensor system for detection of cytotoxic damage caused by ionizing radiation. Title: Photochemical studies in low Earth orbit for organic compounds related to small bodies, Titan and Mars. Current and future facilities. Authors: Cottin, H.; Saiagh, K.; Nguyen, D.; Grand, N.; Bénilan, Y.; Cloix, M.; Coll, P.; Gazaux, M. -C.; Fray, N.; Khalaf, D.; Raulin, F.; Stalort, F.; Carrasco, N.; Szopa, C.; Chaput, D.; Bertrand, M.; Westall, F.; Mattioda, A.; Quinn, R.; Ricco, A.; Santos, O.; Baratta, G. A.; Strazzulla, G.; Palumbo, M. E.; Le Postollec, A.; Dobrijevic, M.; Coussot, G.; Vigier, F.; Vandenabeele-Trambouze, O.; Incerti, S.; Berger, T. Bibcode: 2015BSRSL..84...60C Altcode: The study of the evolution of organic matter subjected to space conditions, and more specifically to solar photons in the vacuum ultraviolet range (120-200 nm) has been undertaken in low Earth Orbit since the 90's, and implemented on various space platforms. The most recent exposure facilities are BIOPAN outside the Russian automatic capsules FOTON, and EXPOSE-E & -R (1&2) outside the International Space Station. They allow the photolysis of many different samples simultaneously, and provide us with valuable data about the formation and evolution of organic matter in the Solar System (meteorites, comets, Titan's atmosphere, the Martian surface...) and in the Interstellar Medium. They have been used by European teams in the recent past(ORGANIC on BIOPAN V-FOTON M2 and UVolution on BIOPAN VI-FOTON M3, PROCESS on EXPOSE-E, AMINO and ORGANICS on EXPOSE-R), and a new EXPOSE set is currently exposed outside the ISS (PSS on EXPOSE-R2). These existing tools are very valuable; however, they have significant limitations that limit their capabilities and scientific return. One of the most critical issues for current studies is the lack of any in-situ analysis of the evolution of the samples as a function of time. Only two measurements are available for the experiment: one before and one after the exposure. A significant step forward has been achieved with the O/OREOS NASA nanosatellite and the OREOcube ESA project with onboard UV-visible measurements. However, for organic samples, following the evolution of the samples would be more informative and provide greater insight with infrared measurements, which display specific patterns characteristic of major organic functionalities in the mid-infrared range (4000-1000 cm-1). Title: GRB 150212A: Skynet DSO14/GORT observations. Authors: Trotter, A.; Reichart, D.; Lacluyze, A.; Haislip, J.; Smith, A.; Caton, D.; Hawkins, L.; McLin, K.; Cominsky, L.; Aji, A.; Berger, T.; Dow, A.; Foster, A.; Frank, N.; Ivarsen, K.; Maples, M.; Moore, J.; Nysewander, M.; Salemi, C.; Crain, J. A. Bibcode: 2015GCN.17458....1T Altcode: 2015GCN..17458...1T No abstract at ADS Title: GRB 150314A: Skynet Yerkes-41 Observations of the Optical Afterglow. Authors: Trotter, A.; Reichart, D.; Lacluyze, A.; Haislip, J.; Hoette, V.; Cudworth, K.; Harper, D.; Kron, R.; Linder, T.; Russell, R.; Struble, E.; Aji, A.; Berger, T.; Dow, A.; Foster, A.; Frank, N.; Ivarsen, K.; Maples, M.; Moore, J.; Nysewander, M.; Salemi, C.; Crain, J. A. Bibcode: 2015GCN.17577....1T Altcode: 2015GCN..17577...1T No abstract at ADS Title: Mars methane detection and variability at Gale crater Authors: Webster, Christopher R.; Mahaffy, Paul R.; Atreya, Sushil K.; Flesch, Gregory J.; Mischna, Michael A.; Meslin, Pierre-Yves; Farley, Kenneth A.; Conrad, Pamela G.; Christensen, Lance E.; Pavlov, Alexander A.; Martín-Torres, Javier; Zorzano, María-Paz; McConnochie, Timothy H.; Owen, Tobias; Eigenbrode, Jennifer L.; Glavin, Daniel P.; Steele, Andrew; Malespin, Charles A.; Archer, P. Douglas; Sutter, Brad; Coll, Patrice; Freissinet, Caroline; McKay, Christopher P.; Moores, John E.; Schwenzer, Susanne P.; Bridges, John C.; Navarro-Gonzalez, Rafael; Gellert, Ralf; Lemmon, Mark T.; MSL Science Team; Abbey, William; Achilles, Cherie; Agard, Christophe; Alexandre Alves Verdasca, José; Anderson, Dana; Anderson, Robert C.; Anderson, Ryan B.; Appel, Jan Kristoffer; Archer, Paul Douglas; Arevalo, Ricardo; Armiens-Aparicio, Carlos; Arvidson, Raymond; Atlaskin, Evgeny; Atreya, Andrew Sushil; Azeez, Aubrey Sherif; Baker, Burt; Baker, Michael; Balic-Zunic, Tonci; Baratoux, David; Baroukh, Julien; Barraclough, Bruce; Battalio, Michael; Beach, Michael; Bean, Keri; Beck, Pierre; Becker, Richard; Beegle, Luther; Behar, Alberto; Belgacem, Inès; Bell, James F., III; Bender, Steven; Benna, Mehdi; Bentz, Jennifer; Berger, Jeffrey; Berger, Thomas; Berlanga, Genesis; Berman, Daniel; Bish, David; Blacksberg, Jordana; Blake, David F.; José Blanco, Juan; Blaney, Ávalos Diana; Blank, Jennifer; Blau, Hannah; Bleacher, Lora; Boehm, Eckart; Bonnet, Jean-Yves; Botta, Oliver; Böttcher, Stephan; Boucher, Thomas; Bower, Hannah; Boyd, Nick; Boynton, William; Braswell, Shaneen; Breves, Elly; Bridges, John C.; Bridges, Nathan; Brinckerhoff, William; Brinza, David; Bristow, Thomas; Brunet, Claude; Brunner, Anna; Brunner, Will; Buch, Arnaud; Bullock, Mark; Burmeister, Sönke; Burton, John; Buz, Jennifer; Cabane, Michel; Calef, Fred; Cameron, James; Campbell, John L.; Cantor, Bruce; Caplinger, Michael; Clifton, Carey, Jr.; Caride Rodríguez, Javier; Carmosino, Marco; Carrasco Blázquez, Isaías; Cavanagh, Patrick; Charpentier, Antoine; Chipera, Steve; Choi, David; Christensen, Lance; Clark, Benton; Clegg, Sam; Cleghorn, Timothy; Cloutis, Ed; Cody, George; Coll, Patrice; Coman, Ecaterina I.; Conrad, Pamela; Coscia, David; Cousin, Agnès; Cremers, David; Crisp, Joy A.; Cropper, Kevin; Cros, Alain; Cucinotta, Francis; d'Uston, Claude; Davis, Scott; Day, Mackenzie; Daydou, Yves; DeFlores, Lauren; Dehouck, Erwin; Delapp, Dorothea; DeMarines, Julia; Dequaire, Tristan; Des Marais, David; Desrousseaux, Roch; Dietrich, William; Dingler, Robert; Domagal-Goldman, Shawn; Donny, Christophe; Downs, Robert; Drake, Darrell; Dromart, Gilles; Dupont, Audrey; Duston, Brian; Dworkin, Jason P.; Dyar, M. Darby; Edgar, Lauren; Edgett, Kenneth; Edwards, Christopher S.; Edwards, Laurence; Edwards, Peter; Ehlmann, Bethany; Ehresmann, Bent; Eigenbrode, Jennifer; Elliott, Beverley; Elliott, Harvey; Ewing, Ryan; Fabre, Cécile; Fairén, Alberto; Fairén, Alberto; Farley, Kenneth; Farmer, Jack; Fassett, Caleb; Favot, Laurent; Fay, Donald; Fedosov, Fedor; Feldman, Jason; Fendrich, Kim; Fischer, Erik; Fisk, Martin; Fitzgibbon, Mike; Flesch, Gregory; Floyd, Melissa; Flückiger, Lorenzo; Forni, Olivier; Fox, Valerie; Fraeman, Abigail; Francis, Raymond; François, Pascaline; Franz, Heather; Freissinet, Caroline; French, Katherine Louise; Frydenvang, Jens; Garvin, James; Gasnault, Olivier; Geffroy, Claude; Gellert, Ralf; Genzer, Maria; Getty, Stephanie; Glavin, Daniel; Godber, Austin; Goesmann, Fred; Goetz, Walter; Golovin, Dmitry; Gómez Gómez, Felipe; Gómez-Elvira, Javier; Gondet, Brigitte; Gordon, Suzanne; Gorevan, Stephen; Graham, Heather; Grant, John; Grinspoon, David; Grotzinger, John; Guillemot, Philippe; Guo, Jingnan; Gupta, Sanjeev; Guzewich, Scott; Haberle, Robert; Halleaux, Douglas; Hallet, Bernard; Hamilton, Victoria; Hand, Kevin; Hardgrove, Craig; Hardy, Keian; Harker, David; Harpold, Daniel; Harri, Ari-Matti; Harshman, Karl; Hassler, Donald; Haukka, Harri; Hayes, Alexander; Herkenhoff, Kenneth; Herrera, Paul; Hettrich, Sebastian; Heydari, Ezat; Hipkin, Victoria; Hoehler, Tori; Hollingsworth, Jeff; Hudgins, Judy; Huntress, Wesley; Hurowitz, Joel; Hviid, Stubbe; Iagnemma, Karl; Indyk, Stephen; Israël, Guy; Jackson, Ryan Steele; Jacob, Samantha; Jakosky, Bruce; Jean-Rigaud, Laurent; Jensen, Elsa; Kløvgaard Jensen, Jaqueline; Johnson, Jeffrey R.; Johnson, Micah; Johnstone, Stephen; Jones, Andrea; Jones, John H.; Joseph, Jonathan; Joulin, Mélissa; Jun, Insoo; Kah, Linda C.; Kahanpää, Henrik; Kahre, Melinda; Kaplan, Hannah; Karpushkina, Natalya; Kashyap, Srishti; Kauhanen, Janne; Keely, Leslie; Kelley, Simon; Kempe, Fabian; Kemppinen, Osku; Kennedy, Megan R.; Keymeulen, Didier; Kharytonov, Alexander; Kim, Myung-Hee; Kinch, Kjartan; King, Penelope; Kirk, Randolph; Kirkland, Laurel; Kloos, Jacob; Kocurek, Gary; Koefoed, Asmus; Köhler, Jan; Kortmann, Onno; Kotrc, Benjamin; Kozyrev, Alexander; Krau, Johannes; Krezoski, ß. Gillian; Kronyak, Rachel; Krysak, Daniel; Kuzmin, Ruslan; Lacour, Jean-Luc; Lafaille, Vivian; Langevin, Yves; Lanza, Nina; Lapôtre, Mathieu; Larif, Marie-France; Lasue, Jérémie; Le Deit, Laetitia; Le Mouélic, Stéphane; Lee, Ella Mae; Lee, Qiu-Mei; Lee, Rebekka; Lees, David; Lefavor, Matthew; Lemmon, Mark; Lepinette, Alain; Lepore, Malvitte Kate; Leshin, Laurie; Léveillé, Richard; Lewin, Éric; Lewis, Kevin; Li, Shuai; Lichtenberg, Kimberly; Lipkaman, Leslie; Lisov, Denis; Little, Cynthia; Litvak, Maxim; Liu, Lu; Lohf, Henning; Lorigny, Eric; Lugmair, Günter; Lundberg, Angela; Lyness, Eric; Madsen, Morten Bo; Magee, Angela; Mahaffy, Paul; Maki, Justin; Mäkinen, Teemu; Malakhov, Alexey; Malespin, Charles; Malin, Michael; Mangold, Nicolas; Manhes, Gerard; Manning, Heidi; Marchand, Geneviève; Marín Jiménez, Mercedes; Martín García, César; Martin, David K.; Martin, Mildred; Martin, Peter; Martínez Martínez, Germán; Martínez-Frías, Jesús; Martín-Sauceda, Jaime; Martín-Soler, Martín Javier; Martín-Torres, F. Javier; Mason, Emily; Matthews, Tristan; Matthiä, Daniel; Mauchien, Patrick; Maurice, Sylvestre; McAdam, Amy; McBride, Marie; McCartney, Elaina; McConnochie, Timothy; McCullough, Emily; McEwan, Ian; McKay, Christopher; McLain, Hannah; McLennan, Scott; McNair, Sean; Melikechi, Noureddine; Mendaza de Cal, Teresa; Merikallio, Sini; Merritt, Sean; Meslin, Pierre-Yves; Meyer, Michael; Mezzacappa, Alissa; Milkovich, Sarah; Millan, Maëva; Miller, Hayden; Miller, Kristen; Milliken, Ralph; Ming, Douglas; Minitti, Michelle; Mischna, Michael; Mitchell, Julie; Mitrofanov, Igor; Moersch, Jeffrey; Mokrousov, Maxim; Molina, Antonio; Moore, Jurado Casey; Moores, John E.; Mora-Sotomayor, Luis; Moreno, Gines; Morookian, John Michael; Morris, Richard V.; Morrison, Shaunna; Mousset, Valérie; Mrigakshi, Alankrita; Mueller-Mellin, Reinhold; Muller, Jan-Peter; Muñoz Caro, Guillermo; Nachon, Marion; Nastan, Abbey; Navarro López, Sara; Navarro