Author name code: laming ADS astronomy entries on 2022-09-14 author:Laming, Martin ------------------------------------------------------------------------ Title: Powerful Diagnostics of Cosmic-Ray Modified Shock by Hα Polarimetry Authors: Shimoda, J.; Laming, M. Bibcode: 2022icrc.confE.140S Altcode: 2022PoS...395E.140S No abstract at ADS Title: The Origin of the Crab Nebula Authors: Temim, Tea; Blair, William P.; Drissen, Laurent; Fox, Ori Dosovitz; Laming, J. Martin; Lyutikov, Maxim; Martin, Thomas; Milisavljevic, Dan; Modjaz, Maryam; Rest, Armin; Sankrit, Ravi; Slane, Patrick; Smith, Nathan; Strolger, Louis-Gregory; Sukhbold, Tuguldur Bibcode: 2021jwst.prop.1714T Altcode: We propose NIRCam and MIRI imaging and MIRI MRS spectroscopy of the iconic Crab Nebula in order to test models of the progenitor and explosion mechanism by mapping the dust distribution, imaging the iron emission, measuring Ni/Fe ratios, and searching for dust compositional variations. The imaging requested will permit us to separate the bright line and synchrotron emission from dust emission and produce the first complete mapping of the dust distribution in the Crab Nebula. The [Fe II] emission will be used to study the spatial distribution of Fe in the remnant and derive its total mass. The MIRI MRS spectra will be used to measure the Ni/Fe ratios across the filaments and determine the dust composition at two positions that may have different ejecta and swept-up circumstellar contributions. These observational measurements can elucidate differences in predictions for the two competing explosion mechanisms for the Crab's progenitor (electron capture vs. Fe-core collapse) and determine whether a dense circumstellar medium, possibly distributed in a disk around the progenitor, has been important in shaping the Crab Nebula as it is observed today. The total requested time for the program is 22.57 hours. Title: Linking the Sun to the heliosphere using composition data and modelling: coronal jets as a test case Authors: Wimmer-Schweingruber, Robert F.; Parenti, Susanna; Del Zanna, G.; Edmondson, J.; Giunta, A.; Hansteen, V. H.; Higginson, A.; Lepri, S.; Laming, M.; Lynch, B. J.; von Steiger, R. E.; Wiegelmann, T.; Zambrana Prado, N. Bibcode: 2019shin.confE.231W Altcode: Understanding the formation and evolution of the solar wind is still a priority in the Solar and Heliospheric communities. We expect a significant progress in terms of observations with the upcoming Solar Orbiter mission (launch in 2020), which will provide detailed in-situ measurements of the solar wind and several remote-sensing observations. However, real progress will only be possible if we improve our understanding of the physical link between what measured in-situ and its source regions on the Sun. In this respect, the plasma chemical and charge-state compositions are considered good diagnostic tools. In this paper we present results obtained from an extensive team work aiming at providing solid diagnostics for linking the in-situ and the remote sensing measurements. For our test cases, we selected two periods when a single active region produced, close to its sunspot, jets which had a counterpart signature in the Heliosphere in the form of type-III radio bursts. These jets therefore marked magnetically open regions expanding in the heliosphere. Firstly, we looked for signatures of the open field associated with the active regions in in-situ data from ACE and WIND, finding potential tracers. Secondly, we studied the magnetic topology of the full Sun and Heliosphere with extrapolations of photospheric data and MHD modeling. We found that the open field area is consistent with the source and evolution of the jets, as observed with EUV imagers (SDO/AIA, STEREO/EUVI). Thirdly, we analysed remote sensing EUV spectroscopic observations to measure the plasma conditions (densities, temperatures and chemical composition) whenever available. We then modeled the solar wind and charge state evolution with the solar distance along the open fields to establish a link between the in-situ signatures and the remote sensing observations. We discuss the various difficulties associated with such studies, and highlight how Solar Orbiter measurements can improve them. Title: Exploring the Properties of Transverse Waves at the Base of the Solar Wind Authors: Weberg, Micah J.; Morton, Richard; McLaughlin, James; Laming, Martin; Ko, Yuan-Kuen Bibcode: 2019shin.confE.173W Altcode: Transverse (or ‘Alfvénic’) waves are commonly invoked by theories and models to explain coronal heating and solar wind acceleration. However, direct measurements are sparse and most of what we know is derived from indirect proxies for wave activity. In this study, we present a large, statistical study of transverse waves directly observed in coronal plumes between May 2010 and May 2019 by SDO / AIA. The data was processed using an automated version of the Northumbria University Wave Tracking Code (NUWT) and presents a detailed picture of wave properties at the base of the solar wind. We find that the bulk wave parameters within the time periods analysed are largely consistent over most of a solar cycle. However, there