González, Rafael; Nealson, Kenneth; Nefian, Ara; Nelson, Tony; Newcombe, Megan; Newman, Claire; Newsom, Horton; Nikiforov, Sergey; Nikitczuk, Matthew; Niles, Paul; Nixon, Brian; Noblet, Audrey; Noe, Eldar; Nolan, Dobrea Thomas; Oehler, Dorothy; Ollila, Ann; Olson, Timothy; Orthen, Tobias; Owen, Tobias; Ozanne, Marie; de Pablo Hernández, Miguel Ángel; Pagel, Hannah; Paillet, Alexis; Pallier, Etienne; Palucis, Marisa; Parker, Timothy; Parot, Yann; Parra, Alex; Patel, Kiran; Paton, Mark; Paulsen, Gale; Pavlov, Alexander; Pavri, Betina; Peinado-González, Verónica; Pepin, Robert; Peret, Laurent; Pérez, René; Perrett, Glynis; Peterson, Joseph; Pilorget, Cedric; Pinet, Patrick; Pinnick, Veronica; Pla-García, Jorge; Plante, Ianik; Poitrasson, Franck; Polkko, Jouni; Popa, Radu; Posiolova, Liliya; Posner, Arik; Pradler, Irina; Prats, Benito; Prokhorov, Vasily; Raaen, Eric; Radziemski, Leon; Rafkin, Scot; Ramos, Miguel; Rampe, Elizabeth; Rapin, William; Raulin, François; Ravine, Michael; Reitz, Günther; Ren, Jun; Rennó, Nilton; Rice, Melissa; Richardson, Mark; Ritter, Birgit; Rivera-Hernández, Frances; Robert, François; Robertson, Kevin; Rodriguez Manfredi, José Antonio; José Romeral-Planelló, Julio; Rowland, Scott; Rubin, David; Saccoccio, Muriel; Said, David; Salamon, Andrew; Sanin, Anton; Sans Fuentes, Sara Alejandra; Saper, Lee; Sarrazin, Philippe; Sautter, Violaine; Savijärvi, Hannu; Schieber, Juergen; Schmidt, Mariek; Schmidt, Walter; Scholes, Daniel; Schoppers, Marcel; Schröder, Susanne; Schwenzer, Susanne P.; Sciascia Borlina, Cauê; Scodary, Anthony; Sebastián Martínez, Eduardo; Sengstacken, Aaron; Shechet, Jennifer Griffes; Shterts, Ruslan; Siebach, Kirsten; Siili, Tero; Simmonds, John J.; Sirven, Jean-Baptiste; Slavney, Susan; Sletten, Ronald; Smith, Michael D.; Sobron Sanchez, Pablo; Spanovich, Nicole; Spray, John; Spring, Justin; Squyres, Steven; Stack, Katie; Stalport, Fabien; Starr, Richard; Stein, Andrew Steele Thomas; Stern, Jennifer; Stewart, Noel; Stewart, Wayne; Stipp, Svane Susan Louise; Stoiber, Kevin; Stolper, Edward; Sucharski, Robert; Sullivan, Robert; Summons, Roger; Sumner, Dawn Y.; Sun, Vivian; Supulver, Kimberley; Sutter, Brad; Szopa, Cyril; Tan, Florence; Tate, Christopher; Teinturier, Samuel; ten Kate, Inge Loes; Thomas, Alicia; Thomas, Peter; Thompson, Lucy; Thuillier, Franck; Thulliez, Emmanual; Tokar, Robert; Toplis, Michael; de la Torre Juárez, Manuel; Torres Redondo, Josefina; Trainer, Melissa; Treiman, Allan; Tretyakov, Vladislav; Ullán-Nieto, Aurora; Urqui-O'Callaghan, Roser; Valentín-Serrano, Patricia; Van Beek, Jason; Van Beek, Tessa; VanBommel, Scott; Vaniman, David; Varenikov, Alexey; Vasavada, Ashwin R.; Vasconcelos, Paulo; de Vicente-Retortillo Rubalcaba, Álvaro; Vicenzi, Edward; Vostrukhin, Andrey; Voytek, Mary; Wadhwa, Meenakshi; Ward, Jennifer; Watkins, Jessica; Webster, Christopher R.; Weigle, Gerald; Wellington, Danika; Westall, Frances; Wiens, Roger; Wilhelm, Mary Beth; Williams, Amy; Williams, Joshua; Williams, Rebecca; Williams, Richard B.; Williford, Kenneth; Wilson, Michael A.; Wilson, Sharon A.; Wimmer-Schweingruber, Robert; Wolff, Michael; Wong, Michael; Wray, James; Yana, Charles; Yen, Albert; Yingst, Aileen; Zeitlin, Cary; Zimdar, Robert; Zorzano Mier, María-Paz Bibcode: 2015Sci...347..415W Altcode: Reports of plumes or patches of methane in the martian atmosphere that vary over monthly time scales have defied explanation to date. From in situ measurements made over a 20-month period by the tunable laser spectrometer of the Sample Analysis at Mars instrument suite on Curiosity at Gale crater, we report detection of background levels of atmospheric methane of mean value 0.69 ± 0.25 parts per billion by volume (ppbv) at the 95% confidence interval (CI). This abundance is lower than model estimates of ultraviolet degradation of accreted interplanetary dust particles or carbonaceous chondrite material. Additionally, in four sequential measurements spanning a 60-sol period (where 1 sol is a martian day), we observed elevated levels of methane of 7.2 ± 2.1 ppbv (95% CI), implying that Mars is episodically producing methane from an additional unknown source. Title: GRB 150318A: Skynet PROMPT-CTIO Observations. Authors: Trotter, A.; Reichart, D.; Haislip, J.; Aji, A.; Beauchemin, R.; Berger, T.; Dow, A.; Foster, A.; Frank, N.; Hinckle, M.; Ivarsen, K.; Lacluyze, A.; Maples, M.; Moore, J.; Nysewander, M.; Salemi, C.; Zbinden, L.; Crain, J. A. Bibcode: 2015GCN.17605....1T Altcode: 2015GCN..17605...1T No abstract at ADS Title: Cosmic radiation exposure of biological test systems during the EXPOSE-R mission Authors: Berger, Thomas; Hajek, Michael; Bilski, Pawel Bibcode: 2015IJAsB..14...27B Altcode: In the frame of the EXPOSE-R mission outside the Russian Zvezda Module of the International Space Station (ISS) passive thermoluminescence dosimeters were applied to measure the radiation exposure of biological samples. The detectors were located beneath the sample carriers to determine the dose levels for maximum shielding. The dose measured beneath the sample carriers varied between 317 +/- 10 and 230 +/- 2 mGy, which amount to an average dose rate of 381 +/- 12 and 276 +/- 2 μGy d-1. These values are close to those assessed for the interior of the ISS and reflect the high shielding of the biological experiments within the EXPOSE-R facility. As a consequence of the high shielding (several g cm-2), the biological samples were predominantly exposed to galactic cosmic heavy ions and trapped protons in the Earth's radiation belts, whereas the trapped electrons did not reach the samples. Title: Estimating the temporal cutoff-rigidity variations and their implication on manned space missions Authors: Herbst, K.; Labrenz, J.; Kopp, A.; Heber, B.; Burmeister, S.; Berger, T. Bibcode: 2014AGUFMSM31A4156H Altcode: Using the PLANETOCOSMICS code the vertical cutoff rigidity or equivalently the minimum energy a particle must have in order to reach a given location on Earth is calculated. The program allows investigations that depend on the Earth's magnetic field strength and geometry as a function of time. Today it is well known that the magnetic field is the subject of temporal variations on long as well as short time-scales which reflects itself, e.g., in the global vertical cutoff-rigidity distribution at 20 km altitude (see Herbst et al., 2013). Focusing on the changes during the era of manned space missions (1961-2014) we extend our analysis of the vertical cutoff rigidity variations to about 450 km i.e. to the International Space Station (ISS) orbit. The outcome of this analysis will be compared to measurements of the DOSimetry TELescope (DOSTEL), an instrument that has been operational for several time periods onboard the ISS, allowing to determine the response function of the instrument. Using the Force-Field parameter derived from neutron monitors (see Usoskin et al., 2011) we will present maps of DOSTEL measurements for more than 50 years that are caused by galactic cosmic ray variations along hypothetical ISS orbits. Title: First High-resolution Spectroscopic Observations by IRIS of a Fast, Helical Prominence Eruption Associated with a Coronal Mass Ejection Authors: Liu, W.; De Pontieu, B.; Okamoto, T. J.; Vial, J. C.; Title, A. M.; Antolin, P.; Berger, T. E.; Uitenbroek, H. Bibcode: 2014AGUFMSH11D..04L Altcode: High-resolution spectroscopic observations of prominence eruptions and associated coronal mass ejections (CMEs) are rare but can provide valuable plasma and energy diagnostics. New opportunities have recently become available with the advent of the Interface Region Imaging Spectrograph (IRIS) mission equipped with high resolution of 0.33-0.4 arcsec in space and 1 km/s in velocity, together with the Hinode Solar Optical Telescope of 0.2 arcsec spatial resolution. We report the first result of joint IRIS-Hinode observations of a spectacular prominence eruption occurring on 2014-May-09. IRIS detected a maximum redshift of 450 km/s, which, combined with the plane-of-sky speed of 800 km/s, gives a large velocity vector of 920 km/s at 30 degrees from the sky plane. This direction agrees with the source location at 30 degrees behind the limb observed by STEREO-A and indicates a nearly vertical ejection. We found two branches of redshifts separated by 200 km/s appearing in all strong lines at chromospheric to transition-region temperatures, including Mg II k/h, C II, and Si IV, suggesting a hollow, rather than solid, cone in the velocity space of the ejected material. Opposite blue- and redshifts on the two sides of the prominence exhibit corkscrew variations both in space and time, suggestive of unwinding rotations of a left-handed helical flux rope. Some erupted material returns as nearly streamline flows, exhibiting distinctly narrow line widths (~10 km/s), about 50% of those of the nearby coronal rain at the apexes of coronal loops, where the rain material is initially formed out of cooling condensation. We estimate the mass and kinetic energy of the ejected and returning material and compare them with those of the associated CME. We will discuss the implications of these observations for CME initiation mechanisms. Title: The Daniel K. Inouye Solar Telescope: A Project Update. Authors: Rimmele, T.; Berger, T.; McMullin, J.; Warner, M.; Casinsi, R.; Kuhn, J.; Lin, H.; Woeger, F.; Schmidt, W.; Tritschler, A.; Inouye, Daniel K.; Solar Telescope Team Bibcode: 2014amos.confE..43R Altcode: The Advanced Technology Solar Telescope will be the largest solar facility ever built. Designed and developed to meet the needs of critical high resolution and high sensitivity spectral and polarimetric observations of the sun, this facility will support key experiments for the study of solar magnetism and its influence on the solar wind, flares, coronal mass ejections and solar irradiance variability. The 4-meter diameter facility will operate over a broad wavelength range (0.35 to 28 microns), using state-of-the-art adaptive optics systems to provide diffraction limited imaging and the ability to resolve features approximately 20 km on the Sun. Five first light instruments will be available at the start of operations. Key subsystems have been designed and fabrication is well underway, including the site construction, which began in December 2012. We provide an update on the development of the facilities both on site at the Haleakala Observatories in Maui and the development of components around the world. We present the overall construction and integration schedule leading to the start of operations in mid-2019 and touch on operations aspects. Title: Construction status of the Daniel K. Inouye Solar Telescope Authors: McMullin, Joseph P.; Rimmele, Thomas R.; Martínez Pillet, Valentin; Berger, Thomas E.; Casini, Roberto; Craig, Simon C.; Elmore, David F.; Goodrich, Bret D.; Hegwer, Steve L.; Hubbard, Robert P.; Johansson, Erik M.; Kuhn, Jeffrey R.; Lin, Haosheng; McVeigh, William; Schmidt, Wolfgang; Shimko, Steve; Tritschler, Alexandra; Warner, Mark; Wöger, Friedrich Bibcode: 2014SPIE.9145E..25M Altcode: The Daniel K. Inouye Solar Telescope (DKIST, renamed in December 2013 from the Advanced Technology Solar Telescope) will be the largest solar facility built when it begins operations in 2019. Designed and developed to meet the needs of critical high resolution and high sensitivity spectral and polarimetric observations of the Sun, the observatory will enable key research for the study of solar magnetism and its influence on the solar wind, flares, coronal mass ejections and solar irradiance variations. The 4-meter class facility will operate over a broad wavelength range (0.38 to 28 microns, initially 0.38 to 5 microns), using a state-of-the-art adaptive optics system to provide diffraction-limited imaging and the ability to resolve features approximately 25 km on the Sun. Five first-light instruments will be available at the start of operations: Visible Broadband Imager (VBI; National Solar Observatory), Visible SpectroPolarimeter (ViSP; NCAR High Altitude Observatory), Visible Tunable Filter (VTF; Kiepenheuer Institut für Sonnenphysik), Diffraction Limited Near InfraRed SpectroPolarimeter (DL-NIRSP; University of Hawai'i, Institute for Astronomy) and the Cryogenic Near InfraRed SpectroPolarimeter (Cryo-NIRSP; University of Hawai'i, Institute for Astronomy). As of mid-2014, the key subsystems have been designed and fabrication is well underway, including the site construction, which began in December 2012. We provide an update on the development of the facilities both on site at the Haleakalā Observatories on Maui and the development of components around the world. We present the overall construction and integration schedule leading to the handover to operations in mid 2019. In addition, we outline the evolving challenges being met by the project, spanning the full spectrum of issues covering technical, fiscal, and geographical, that are specific to this project, though with clear counterparts to other large astronomical construction projects. Title: The Interface Region Imaging Spectrograph (IRIS) Authors: De Pontieu, B.; Title, A. M.; Lemen, J. R.; Kushner, G. D.; Akin, D. J.; Allard, B.; Berger, T.; Boerner, P.; Cheung, M.; Chou, C.; Drake, J. F.; Duncan, D. W.; Freeland, S.; Heyman, G. F.; Hoffman, C.; Hurlburt, N. E.; Lindgren, R. W.; Mathur, D.; Rehse, R.; Sabolish, D.; Seguin, R.; Schrijver, C. J.; Tarbell, T. D.; Wülser, J. -P.; Wolfson, C. J.; Yanari, C.; Mudge, J.; Nguyen-Phuc, N.; Timmons, R.; van Bezooijen, R.; Weingrod, I.; Brookner, R.; Butcher, G.; Dougherty, B.; Eder, J.; Knagenhjelm, V.; Larsen, S.; Mansir, D.; Phan, L.; Boyle, P.; Cheimets, P. N.; DeLuca, E. E.; Golub, L.; Gates, R.; Hertz, E.; McKillop, S.; Park, S.; Perry, T.; Podgorski, W. A.; Reeves, K.; Saar, S.; Testa, P.; Tian, H.; Weber, M.; Dunn, C.; Eccles, S.; Jaeggli, S. A.; Kankelborg, C. C.; Mashburn, K.; Pust, N.; Springer, L.; Carvalho, R.; Kleint, L.; Marmie, J.; Mazmanian, E.; Pereira, T. M. D.; Sawyer, S.; Strong, J.; Worden, S. P.; Carlsson, M.; Hansteen, V. H.; Leenaarts, J.; Wiesmann, M.; Aloise, J.; Chu, K. -C.; Bush, R. I.; Scherrer, P. H.; Brekke, P.; Martinez-Sykora, J.; Lites, B. W.; McIntosh, S. W.; Uitenbroek, H.; Okamoto, T. J.; Gummin, M. A.; Auker, G.; Jerram, P.; Pool, P.; Waltham, N. Bibcode: 2014SoPh..289.2733D Altcode: 2014arXiv1401.2491D; 2014SoPh..tmp...25D The Interface Region Imaging Spectrograph (IRIS) small explorer spacecraft provides simultaneous spectra and images of the photosphere, chromosphere, transition region, and corona with 0.33 - 0.4 arcsec spatial resolution, two-second temporal resolution, and 1 km s−1 velocity resolution over a field-of-view of up to 175 arcsec × 175 arcsec. IRIS was launched into a Sun-synchronous orbit on 27 June 2013 using a Pegasus-XL rocket and consists of a 19-cm UV telescope that feeds a slit-based dual-bandpass imaging spectrograph. IRIS obtains spectra in passbands from 1332 - 1358 Å, 1389 - 1407 Å, and 2783 - 2834 Å, including bright spectral lines formed in the chromosphere (Mg II h 2803 Å and Mg II k 2796 Å) and transition region (C II 1334/1335 Å and Si IV 1394/1403 Å). Slit-jaw images in four different passbands (C II 1330, Si IV 1400, Mg II k 2796, and Mg II wing 2830 Å) can be taken simultaneously with spectral rasters that sample regions up to 130 arcsec × 175 arcsec at a variety of spatial samplings (from 0.33 arcsec and up). IRIS is sensitive to emission from plasma at temperatures between 5000 K and 10 MK and will advance our understanding of the flow of mass and energy through an interface region, formed by the chromosphere and transition region, between the photosphere and corona. This highly structured and dynamic region not only acts as the conduit of all mass and energy feeding into the corona and solar wind, it also requires an order of magnitude more energy to heat than the corona and solar wind combined. The IRIS investigation includes a strong numerical modeling component based on advanced radiative-MHD codes to facilitate interpretation of observations of this complex region. Approximately eight Gbytes of data (after compression) are acquired by IRIS each day and made available for unrestricted use within a few days of the observation. Title: The Rayleigh-Taylor Instability and the role of Prominences in the Chromosphere-Corona Mass Cycle Authors: Berger, Thomas; Liu, Wei; Hillier, Andrew; Scullion, Eamon; Low, Boon Chye Bibcode: 2014AAS...22421201B Altcode: We review recent results in the study of so-called "prominence bubbles", a buoyant instability discovered in quiescent solar prominences by the Hinode/SOT instrument in 2007. Analysis of the plasma flows along the boundary of the bubbles indicates that shear flows leading to Kelvin-Helmholtz instability waves can develop into the seed perturbations triggering the Rayleigh-Taylor instability. The non-linear phase of the RT instability leads to the formation of large turbulent plumes that transport the bubble plasma (and presumably magnetic flux) into the overlying coronal flux rope. We propose that the upward turbulent transport of hot bubble plasma and the downflows of cooler chromospheric plasma in the prominence are related aspects of a large-scale "chromosphere-corona mass cycle" in which hot plasma and magnetic flux and helicity from the chromosphere are transported upwards while the cooler prominence plasma downflows, which decouple from the magnetic field they are originally frozen-into, represent the condensation return flows of the cycle. This cycling enables a mechanism by which magnetic flux and helicity build up in the coronal flux rope while mass drains out of the flux rope, eventually triggering a "loss of confinement" eruption in the form of a CME. Title: Evidence of Magnetic Reconnection Involving Partially Ionized Coronal Rain near Null Points Observed by SDO/AIA and IRIS Authors: Liu, Wei; Antolin, Patrick; Sun, Xudong; Berger, Thomas E. Bibcode: 2014shin.confE..50L Altcode: Coronal rain is cool, partially ionized material formed in the hot, fully ionized corona. We report a newly discovered class of coronal rain formed near cusp-shaped portions of coronal loops, indicative of topological null points. We present evidence of cross-field flows associated with magnetic reconnection near such null points from SDO/AIA and IRIS observations, investigate the responsible magnetic environment, and infer clues to where and when catastrophic cooling take place to produce coronal rain. We also discuss the implications of such a cooling process for the enigmatic coronal heating mechanisms (e.g., Antolin et al. 2010) and compare transient coronal rain and persistent prominence downflows. Title: IRIS Observations of Coronal Rain and Prominences: Return Flows of the Chromosphere-Corona Mass Cycle Authors: Liu, Wei; Berger, Thomas; Antolin, Patrick; Schrijver, Karel Bibcode: 2014AAS...22431303L Altcode: It has recently been recognized that a mass cycle (e.g., Berger et al. 2011; McIntosh et al. 2012) between the hot, tenuous solar corona and the cool, dense chromosphere underneath it plays an important role in the mass budget and dynamic evolution of the solar atmosphere. Although the corona ultimately loses mass through the solar wind and coronal mass ejections, a fraction of its mass returns to the chromosphere in coronal rain, downflows of prominences, and other as-yet unidentified processes. We present here analysis of joint observations of IRIS, SDO/AIA, and Hinode/SOT of such phenomena. By utilizing the wide temperature coverage (logT: 4 - 7) provided by these instruments combined, we track the coronal cooling sequence (e.g., Schrijver 2001; Liu et al. 2012; Berger et al. 2012) leading to the formation of such material at transition region or chromospheric temperatures (logT: 4 - 5) in the million-degree corona. We compare the cooling times with those expected from the radiative cooling instability. We also measure the kinematics and densities of such downflows and infer their mass fluxes, which are compared to the upward mass fluxes into the corona, e.g., those associated with spicules and flux emergence. Special attention is paid to coronal rain formed near cusp-shaped portions of coronal loops, funnel-shaped prominences at dips of coronal loops, and their respective magnetic environments. With the information about where and when such catastrophic cooling events take place, we discuss the implications for the enigmatic coronal heating mechanisms (e.g., Antolin et al. 2010). Title: Dose and dose equivalent and