is some evidence for smaller-scale variations with height, latitude, and over time periods of a few years. We will also explore the possibility of frequency-dependant processes which may give limits on the height at which wave dissipation, and thereby solar wind acceleration, begins. Lastly, we will give estimates for the total energy flux contained in the waves and discuss how it compares to the energy required to accelerate the solar wind. Title: Element Abundances and Solar Wind Origins Authors: Laming, Martin Bibcode: 2019shin.confE..29L Altcode: We examine the different element abundances exhibited by the closed loop solar corona and the slow speed solar wind. Both are subject to the First Ionization Potential (FIP) Effect, the enhancement in coronal abundance of elements with FIP below 10 eV (e.g. Mg, Si, Fe) with respect to high FIP elements (e.g. O, Ne, Ar), but with subtle differences. Intermediate elements, S, P, and C, with FIP just above 10 eV, behave as high FIP elements in closed loops, but are fractionated more like low FIP elements in the solar wind. On the basis of FIP fractionation by the ponderomotive force in the chromosphere, we discuss fractionation scenarios where this difference might originate. Fractionation low in the chromosphere where hydrogen is neutral enhances the S, P and C abundances. This arises with nonresonant waves, which are ubiquitous in open field regions, and is also stronger with torsional Alfven waves, as opposed to shear (i.e. planar) waves. We discuss the bearing these findings have on models of interchange reconnection as the source of the slow speed solar wind. The outflowing solar wind must ultimately be a mixture of the plasma in the originally open and closed fields, and the proportions and degree of mixing should depend on details of the reconnection process. We also describe novel diagnostics in ultraviolet and extreme ultraviolet spectroscopy now available with these new insights, with the prospect of investigating slow speed solar wind origins and the contribution of interchange reconnection by remote sensing. Title: The Correlation Between The Enhanced Sulfur Abundance in Slow Solar Winds and The Magnetic Field Geometry of Their Source Regions Authors: Kuroda, Natsuha; Laming, Martin Bibcode: 2019shin.confE...9K Altcode: We present an examination of the First Ionization Potential (FIP) fractionation scenario by the ponderomotive force in the chromosphere by using observations from The Solar Wind Ion Composition Spectrometer (SWICS) on board The Advanced Composition Explorer (ACE). Based on the prediction of the ponderomotive force model by Laming et al. (2019) that the abundance enhancements of intermediate FIP elements, S, P, and C, in slow solar wind can be explained by the release of plasma from strong open fields, much stronger than those usually associated with fast wind source regions, we examine the possible correspondence between the enhanced fractionation of intermediate FIP elements in slow solar winds and the magnetic field strength of their source regions. We do so by surveying the extensive record of solar wind speeds and composition from the ACE mission, and investigating the magnetic feature on the Sun associated with the repeated sulfur abundance anomaly corresponding to the decrease in the solar wind speed, found over about four solar rotation cycles in the beginning of 2008. We also obtain rough profiles of the magnetic field strength at the source regions of these slow winds, estimate the fractionation values of various elements using the ponderomotive force model with the field profiles as inputs, and compare the results with the observed fractionation values." Title: On the Detection of Coronal Suprathermal Ions and their Role as Seeds for SEP Production Authors: Laming, Martin; Strachan, Leonard; Tun, Sam; Ko, Yuan-Kuen; Socker, Dennis; Brown, Charles; Provornikova, Elena; Moses, Dan Bibcode: 2016shin.confE...7L Altcode: We review the problem of understanding the variability in Solar Energetic Particle (SEP) events, wherein two ostensibly similar CMEs can have very different SEP characteristics. A number of lines of evidence suggest that the presence or absence of a population of suprathermal ions in the corona, known as seed particles, is the determining factor, and that monitoring this population could lead to forecasts of SEP events. We discuss an observational technique designed to solve this problem by detecting suprathermal seed particles as extended wings on spectral lines, and describe an experiment designed for a flight opportunity on the DoD Space Test Program, due for launch in 2019. Title: Waves at Oblique Shocks and the Highest Cosmic Ray Energies in Tychos SNR Authors: Laming, Martin Bibcode: 2015xrvw.confE..10L Altcode: We describe a new model for the stripes of synchrotron radiation seen in the remnant of Tychos supernova, in terms of Alfven wave generation by the Bell Instability, followed by reflection, refraction and damping at an oblique shock. Based on estimates for damping rates due to turbulent cascade and transit time damping, we estimate the dependence of the visibility of the stripes on the shock