related risk during a cruise to Mars Authors: Reitz, Günther; Matthiae, Daniel; Berger, Thomas; Zeitlin, Cary; Hassler, Don; Rafkin, Scott; Ehresmann, Bent; Cucinotta, Francis; Wimmer-Schweingruber, Robert; Boehm, Eckart; Burmeister, Soenke; Guo, Jingnan; Koehler, jan; Martin, Cesar; Boettcher, Stephan; Brinza, David; Posner, Arik Bibcode: 2014EGUGA..1616162R Altcode: The radiation exposure in space can be estimated with numerical simulations applying different models for the galactic cosmic rays (GCR) irradiating a defined shielding geometry or by in situ measurements. A comparison of commonly used GCR models, Badhwar-O'Neill2010, Burger-Usoskin, CREME2009/CREME96, and the recently released Badhwar-O'Neill 2011 with the newly developed DLR model show considerable differences in particle fluences. The differences arising in the calculated radiation exposure by applying these models were quantified in terms of absorbed dose and dose equivalent rates using the GEANT4 Monte-Carlo framework for different shielding thicknesses and the cumulative shielding distribution of the MSL transfer vehicle. The calculations are compared with actual measurement of the Radiation Assessment detector (RAD) of the Mars Science Lab (MSL) on its cruise towards Mars and on the surface of Mars. From the dose equivalents measured and calculated estimates of the upper and lower limits for the risks for a human flight to Mars assuming the radiation environment experienced by MSL-RAD are given using the NASA risk model. Title: GRB 141026A: Skynet PROMPT-CTIO/Yerkes-41 Observations. Authors: Trotter, A.; Haislip, J.; Reichart, D.; Hoette, V.; Cudworth, K.; Harper, D.; Kron, R.; Linder, T.; Russell, R.; Struble, E.; Aji, A.; Beauchemin, R.; Berger, T.; Dow, A.; Foster, A.; Frank, N.; Hinckle, M.; Ivarsen, K.; Lacluyze, A.; Maples, M.; Moore, J.; Nysewander, M.; Salemi, C.; Zbinden, L.; Crain, J. A. Bibcode: 2014GCN.16967....1T Altcode: 2014GCN..16967...1T No abstract at ADS Title: GRB 140215A: continued skynet PROMPT observations of the optical afterglow. Authors: Lacluyze, A.; Haislip, J.; Reichart, D.; Trotter, A.; Poshyachinda, S.; Rujopakarn, W.; Foster, A.; Frank, N.; Ivarsen, K.; Moore, J.; Nysewander, M.; Beauchemin, R.; Berger, T.; Carroll, M.; Cromartie, H. T.; Egger, R.; Hinckle, M.; Ireland, A.; Maples, M.; Scott, L.; Crain, J. A. Bibcode: 2014GCN.15858....1L Altcode: 2014GCN..15858...1L No abstract at ADS Title: Mars' Surface Radiation Environment Measured with the Mars Science Laboratory's Curiosity Rover Authors: Hassler, Donald M.; Zeitlin, Cary; Wimmer-Schweingruber, Robert F.; Ehresmann, Bent; Rafkin, Scot; Eigenbrode, Jennifer L.; Brinza, David E.; Weigle, Gerald; Böttcher, Stephan; Böhm, Eckart; Burmeister, Soenke; Guo, Jingnan; Köhler, Jan; Martin, Cesar; Reitz, Guenther; Cucinotta, Francis A.; Kim, Myung-Hee; Grinspoon, David; Bullock, Mark A.; Posner, Arik; Gómez-Elvira, Javier; Vasavada, Ashwin; Grotzinger, John P.; MSL Science Team; Kemppinen, Osku; Cremers, David; Bell, James F.; Edgar, Lauren; Farmer, Jack; Godber, Austin; Wadhwa, Meenakshi; Wellington, Danika; McEwan, Ian; Newman, Claire; Richardson, Mark; Charpentier, Antoine; Peret, Laurent; King, Penelope; Blank, Jennifer; Schmidt, Mariek; Li, Shuai; Milliken, Ralph; Robertson, Kevin; Sun, Vivian; Baker, Michael; Edwards, Christopher; Ehlmann, Bethany; Farley, Kenneth; Griffes, Jennifer; Miller, Hayden; Newcombe, Megan; Pilorget, Cedric; Rice, Melissa; Siebach, Kirsten; Stack, Katie; Stolper, Edward; Brunet, Claude; Hipkin, Victoria; Léveillé, Richard; Marchand, Geneviève; Sánchez, Pablo Sobrón; Favot, Laurent; Cody, George; Steele, Andrew; Flückiger, Lorenzo; Lees, David; Nefian, Ara; Martin, Mildred; Gailhanou, Marc; Westall, Frances; Israël, Guy; Agard, Christophe; Baroukh, Julien; Donny, Christophe; Gaboriaud, Alain; Guillemot, Philippe; Lafaille, Vivian; Lorigny, Eric; Paillet, Alexis; Pérez, René; Saccoccio, Muriel; Yana, Charles; Armiens-Aparicio, Carlos; Rodríguez, Javier Caride; Blázquez, Isaías Carrasco; Gómez, Felipe Gómez; Hettrich, Sebastian; Malvitte, Alain Lepinette; Jiménez, Mercedes Marín; Martínez-Frías, Jesús; Martín-Soler, Javier; Martín-Torres, F. Javier; Jurado, Antonio Molina; Mora-Sotomayor, Luis; Caro, Guillermo Muñoz; López, Sara Navarro; Peinado-González, Verónica; Pla-García, Jorge; Manfredi, José Antonio Rodriguez; Romeral-Planelló, Julio José; Fuentes, Sara Alejandra Sans; Martinez, Eduardo Sebastian; Redondo, Josefina Torres; Urqui-O'Callaghan, Roser; Mier, María-Paz Zorzano; Chipera, Steve; Lacour, Jean-Luc; Mauchien, Patrick; Sirven, Jean-Baptiste; Manning, Heidi; Fairén, Alberto; Hayes, Alexander; Joseph, Jonathan; Squyres, Steven; Sullivan, Robert; Thomas, Peter; Dupont, Audrey; Lundberg, Angela; Melikechi, Noureddine; Mezzacappa, Alissa; Berger, Thomas; Matthia, Daniel; Prats, Benito; Atlaskin, Evgeny; Genzer, Maria; Harri, Ari-Matti; Haukka, Harri; Kahanpää, Henrik; Kauhanen, Janne; Kemppinen, Osku; Paton, Mark; Polkko, Jouni; Schmidt, Walter; Siili, Tero; Fabre, Cécile; Wray, James; Wilhelm, Mary Beth; Poitrasson, Franck; Patel, Kiran; Gorevan, Stephen; Indyk, Stephen; Paulsen, Gale; Gupta, Sanjeev; Bish, David; Schieber, Juergen; Gondet, Brigitte; Langevin, Yves; Geffroy, Claude; Baratoux, David; Berger, Gilles; Cros, Alain; d'Uston, Claude; Forni, Olivier; Gasnault, Olivier; Lasue, Jérémie; Lee, Qiu-Mei; Maurice, Sylvestre; Meslin, Pierre-Yves; Pallier, Etienne; Parot, Yann; Pinet, Patrick; Schröder, Susanne; Toplis, Mike; Lewin, Éric; Brunner, Will; Heydari, Ezat; Achilles, Cherie; Oehler, Dorothy; Sutter, Brad; Cabane, Michel; Coscia, David; Israël, Guy; Szopa, Cyril; Dromart, Gilles; Robert, François; Sautter, Violaine; Le Mouélic, Stéphane; Mangold, Nicolas; Nachon, Marion; Buch, Arnaud; Stalport, Fabien; Coll, Patrice; François, Pascaline; Raulin, François; Teinturier, Samuel; Cameron, James; Clegg, Sam; Cousin, Agnès; DeLapp, Dorothea; Dingler, Robert; Jackson, Ryan Steele; Johnstone, Stephen; Lanza, Nina; Little, Cynthia; Nelson, Tony; Wiens, Roger C.; Williams, Richard B.; Jones, Andrea; Kirkland, Laurel; Treiman, Allan; Baker, Burt; Cantor, Bruce; Caplinger, Michael; Davis, Scott; Duston, Brian; Edgett, Kenneth; Fay, Donald; Hardgrove, Craig; Harker, David; Herrera, Paul; Jensen, Elsa; Kennedy, Megan R.; Krezoski, Gillian; Krysak, Daniel; Lipkaman, Leslie; Malin, Michael; McCartney, Elaina; McNair, Sean; Nixon, Brian; Posiolova, Liliya; Ravine, Michael; Salamon, Andrew; Saper, Lee; Stoiber, Kevin; Supulver, Kimberley; Van Beek, Jason; Van Beek, Tessa; Zimdar, Robert; French, Katherine Louise; Iagnemma, Karl; Miller, Kristen; Summons, Roger; Goesmann, Fred; Goetz, Walter; Hviid, Stubbe; Johnson, Micah; Lefavor, Matthew; Lyness, Eric; Breves, Elly; Dyar, M. Darby; Fassett, Caleb; Blake, David F.; Bristow, Thomas; DesMarais, David; Edwards, Laurence; Haberle, Robert; Hoehler, Tori; Hollingsworth, Jeff; Kahre, Melinda; Keely, Leslie; McKay, Christopher; Wilhelm, Mary Beth; Bleacher, Lora; Brinckerhoff, William; Choi, David; Conrad, Pamela; Dworkin, Jason P.; Floyd, Melissa; Freissinet, Caroline; Garvin, James; Glavin, Daniel; Harpold, Daniel; Jones, Andrea; Mahaffy, Paul; Martin, David K.; McAdam, Amy; Pavlov, Alexander; Raaen, Eric; Smith, Michael D.; Stern, Jennifer; Tan, Florence; Trainer, Melissa; Meyer, Michael; Voytek, Mary; Anderson, Robert C.; Aubrey, Andrew; Beegle, Luther W.; Behar, Alberto; Blaney, Diana; Calef, Fred; Christensen, Lance; Crisp, Joy A.; DeFlores, Lauren; Ehlmann, Bethany; Feldman, Jason; Feldman, Sabrina; Flesch, Gregory; Hurowitz, Joel; Jun, Insoo; Keymeulen, Didier; Maki, Justin; Mischna, Michael; Morookian, John Michael; Parker, Timothy; Pavri, Betina; Schoppers, Marcel; Sengstacken, Aaron; Simmonds, John J.; Spanovich, Nicole; Juarez, Manuel de la Torre; Webster, Christopher R.; Yen, Albert; Archer, Paul Douglas; Jones, John H.; Ming, Douglas; Morris, Richard V.; Niles, Paul; Rampe, Elizabeth; Nolan, Thomas; Fisk, Martin; Radziemski, Leon; Barraclough, Bruce; Bender, Steve; Berman, Daniel; Dobrea, Eldar Noe; Tokar, Robert; Vaniman, David; Williams, Rebecca M. E.; Yingst, Aileen; Lewis, Kevin; Leshin, Laurie; Cleghorn, Timothy; Huntress, Wesley; Manhès, Gérard; Hudgins, Judy; Olson, Timothy; Stewart, Noel; Sarrazin, Philippe; Grant, John; Vicenzi, Edward; Wilson, Sharon A.; Hamilton, Victoria; Peterson, Joseph; Fedosov, Fedor; Golovin, Dmitry; Karpushkina, Natalya; Kozyrev, Alexander; Litvak, Maxim; Malakhov, Alexey; Mitrofanov, Igor; Mokrousov, Maxim; Nikiforov, Sergey; Prokhorov, Vasily; Sanin, Anton; Tretyakov, Vladislav; Varenikov, Alexey; Vostrukhin, Andrey; Kuzmin, Ruslan; Clark, Benton; Wolff, Michael; McLennan, Scott; Botta, Oliver; Drake, Darrell; Bean, Keri; Lemmon, Mark; Schwenzer, Susanne P.; Anderson, Ryan B.; Herkenhoff, Kenneth; Lee, Ella Mae; Sucharski, Robert; Hernández, Miguel Ángel de Pablo; Ávalos, Juan José Blanco; Ramos, Miguel; Malespin, Charles; Plante, Ianik; Muller, Jan-Peter; Navarro-González, Rafael; Ewing, Ryan; Boynton, William; Downs, Robert; Fitzgibbon, Mike; Harshman, Karl; Morrison, Shaunna; Dietrich, William; Kortmann, Onno; Palucis, Marisa; Sumner, Dawn Y.; Williams, Amy; Lugmair, Günter; Wilson, Michael A.; Rubin, David; Jakosky, Bruce; Balic-Zunic, Tonci; Frydenvang, Jens; Jensen, Jaqueline Kløvgaard; Kinch, Kjartan; Koefoed, Asmus; Madsen, Morten Bo; Stipp, Susan Louise Svane; Boyd, Nick; Campbell, John L.; Gellert, Ralf; Perrett, Glynis; Pradler, Irina; VanBommel, Scott; Jacob, Samantha; Owen, Tobias; Rowland, Scott; Atlaskin, Evgeny; Savijärvi, Hannu; García, César Martín; Mueller-Mellin, Reinhold; Bridges, John C.; McConnochie, Timothy; Benna, Mehdi; Franz, Heather; Bower, Hannah; Brunner, Anna; Blau, Hannah; Boucher, Thomas; Carmosino, Marco; Atreya, Sushil; Elliott, Harvey; Halleaux, Douglas; Rennó, Nilton; Wong, Michael; Pepin, Robert; Elliott, Beverley; Spray, John; Thompson, Lucy; Gordon, Suzanne; Newsom, Horton; Ollila, Ann; Williams, Joshua; Vasconcelos, Paulo; Bentz, Jennifer; Nealson, Kenneth; Popa, Radu; Kah, Linda C.; Moersch, Jeffrey; Tate, Christopher; Day, Mackenzie; Kocurek, Gary; Hallet, Bernard; Sletten, Ronald; Francis, Raymond; McCullough, Emily; Cloutis, Ed; ten Kate, Inge