obliquity, and determine a maximum cosmic ray energy in Tychos SNR in the range 6 x 1014 - 1 x 1015 eV, close to the knee in the cosmic ray spectrum. With such an understanding, synchrotron stripes ought in principle to be more commonly seen in SNRs, and should constitute a prime science topic for any future X-ray astronomy observatory. Title: X-ray Surveyor Discussion Session Results from the X-ray Vision Workshop Authors: Allured, Ryan; Arenberg, Jonathan; Bogdan, Akos; Canning, Rebecca; Churazov, Eugene; Civano, Francesca; Clarke, Tracy; Corrales, Lia; Di Matteo, Tiziana; Elvis, Martin; Fabbiano, Giuseppina; Falcone, Abe; Garcia, Javier; Gaskin, Jessica; Goldman, Itzhak; Kargaltsev, Oleg; Klinger, Noel; Laming, Martin; McNamara, Brian; Markevitch, Maxim; Marshall, Herman; Mosquera, Ana; Mroczkowski, Anthony; Natarajan, Priyamvada; Nielsen, Joey; Nowak, Michael; Ozel, Feryal; Poppenhaeger, Katja; Porquet, Delphine; Randall, Scott; Schwartz, Daniel; Swartz, Douglas A.; Temim, Tea; Van Weeren, Reinout; Weisskopf, Martin; Zhuravleva, Irina; ZuHone, John A. Bibcode: 2015xrvw.confE...6A Altcode: This paper summarizes the results of a brainstorming session held during the X-ray Vision Workshop (Oct 6-8, 2015, Washington DC). The workshop was convened to discuss the scientific potential of the X-ray Surveyor mission. The X-ray Surveyor concept, which was defined by the Astrophysics Roadmap, is to effect a 100-fold gain in survey and spectroscopic capability over the Chandra X-ray Observatory, while at least matching Chandra’s sub-arcsecond imaging capability.
This paper is intended to inform interested scientists of the growing discussion in
our community and to solicit their input in the area of new science that a next
generation high-resolution X-ray Observatory may provide for astrophysics. This
paper is not an official document and is certainly not the definitive science case for an X-ray Surveyor mission. It is, instead, an early input to this discussion, which we hope will lead to a full reference white paper on the X-Ray Surveyor concept. Title: In search of the radio signatures on SEP-productive solar active regions Authors: Tun Beltran, Samuel D.; Laming, Martin Bibcode: 2015TESS....120322T Altcode: Solar active regions may produce a wide variety of transients in the meter-decameter wavelength range.Some of these bursts result from mildly relativistic electron beams traveling along closed (type I) or open (type III) magnetic field lines or from energized electrons trapped in coronal magnetic fields (IV). The energization of these electron populations may be achieved through magnetic field reconnection. Reconnection may also be the driver which creates populations of suprathermal electrons. These suprathermals are now viewed as a prerequisite for the efficient production of solar energetic particles through shock-driven acceleration. We here present work done towards deriving a radio indicator for levels of reconnection correlated with large SEP storms. Working mostly with data from the Nançay Radioheliograph, spatio-spectral analysis is carried out on SEP-rich AR and a control group that is not. We discuss the most promising candidates of the sought after signature. Title: MHD Turbulence and the FIP Effect Authors: Laming, Martin Bibcode: 2010APS..DPPPM0014L Altcode: 2010APS..DPPPM10014 The First Ionization Potential (FIP) Effect is the by now well known abundance anomaly in the solar corona and slow speed solar wind, where elements with FIP less than about 10 eV (e.g. Fe, Mg, Si) are enhanced in abundance by a factor of about 3-4. High FIP elements (e.g. C, O, Ar) are essentially unchanged, while the highest FIP element, He, is depleted by a factor of about 0.5. A similar, though reduced abundance anomaly is found in the fast speed solar wind, and in coronal holes. These element fractionations are best explained by the action of the ponderomotive force in the solar chromosphere, arising as Alfvén waves reflect from the strong density gradients. Chromospheric ions, but not neutrals, are preferentially accelerated upwards. I will describe some recent developments, including the parametric generation of slow mode waves by the Alfvén wave driver, that now allows both the enhancement of Fe, Mg, S, etc, and the depletion of He to occur simultaneously. Title: Analytic Approach to the Stability of Standing Accretion Shocks Authors: Laming, Martin Bibcode: 2008APS..APR10HE03L Altcode: We explore an analytic model of the accretion shock in the postbounce phase of a core-collapse supernova explosion. We find growing oscillations of the shock in the l=1 and 2 modes, in agreement with a variety of existing numerical simulations. For modest values of the ratio of the outer accretion shock to that of the inner boundary to the shocked flow, the instability appears to derive from the growth of trapped sound waves, whereas at higher values, postshock advection clearly plays a role. Thus, the model described here may relate to the different mechanisms of instability recently advocated by Blondin & Mezzacappa and by Foglizzo and collaborators. Title: A Mechanism for Electron-Proton Temperature Equilibration in Collisionless