Loes; Kuzmin, Ruslan; Arvidson, Raymond; Fraeman, Abigail; Scholes, Daniel; Slavney, Susan; Stein, Thomas; Ward, Jennifer; Berger, Jeffrey; Moores, John E. Bibcode: 2014Sci...343D.386H Altcode: The Radiation Assessment Detector (RAD) on the Mars Science Laboratory's Curiosity rover began making detailed measurements of the cosmic ray and energetic particle radiation environment on the surface of Mars on 7 August 2012. We report and discuss measurements of the absorbed dose and dose equivalent from galactic cosmic rays and solar energetic particles on the martian surface for ~300 days of observations during the current solar maximum. These measurements provide insight into the radiation hazards associated with a human mission to the surface of Mars and provide an anchor point with which to model the subsurface radiation environment, with implications for microbial survival times of any possible extant or past life, as well as for the preservation of potential organic biosignatures of the ancient martian environment. Title: Introduction to session F2.3 ``Space Radiation Dosimetry—Measurements and Models, Detector Development and Groundbased Characterisation'' Authors: Berger, Thomas Bibcode: 2014cosp...40E.293B Altcode: Introduction to the session F2.3 "Space Radiation Dosimetry" Title: Prominence Science with ATST Instrumentation Authors: Rimmele, Thomas; Berger, Thomas; Casini, Roberto; Elmore, David; Kuhn, Jeff; Lin, Haosheng; Schmidt, Wolfgang; Wöger, Friedrich Bibcode: 2014IAUS..300..362R Altcode: The 4m Advance Technology Solar Telescope (ATST) is under construction on Maui, HI. With its unprecedented resolution and photon collecting power ATST will be an ideal tool for studying prominences and filaments and their role in producing Coronal Mass Ejections that drive Space Weather. The ATST facility will provide a set of first light instruments that enable imaging and spectroscopy of the dynamic filament and prominence structure at 8 times the resolution of Hinode. Polarimeters allow high precision chromospheric and coronal magnetometry at visible and infrared (IR) wavelengths. This paper summarizes the capabilities of the ATST first-light instrumentation with focus on prominence and filament science. Title: European Crew Personal Active Dosimeter (EuCPAD), a novel dosimetry system utilizing operational and scientific synergies for the benefit of humans in space Authors: Straube, Ulrich; Berger, Thomas Bibcode: 2014cosp...40E3215S Altcode: A significant expansion of Human presence in space can be recognized over the last decade. Not only the frequency of human space mission did rise, but also time in space, mission duration with extended flights lasting half a year or more are becoming "standard". Despite the challenges to human health and well-being are still significant, or may even increase with mission length and work density. Also radiation exposure in space remains one of the inevitable and dominating factors relevant to crew- health, -safety and therefore mission success. The radiation environment that the space crews are exposed to differs significantly as compared to earth. Exposure in flight exceed doses that are usually received by terrestrial radiation workers on ground. Expanding "medical" demands are not a solely characteristics of current and current and upcoming mission scenarios. Likewise the margins for what is understood as "efficient utilization" for the fully operational science platform ISS, are immense. Understanding, accepting and approaching these challenges ESA-HSO did choose a particular pass of implementation for one of their current developments. Exploiting synergies of research, science and medical operational aspects, the "European Crew Personal Active Dosimeter for Astronauts (EuCPAD)" development exactly addresses these circumstances. It becomes novel part of ESA Radiation Protection Initiative for astronauts. The EuCPAD project aims at the development and manufacturing of an active (powered) dosimeter system to measure astronaut's exposures, support risk assessment dose management by providing a differentiated data set. Final goal is the verification of the system capabilities for medical monitoring at highest standards. The EuCPAD consists of several small portable Personal Active Dosimeters (MU = Mobile Unitas) and a rack mounted docking station “Personal Storage Device (PSD)” for MU storage, data read out and telemetry. The PSD furthermore contains a Tissue Equivalent Proportional Counter (TEPC) and an internal MU(iMU) to enable complex environmental measurements and cross calibrations. This presentation will give an introduction to the dosimetry system and of the current status. The EuCPAD project is carried out under ESA Contract No. 4200023059/09/NL/CP, Title: 10Be Production in the Atmosphere by Galactic Cosmic Rays Authors: Matthiä, Daniel; Herbst, Klaudia; Heber, Bernd; Berger, Thomas; Reitz, Günther Bibcode: 2014crh..book..333M Altcode: No abstract at ADS Title: GRB 141221A: Skynet PROMPT-CTIO observations of the optical afterglow. Authors: Trotter, A.; Haislip, J.; Reichart, D.; Aji, A.; Beauchemin, R.; Berger, T.; Dow, A.; Foster, A.; Frank, N.; Hinckle, M.; Ivarsen, K.; Lacluyze, A.; Maples, M.; Moore, J.; Nysewander, M.; Salemi, C.; Zbinden, L.; Crain, J. A. Bibcode: 2014GCN.17210....1T Altcode: 2014GCN..17210...1T No abstract at ADS Title: Dose Measurements on the BION-M1 satellite applying passive detector packages Authors: Stradi, Andrea; Berger, Thomas; Kodaira, Satoshi; Kubancak, Jan; Palfalvi, Jozsef K.; Ambrozova, Iva; Tolochek, Raisa; Shurshakov, Vyacheslav; Szabo, Julianna Bibcode: 2014cosp...40E3214S Altcode: A passive detector package was developed in the past years in the Centre for Energy Research, Hungarian Academy of Science to detect cosmic ray particles, to determine their flux and dose. It consists of thermoluminescent detectors (TLD) and plastic solid state nuclear track detectors (SSNTD). In the frame of a scientific co-operation between the Institute for Biomedical Problems (IBMP) fourteen packages were flow within the new BION-M1 satellite program together with biological samples and detector packages from other participants. Two packages were located outside and the rest ones inside the recoverable capsule. Comparing to the previous BION and similar FOTON experiments, (all together 17 successful ones), this flight was a “champion” with the highest altitude (575 km), orbital inclination (64.9°) and flight duration (30 days). The external exposure provided a unique possibility to study not only the elevated level of cosmic rays but also the behavior of the detector packages in extreme circumstances as low temperature and pressure. The paper will summarize the construction of the detector packages, the calibration and evaluation processes, as well as, the linear energy transfer (LET) spectra, the absorbed dose and the mean quality factor. These quantities will be compared taking into consideration their location inside and outside the capsule and to the results of other participants. Also some comparison of results to the previous BION and FOTON flights and contemporary measurements on the ISS will be presented. Title: GRB 140301A: skynet R-COP observations. Authors: Trotter, A.; Haislip, J.; Lacluyze, A.; Reichart, D.; Verveer, A.; Spuck, T.; Foster, A.; Frank, N.; Ivarsen, K.; Moore, J.; Nysewander, M.; Beauchemin, R.; Berger, T.; Carroll, M.; Cromartie, H. T.; Egger, R.; Hinckle, M.; Ireland, A.; Maples, M.; Scott, L.; Crain, J. A. Bibcode: 2014GCN.15897....1T Altcode: 2014GCN..15897...1T No abstract at ADS Title: Future Diagnostic Capabilities: The 4-meter Daniel K. Inouye Solar Telescope Authors: Berger, Thomas; Reardon, Kevin; Elmore, David; Woeger, Friedrich; Tritschler, Alexandra; Rimmele, Thomas Bibcode: 2014cosp...40E.294B Altcode: We discuss the observational capabilities of the Daniel K. Inouye Solar Telescope (DKSIT), formerly known as the Advanced Technology Solar Telescope (ATST), currently under construction on Haleakala Mountain on the island of Maui, Hawaii, with first light anticipated in mid-2019. The DKIST will be a 4-meter aperture Gregorian telescope with advanced environmental control and adaptive optics capable of producing diffraction-limited resolution in visible light of 0.03" or about 20 km in the solar photosphere. The first light instrument suite will include the Visible Broadband Imager (VBI), an interference filter-based instrument capable of 30 Hz imaging of photospheric and chromospheric magnetic structures in the 380 to 800 nm wavelength range. All VBI images will be reconstructed in near-real-time using the KISIP speckle reconstruction algorithm adapted to the DKIST optical and AO configuration. The Visible Spectropolarimeter (ViSP) instrument being fabricated by the High Altitude Observatory (HAO) will enable high-precision slit-spectropolarimetery in any three spectral regions from 380 to 900 nm. The ViSP instrument will be the highest precision spectropolarimeter ever produced with a spatial resolution of approximately 40 km at 600 nm and temporal resolution of 10s to achieve 1e-03 polarimetric precision. The Visible Tunable Filter (VTF) instrument under fabrication at the Kiepenheuer Institute for Solar Physics (KIS) is a triple-etalon Fabry-Perot imaging spectropolarimeter instrument capable of diffraction limited measurements of the Fe I 630.2 nm and Ca II 854.2 nm spectral lines for Doppler and magnetic measurements in the photosphere and chromosphere, respectively. The VTF will also enable the highest spatial and temporal resolution observations yet achieved in the H-alpha line for detailed studies of chromospheric dynamics in response to photospheric magnetic drivers. The Diffraction-Limited Near-IR Spectropolarimeter (DL-NiRSP) and the Cryogenic Near-IR Spectropolarimeter (Cryo-NiRSP) instruments, both under fabrication at the University of Hawaii, will enable polarimetric and spectroscopic investigations in the largely unexplored infra-red spectral region. The DL-NiRSP will span 900 nm to 2.5 microns in wavelength and include a novel fiber-optic "Integral Field Unit" (IFU) for true imaging spectropolarimetry in three simultaneous spectral regions over a variable field of view. This instrument will enable revolutionary measurements of prominence magnetic fields and will also, in the wider field mode, enable coronal polarimetric studies. The Cryo-NiRSP instrument spans the 1--5 micron wavelength range and will make near-diffraction limited 0.3" resolution slit-scan measurements of the coronal magnetic field out to 1.3 solar radii with temporal resolution measured in minutes. The DKIST facility will undergo extensive polarimetric calibration to ensure that the ultimate goal of 5e-04 polarimetic precision is obtainable under the best conditions. All of the data from the DKIST will be transmitted to the central DKIST data center in Boulder, Colorado where automated reduction and calibration pipelines will rapidly provide the community with calibrated data products for use in science investigations. The DKIST will also be operated in a "Service Mode" access model in which investigators will not be required to travel to the telescope to accomplish their science observations. Title: GRB 140518A: Skynet GORT Detections of the Optical Afterglow. Authors: Trotter, A.; Lacluyze, A.; Haislip, J.; Reichart, D.; McLin, K.; Cominsky, L.; Cromartie, H. T.; Foster, A.; Frank, N.; Ivarsen, K.; Maples, M.; Moore, J.; Nysewander, M.; Beauchemin, R.; Berger, T.; Dow, A.; Hinckle, M.; Patterson, A.; Pegues, H.; Pozo, J.; Waddell, D.; Crain, J. A. Bibcode: 2014GCN.16304....1T Altcode: 2014GCN..16304...1T No abstract at ADS Title: Solar Prominence Fine Structure and Dynamics Authors: Berger, Thomas Bibcode: 2014IAUS..300...15B Altcode: We review recent observational and theoretical results on the fine structure and dynamics of solar prominences, beginning with an overview of prominence classifications, the proposal of possible new ``funnel prominence'' classification, and a discussion of the recent ``solar tornado'' findings. We then focus on quiescent prominences to review formation, down-flow dynamics, and the ``prominence bubble'' phenomena. We show new observations of the prominence bubble Rayleigh-Taylor instability triggered by a Kelvin-Helmholtz shear flow instability occurring along the bubble boundary. Finally we review recent studies on plasma composition of bubbles, emphasizing that differential emission measure (DEM) analysis offers a more quantitative analysis than photometric comparisons. In conclusion, we discuss the relation of prominences to coronal magnetic flux ropes, proposing that prominences can be understood as partially ionized condensations of plasma forming the return flow of a general magneto-thermal convection in the corona. Title: Development of a New Radiation Sensor for Satellite Missions Authors: Ritter, Birgit; Berger, Thomas; Reitz, Guenther; Hauslage, Jens; Marsalek, Karel; Aeckerlein, Joachim; M, Hartmut Bibcode: 2014cosp...40E2748R Altcode: The RAMIS (RAdiation Measurements In Space) experiment aims to measure cosmic radiation with energy deposition ranging from minimal ionizing protons up to relativistic iron nuclei. The radiation detector principle uses two silicon detectors, each with an active area of 0.5cm² that are arranged in a telescope configuration. The experiment will fly in 2016 on the first mission of the newly developed DLR (German Aerospace Center) Compact Satellite, which intends to provide an easy accessible platform for scientific research within DLR as well as for international partners and their experiments. As the satellite will orbit Earth at an altitude of about 600 km on a polar orbit, valuable insights are gained not only in the galactic cosmic ray (GCR) component of the radiation field and in solar energetic particles (SEPs) in case of solar events. Also the trapped radiation in the horns of the electron belts around Earth can be studied in detail. Particle fluxes will be monitored and energy deposition spectra recorded from which linear energy transfer spectra will be generated. These spectra give an estimate for the quality of the radiation field. The RAMIS experiment consists of two modules, i.e. two small silicon detector telescopes, with one module being located outside on top of the satellite, while the other one is placed inside next to the primary payload of the satellite, the Eu:CROPIS experiment. Eu:CROPIS is a combined self-sustained biological life support system under Moon and Mars gravity, which uses Euglena as oxygen suppliers, biofilter for wastewater treatment and detoxification, and urine as primary fertilizer. In addition to its scientific output RAMIS will provide dosimetric monitoring for Eu:CROPIS and serve as a radiation exposure information system for the satellite bus. Furthermore the obtained data can be used for benchmarking and improvement of radiation belt models as well as of shielding models by combining the results of both modules. The RAMIS experiment, the prototype performance and first test measurements of the detector system will be presented. Title: Long term dose monitoring onboard the European Columbus module of the International Space Station (ISS) in the frame of the DOSIS and DOSIS 3D project Authors: Berger, Thomas Bibcode: 2014cosp...40E.292B Altcode: The radiation environment encountered in space differs in nature from that on earth, consisting mostly of high energetic ions from protons up to iron, resulting in radiation levels far exceeding the ones present on earth for occupational radiation workers. Accurate knowledge of the physical characteristics of the space radiation field in dependence on the solar activity, the orbital parameters and the different shielding configurations of the International Space Station (ISS) is therefore needed. For the investigation of the spatial and temporal distribution of the radiation field inside the European Columbus module the experiment “Dose Distribution Inside the ISS” (DOSIS), under the project and science lead of the German Aerospace Center (DLR), was launched on July 15th 2009 with STS-127 to the ISS. The DOSIS experiment consists of a combination of “Passive Detector Packages” (PDP) distributed at eleven locations inside Columbus for the measurement of the spatial variation of the radiation field and two active Dosimetry Telescopes (DOSTELs) with a Data and Power Unit (DDPU) in a dedicated nomex pouch mounted at a fixed location beneath the European Physiology Module rack (EPM) for the measurement of the temporal variation of the radiation field parameters. The DOSIS experiment suite measured during the lowest solar minimum conditions in the space age from July 2009 to June 2011. In July 2011 the active hardware was transferred to ground for refurbishment and preparation for the follow up DOSIS 3D experiment. The hardware for DOSIS 3D was launched with Soyuz 30S to the ISS on May 15th 2012. The PDPs are replaced with each even number Soyuz flight starting with Soyuz 30S. Data from the active detectors is transferred to ground via the EPM rack which is activated once a month for this action. The presentation will give an overview of the DOSIS and DOSIS 3D experiment and focus on the results from the passive radiation detectors from the DOSIS 3D experiment (2012 - 2014) in comparison to the data of the DOSIS experiment (2009 - 2011). The Polish contribution was supported by the National Science Centre (No DEC-2012/06/M/ST9/00423). The CAU contributions to DOSIS and DOSIS 3D are financially supported by BMWi under Grants 50WB0826, 50WB1026 and 50WB1232. Title: GRB 141221A: Continued Skynet PROMPT-CTIO observations. Authors: Trotter, A.; Haislip, J.; Reichart, D.; Aji, A.; Beauchemin, R.; Berger, T.; Dow, A.; Foster, A.; Frank, N.; Hinckle, M.; Ivarsen, K.; Lacluyze, A.; Maples, M.; Moore, J.; Nysewander, M.; Salemi, C.; Zbinden, L.; Crain, J. A. Bibcode: 2014GCN.17221....1T Altcode: 2014GCN..17221...1T No abstract at ADS Title: GRB 141031A: Skynet PROMPT-CTIO Observations. Authors: Trotter, A.; Haislip, J.; Reichart, D.; Aji, A.; Beauchemin, R.; Berger, T.; Dow, A.; Foster, A.; Frank, N.; Hinckle, M.; Ivarsen, K.; Lacluyze, A.; Maples, M.; Moore, J.; Nysewander, M.; Salemi, C.; Zbinden, L.; Crain, J. A. Bibcode: 2014GCN.17004....1T Altcode: 2014GCN..17004...1T No abstract at ADS Title: GRB140215A: skynet PROMPT optical observations. Authors: Lacluyze, A.; Haislip, J.; Reichart, D.; Trotter, A.; Foster, A.; Frank, N.; Ivarsen, K.; Moore, J.; Nysewander, M.; Beauchemin, R.; Berger, T.; Carroll, M.; Cromartie, H. T.; Egger, R.; Hinckle, M.; Ireland, A.; Maples, M.; Scott, L.; Crain, J. A. Bibcode: 2014GCN.15840....1L Altcode: 2014GCN..15840...1L No abstract at ADS Title: Correction: MAXI J1421-613: skynet PROMPT/R-COP observations. Authors: Trotter, A.; Reichart, D.; Verveer, A.; Spuck, T.; Lacluyze, A.; Haislip, J.; Foster, A.; Frank, N.; Ivarsen, K.; Moore, J.; Nysewander, M.; Beauchemin, R.; Berger, T.; Carroll, M.; Cromartie, H. T.; Egger, R.; Hinckle, M.; Ireland, A.; Maples, M.; Scott, L.; Crain, J. A.; Baumgartner, W. H. Bibcode: 2014GCN.15755....1T Altcode: 2014GCN..15755...1T No abstract at ADS Title: GRB 141022A: Skynet PROMPT-CTIO Observations. Authors: Trotter, A.; Haislip, J.; Reichart, D.; Aji, A.; Beauchemin, R.; Berger, T.; Dow, A.; Foster, A.; Frank, N.; Hinckle, M.; Ivarsen, K.; Lacluyze, A.; Maples, M.; Moore, J.; Nysewander, M.; Salemi, C.; Zbinden, L.; Crain, J. A. Bibcode: 2014GCN.17023....1T Altcode: 2014GCN..17023...1T No abstract at ADS Title: GRB 140213A: continued skynet R-COP/PROMPT detections of a rebrightening optical afterglow. Authors: Trotter, A.; Haislip, J.; Reichart, D.; Lacluyze, A.; Verveer, A.; Spuck, T.; Foster, A.; Frank, N.; Ivarsen, K.; Moore, J.; Nysewander, M.; Beauchemin, R.; Berger, T.; Carroll, M.; Cromartie, H. T.; Egger, R.; Hinckle, M.; Ireland, A.; Maples, M.; Scott, L.; Crain, J. A. Bibcode: 2014GCN.15859....1T Altcode: 2014GCN..15859...1T No abstract at ADS Title: GRB 141212A: Skynet R-COP Observations. Authors: Trotter, A.; Haislip, J.; Reichart, D.; Verveer, A.; Spuck, T.; Aji, A.; Beauchemin, R.; Berger, T.; Dow, A.; Foster, A.; Frank, N.; Hinckle, M.; Ivarsen, K.; Lacluyze, A.; Maples, M.; Moore, J.; Nysewander, M.; Salemi, C.; Zbinden, L.; Crain, J. A. Bibcode: 2014GCN.17161....1T Altcode: 2014GCN..17161...1T No abstract at ADS Title: GRB 141017A: Skynet PROMPT-CTIO/SSO Observations. Authors: Trotter, A.; Haislip, J.; Reichart, D.; Aji, A.; Beauchemin, R.; Berger, T.; Dow, A.; Foster, A.; Frank, N.; Hinckle, M.; Ivarsen, K.; Lacluyze, A.; Maples, M.; Moore, J.; Nysewander, M.; Salemi, C.; Zbinden, L.; Crain, J. A. Bibcode: 2014GCN.17028....1T Altcode: 2014GCN..17028...1T No abstract at ADS Title: GRB 140118A/MAXI J1421-613: skynet PROMPT/R-COP observations. Authors: Trotter, A.; Reichart, D.; Verveer, A.; Spuck, T.; Lacluyze, A.; Haislip, J.; Foster, A.; Frank, N.; Ivarsen, K.; Moore, J.; Nysewander, M.; Beauchemin, R.; Berger, T.; Carroll, M.; Cromartie, H. T.; Egger, R.; Hinckle, M.; Ireland, A.; Maples, M.; Scott, L.; Crain, J. A. Bibcode: 2014GCN.15753....1T Altcode: 2014GCN..15753...1T No abstract at ADS Title: GRB 140213A: continued skynet R-COP/PROMPT observations of the optical afterglow. Authors: Trotter, A.; Haislip, J.; Reichart, D.; Lacluyze, A.; Verveer, A.; Spuck, T.; Foster, A.; Frank, N.; Ivarsen, K.; Moore, J.; Nysewander, M.; Beauchemin, R.; Berger, T.; Carroll, M.; Cromartie, H. T.; Egger, R.; Hinckle, M.; Ireland, A.; Maples, M.; Scott, L.; Crain, J. A. Bibcode: 2014GCN.15862....1T Altcode: 2014GCN..15862...1T No abstract at ADS Title: GRB 140213A: skynet R-COP detection of optical afterglow. Authors: Trotter, A.; Haislip, J.; Reichart, D.; Lacluyze, A.; Verveer, A.; Spuck, T.; Foster, A.; Frank, N.; Ivarsen, K.; Moore, J.; Nysewander, M.; Beauchemin, R.; Berger, T.; Carroll, M.; Cromartie, H. T.; Egger, R.; Hinckle, M.; Ireland, A.; Maples, M.; Scott, L.; Crain, J. A. Bibcode: 2014GCN.15828....1T Altcode: 2014GCN..15828...1T No abstract at ADS Title: Long term dose monitoring onboard the European Columbus module of the international space station (ISS) in the frame of DOSIS and DOSIS 3D project - results from the active instruments Authors: Burmeister, Soenke; Berger, Thomas; Reitz, Guenther; Boehme, Matthias; Haumann, Lutz; Labrenz, Johannes Bibcode: 2014cosp...40E.434B Altcode: Besides the effects of the microgravity environment, and the psychological and psychosocial problems encountered in confined spaces, radiation is the main health detriment for long duration human space missions. The radiation environment encountered in space differs in nature from that on earth, consisting mostly of high energetic ions from protons up to iron, resulting in radiation levels far exceeding the ones encountered on earth for occupational radiation workers. Accurate knowledge of the physical characteristics of the space radiation field in dependence on the solar activity, the orbital parameters and the different shielding configurations of the International Space Station ISS is therefore needed. For the investigation of the spatial and temporal distribution of the radiation field inside the European COLUMBUS module the experiment DOSIS (Dose Distribution Inside the ISS) under the lead of DLR has been launched on July 15 (th) 2009 with STS-127 to the ISS. The experimental package was transferred from the Space Shuttle into COLUMBUS on July 18 (th) . It consists of a combination of passive detector packages (PDP) distributed at 11 locations inside the European Columbus Laboratory and two active radiation detectors (Dosimetry Telescopes = DOSTELs) with a DDPU (DOSTEL Data and Power Unit) in a Nomex pouch (DOSIS MAIN BOX) mounted at a fixed location beneath the European Physiology Module rack (EPM) inside COLUMBUS. The active components of the DOSIS experiment were operational from July 18 (th) 2009 to June 16 (th) 2011. After refurbishment the hardware has been reactivated on May 15 (th) 2012 as active part of the DOSIS 3D experiment and provides continuous data since this activation. The presentation will focus on the latest results from the two DOSTEL instruments as absorbed dose, dose equivalent and the related LET spectra gathered within the DOSIS (2009 - 2011) and DOSIS 3D (2012 - 2014) experiment. The CAU contributions to DOSIS and DOSIS 3D are financially supported by BMWi under Grants 50WB0826, 50WB1026 and 50WB1232 Title: Coronal Condensation in Funnel Prominences as Return Flows of the Chromosphere-Corona Mass Cycle Authors: Liu, Wei; Berger, Thomas E.; Low, B. C. Bibcode: 2014IAUS..300..441L Altcode: We present SDO/AIA observations of a potentially novel type of prominence, called ``funnel prominence'', that forms out of coronal condensation at magnetic dips. They can drain a large amount of mass (up to ~1015 g day-1) and may play an important role as return flows of the chromosphere-corona mass cycle. Title: Preparation of the Biochip experiment on the EXPOSE-R2 mission outside the International Space Station Authors: Vigier, F.; Le Postollec, A.; Coussot, G.; Chaput, D.; Cottin, H.; Berger, T.; Incerti, S.; Triqueneaux, S.; Dobrijevic, M.; Vandenabeele-Trambouze, O. Bibcode: 2013AdSpR..52.2168V Altcode: Biochips might be suited for planetary exploration. Indeed, they present great potential for the search for biomarkers - molecules that are the sign of past or present life in space - thanks to their size (miniaturized devices) and sensitivity. Their detection principle is based on the recognition of a target molecule by affinity receptors fixed on a solid surface. Consequently, one of the main concerns when developing such a system is the behavior of the biological receptors in a space environment. In this paper, we describe the preparation of an experiment planned to be part of the EXPOSE-R2 mission, which will be conducted on the EXPOSE-R facility, outside the International Space Station (ISS), in order to study the resistance of biochip models to space constraints (especially cosmic radiation and thermal cycling). This experiment overcomes the limits of ground tests which do not reproduce exactly the space parameters. Indeed, contrary to ground experiments where constraints are applied individually and in a limited time, the biochip models on the ISS will be exposed to cumulated constraints during several months. Finally, this ISS experiment is a necessary step towards planetary exploration as it will help assessing whether a biochip can be used for future exploration missions. Title: Estimation of Galactic Cosmic Ray exposure inside and outside the Earth's magnetosphere during the recent solar minimum between solar cycles 23 and 24 Authors: Mrigakshi, Alankrita Isha; Matthiä, Daniel; Berger, Thomas; Reitz, Günther; Wimmer-Schweingruber, Robert F. Bibcode: 2013AdSpR..52..979M Altcode: The evidently low solar activity observed between solar cycles 23 and 24 during the years 2008-2010 led to a substantial increase in the Galactic Cosmic Ray (GCR) intensity in comparison with preceding solar minima. As the GCRs consist of highly-ionizing charged particles having the potential to cause biological damage, they are a subject of concern for manned missions to space. With the enhanced particle fluxes observed between 2008 and 2010, it is reasonable to assume that the radiation exposure from GCR must have also increased to unusually high levels. In this paper, the GCR exposure outside and inside the Earth's magnetosphere is numerically calculated for time periods starting from 1970 to the end of 2011 in order to investigate the increase in dose levels during the years 2008-2010 in comparison with the last three solar minima. The dose rates were calculated in a water sphere, used as a surrogate for the human body, either unshielded or surrounded by aluminium shielding of 0.3, 10 or 40 g/cm2. By performing such a long-term analysis, it was estimated that the GCR exposure during the recent solar minimum was indeed the largest in comparison with previous minima and that the increase was more pronounced for locations outside the magnetosphere. Title: Organ shielding and doses in Low-Earth orbit calculated for spherical and anthropomorphic phantoms Authors: Matthiä, Daniel; Berger, Thomas; Reitz, Günther Bibcode: 2013AdSpR..52..528M Altcode: Humans in space are exposed to elevated levels of radiation compared to ground. Different sources contribute to the total exposure with galactic cosmic rays being the most important component. The application of numerical and anthropomorphic phantoms in simulations allows the estimation of dose rates from galactic cosmic rays in individual organs and whole body quantities such as the effective dose. The male and female reference phantoms defined by the International Commission on Radiological Protection and the hermaphrodite numerical RANDO phantom are voxel implementations of anthropomorphic phantoms and contain all organs relevant for radiation risk assessment. These anthropomorphic phantoms together with a spherical water phantom were used in this work to translate the mean shielding of organs in the different anthropomorphic voxel phantoms into positions in the spherical phantom. This relation allows using a water sphere as surrogate for the anthropomorphic phantoms in both simulations and measurements. Moreover, using spherical phantoms in the calculation of radiation exposure offers great advantages over anthropomorphic phantoms in terms of computational time. In this work, the mean shielding of organs in the different voxel phantoms exposed to isotropic irradiation is presented as well as the corresponding depth in a water sphere. Dose rates for Low-Earth orbit from galactic cosmic rays during solar minimum conditions were calculated using the different phantoms and are compared to the results for a spherical water phantom in combination with the mean organ shielding. For the spherical water phantom the impact of different aluminium shielding between 1 g/cm2 and 100 g/cm2 was calculated. The dose equivalent rates were used to estimate the effective dose rate. Title: The Advanced Technology Solar Telescope Construction Status Report Authors: McMullin, Joseph P.; Rimmele, T. R.; Warner, M.; Berger, T.; Keil, S. L. Bibcode: 2013SPD....4440001M Altcode: The Advanced Technology Solar Telescope (ATST) will provide observing capabilities in the visible through infrared wavelengths with unprecedented resolution and sensitivity. Designed to study solar magnetism that controls the solar wind, flares, CMEs and variability in the Sun's output, the ATST will be capable of detecting and spatially resolving the fundamental astrophysical processes at their intrinsic scales throughout the solar atmosphere. The 4-m class facility is currently under construction in Maui, HI on the Haleakala Observatories site with a scheduled completion of July 2019. Since the start of site construction in December of 2012, significant progress has been made toward the development of the observatory buildings (excavation, foundations, working towards the steel erection). In addition, off-site, the major subsystems of the telescope have been contracted, designs are complete and fabrication is underway. We review the science drivers, design details, technical challenges, and provide a construction status update on the subsystems and their integration. Title: The ATST Instrumentation suite: capabilities, synergies, and science goals Authors: Berger, Thomas; ATST Science Team Bibcode: 2013SPD....4440002B Altcode: The ATST will have a full complement of first generation instrumentation to cover observations of the solar atmosphere from the photosphere to the corona: the Visible Broadband Imager (VBI) will be an interference filter imager providing the highest spatial and temporal resolution image sequences for ATST, spanning from the deep photosphere through the chromosphere, and perhaps providing coronal imaging as well; the Visible Spectropolarimeter (ViSP) will be an advanced slit spectropolarimeter enabling simultaneous multi-line spectropolarimetry from 380 to 900 nm; the Visible Tunable Filter (VTF) will be a dual tunable Fabry-Perot system enabling rapid cadence spectral imaging and spectropolarimetry in the 520 to 870 nm range; the Diffraction-limited Near-IR Spectropolarimeter (DL-NiRSP) will be an advanced fiber-optic image plane spectropolarimeter offering simultaneous imaging and full-profile spectropolarimetry from 900 to 2500 nm; and the Cryogenic Near-IR Spectropolarimeter (Cryo-NiRSP) will provide coronal slit spectropolarimetry from 1--5 microns. We will review the science capabilities of these first generation instruments as well as their synergistic use in multi-instrument observing programs to achieve novel science investigations. Title: Funnel Prominences as Return Flows of the Chromosphere-Corona Mass Cycle: SDO/AIA Observations of Coronal Condensation Authors: Liu, Wei; Berger, T.; Low, B. C. Bibcode: 2013SPD....44...42L Altcode: It has recently been proposed that prominences play an important role as return flows of the chromosphere-corona mass cycle, in which hot plasma is transported upward in forms of spicules and prominence bubbles (likely due to flux emergence), while cool plasma drains downward in forms of vertical prominence threads (Berger et al. 2011 Nature). A critical step in this cycle is the condensation of the million-degree coronal plasma into T<10,000 K prominence material by a radiative cooling instability (i.e., thermal non-equilibrium), as numerically simulated (Karpen & Antiochos 2008; Xia et al. 2012) and first evidenced in recent SDO/AIA observations (Liu et al. 2012; Berger et al. 2012 ApJL). Such a runaway cooling process occurs in coronal loops of various sizes and generally leads to condensation at magnetic dips and formation of funnel-shaped prominences. A moderate-sized prominence can drain a significant mass of typically 10^15 gram/day, which is comparable to the mass of a CME or a fraction of the entire corona. Here we present a survey of funnel prominences that appear to be common in AIA observations at various locations and times. We find longer cooling times in longer/taller coronal loops whose densities are lower, consistent with the expected quadratic dependence on density of the optically-thin radiative loss. We propose that such funnel prominences, usually small in size, can constitute a new type of prominences, and similar processes can produce elementary building blocks of large-scale quiescent prominences in filament channels. This picture is supported by the recent theoretical development on spontaneous formation of current sheets and condensations manifested as prominence threads (Low et al. 2012a, b, ApJ).Abstract (2,250 Maximum Characters): It has recently been proposed that prominences play an important role as return flows of the chromosphere-corona mass cycle, in which hot plasma is transported upward in forms of spicules and prominence bubbles (likely due to flux emergence), while cool plasma drains downward in forms of vertical prominence threads (Berger et al. 2011 Nature). A critical step in this cycle is the condensation of the million-degree coronal plasma into T<10,000 K prominence material by a radiative cooling instability (i.e., thermal non-equilibrium), as numerically simulated (Karpen & Antiochos 2008; Xia et al. 2012) and first evidenced in recent SDO/AIA observations (Liu et al. 2012; Berger et al. 2012 ApJL). Such a runaway cooling process occurs in coronal loops of various sizes and generally leads to condensation at magnetic dips and formation of funnel-shaped prominences. A moderate-sized prominence can drain a significant mass of typically 10^15 gram/day, which is comparable to the mass of a CME or a fraction of the entire corona. Here we present a survey of funnel prominences that appear to be common in AIA observations at various locations and times. We find longer cooling times in longer/taller coronal loops whose densities are lower, consistent with the expected quadratic dependence on density of the optically-thin radiative loss. We propose that such funnel prominences, usually small in size, can constitute a new type of prominences, and similar processes can produce elementary building blocks of large-scale quiescent prominences in filament channels. This picture is supported by the recent theoretical development on spontaneous formation of current sheets and condensations manifested as prominence threads (Low et al. 2012a, b, ApJ). Title: 10Be Production in the Atmosphere by Galactic Cosmic Rays Authors: Matthiä, Daniel; Herbst, Klaudia; Heber, Bernd; Berger, Thomas; Reitz, Günther Bibcode: 2013SSRv..176..333M Altcode: 2011SSRv..tmp..290M Galactic cosmic ray nuclei and energetic protons produced in solar flares and accelerated by coronal mass ejections are the main sources of high-energy particles of extraterrestrial origin in near-Earth space and inside the Earth's atmosphere. The intensity of galactic cosmic rays inside the heliosphere is strongly influenced by the modulation of the interstellar source particles on their way through interplanetary space. Among others, this modulation depends on the activity of the Sun, and the resulting intensity of the energetic particles in the atmosphere is an indicator of the solar activity. Therefore, rare isotopes found in historical archives and produced by spallation reactions of primary and secondary hadrons of cosmic origin in the atmosphere, so-called cosmogenic nuclides, can be used to reconstruct the solar activity in the past. The production rate of 10Be, one of the cosmogenic nuclides most adequate to study the solar activity, is presented showing its variations with geographic latitude and altitude and the dependence on different production cross-sections present in literature. In addition, estimates for altitude integrated production rates of 10Be at different locations since the early nineteen sixties are shown. Title: The Advanced Technology Solar Telescope: Science Drivers and Construction Status Authors: Rimmele, Thomas; Berger, Thomas; McMullin, Joseph; Keil, Stephen; Goode, Phil; Knoelker, Michael; Kuhn, Jeff; Rosner, Robert; Casini, Roberto; Lin, Haosheng; Woeger, Friedrich; von der Luehe, Oskar; Tritschler, Alexandra; Atst Team Bibcode: 2013EGUGA..15.6305R Altcode: The 4-meter Advance Technology Solar Telescope (ATST) currently under construction on the 3000 meter peak of Haleakala on Maui, Hawaii will be the world's most powerful solar telescope and the leading ground-based resource for studying solar magnetism. The solar atmosphere is permeated by a 'magnetic carpet' that constantly reweaves itself to control solar irradiance and its effects on Earth's climate, the solar wind, and space weather phenomena such as flares and coronal mass ejections. Precise measurement of solar magnetic fields requires a large-aperture solar telescope capable of resolving a few tens of kilometers on the solar surface. With its 4 meter aperture, the ATST will for the first time resolve magnetic structure at the intrinsic scales of plasma convection and turbulence. The ATST's ability to perform accurate and precise spectroscopic and polarimetric measurements of magnetic fields in all layers of the solar atmosphere, including accurate mapping of the elusive coronal magnetic fields, will be transformative in advancing our understanding of the magnetic solar atmosphere. The ATST will utilize the Sun as an important astro- and plasma-physics "laboratory" demonstrating key aspects of omnipresent cosmic magnetic fields. The ATST construction effort is led by the US National Solar Observatory. State-of-the-art instrumentation will be constructed by US and international partner institutions. The technical challenges the ATST is facing are numerous and include the design of the off-axis main telescope, the development of a high order adaptive optics system that delivers a corrected beam to the instrument laboratory, effective handling of the solar heat load on optical and structural elements, and minimizing scattered light to enable observations of the faint corona. The ATST project has transitioned from design and development to its construction phase. The project has awarded design and fabrication contracts for major telescope subsystems. Site construction has commenced following the successful conclusion of the site permitting process. Science goals and construction status of telescope and instrument systems will be discussed. Title: Comparison of solar horizontal velocity fields from SDO/HMI and Hinode data Authors: Roudier, Th.; Rieutord, M.; Prat, V.; Malherbe, J. M.; Renon, N.; Frank, Z.; Švanda, M.; Berger, T.; Burston, R.; Gizon, L. Bibcode: 2013A&A...552A.113R Altcode: 2013arXiv1303.4271R Context. The measurement of the Sun's surface motions with a high spatial and temporal resolution is still a challenge.