Shocks Authors: Ghavamian, Parviz; Laming, M.; Rakowski, C. E. Bibcode: 2007AAS...210.4101G Altcode: 2007BAAS...39..154G The analysis of Balmer-dominated optical spectra from non-radiative (adiabatic) SNRs has shown that the ratio of the electron to proton temperature at the blast wave is close to unity at shock speeds below 400 km/s, but declines sharply down to the the mass proportional value (1/1836) at shock speeds exceeding 2000 km/s. We propose a physical model for the heating of electrons and ions in non-cosmic ray dominated, strong shocks (> 400 km/s) wherein the electrons are heated by lower hybrid waves immediately ahead of the shock front. These waves arise naturally from the cosmic ray pressure gradient upstream from the shock. The model predicts a nearly constant level of electron heating over a wide range of shock speeds, resulting in an inverse square relationship between T(electon)/T(proton) and shock speed that is fully consistent with the observations. Title: Jets and Asymmetries in the Cas A SNR Authors: Laming, Martin Bibcode: 2006sgrb.confE..35L Altcode: In April-May 2004 the instruments on the Chandra X-ray observatory acquired an unprecedented deep integration of the Cassiopeia A supernova remnant, for a total of 1 million seconds. I will present the results of an initial analysis of the so-called "jet" regions of the remnants, and review analyses of earlier data from the Chandra archive, with a view to highlighting aspects of the explosion asymmetry that are visible today in the morphology and spectra of the remnant. In particular from x-ray spectroscopy, we can show that the "jets" are indeed associated with asymmetry of the explosion as opposed to asymmetry in the circumstellar medium, and start to place numbers on the various parameters involved. We also make initial inferences on asymmetries in the Fe/Si inner ejecta and their possible relation to the direction of the compact central object natal kick. Title: Supernova and Gamma-Ray Burst Remnants Authors: Chevalier, Roger; Hwang, Una; Laming, Martin Bibcode: 2006sgrb.confE....C Altcode: The connection between Supernovae and Gamma-Ray Bursts has provided insights to extend our understanding of both these phenomena beyond what was known from studying them separately. A unique window into the connections between the progenitors and mechanisms of supernova and gamma-ray burst explosions is provided by their remnants. This meeting brings together experts of the remnants of both Supernovae and Gamma-Ray Bursts to combine this collective knowledge and to foster productive communication between theorists and observers. Title: Electron Heating in the Solar Wind Authors: Laming, M. Bibcode: 2005AGUSMSP51B..06L Altcode: We report on progress in modeling the elevated charge states observed in the fast solar wind with respect to the coronal hole source region. Improvements include the incorporation of new atomic data for dielectronic recombination of L-shell ions in our modeling, following the recent work of Badnell and collaborators. A second issue considered will be that of magnetic field inhomogeneity (as opposed to plasma density inhomogeneity) as an agent of instability. High temperature ions gyrating in curved magnetic field produce local anisotropies in their velocity distribution function, which in turn are unstable to the generation of lower hybrid waves. These waves then damp by heating electrons, giving rise to the observed increase in ion charge state. Work supported by NASA LWS NNH05AA05i and by the NRL/ONR Solar Magnetism and the Earth's Environment 6.1 Research Option. Title: Instruments: ACIS - Science Highlights: Chandra Ms Observation of Cassiopeia A Authors: Hwang, Una; Laming, Martin Bibcode: 2005ChNew..12....7H Altcode: No abstract at ADS Title: The FIP effect is solved! Authors: Laming, M. Bibcode: 2004cosp...35.1145L Altcode: 2004cosp.meet.1145L We discuss a further development of models along the lines originally suggested by Schwadron, Fisk and Zurbuchen (1999). These authors considered wave heated coronal loops where waves penetrate to loop footpoints, heating ions but not neutrals. This gives rise to abundance enhancements in elements which are ionized in the chromosphere (i.e. low first ionization potential) over those which are neutral through the higher ion scale height. Due to the low energy density residing in waves which can resonate with ion gyrofrequencies, we consider the effect of nonresonant waves through the ponderomotive force they exert on ions. For a broad class of solutions, an upward ponderomotive force exists on ions, and for quite reasonable wave energy densities reproduces the observed solar FIP abundance enhancement very well. Varying wave energy density varies the FIP enhancement, and for certain special cases a downwards ponderomotive force on ions may occur. The possible application of this to the inverse FIP effect observed in highly active stellar coronae will be discussed. Work supported by NASA Grant NAG5-9105, NASA Contract S13783G and by the NRL/ONR Solar Magnetism and the Earth's Environment 6.1 Research Option. Title: Laser-plasma simulations of astrophysical phenomena and novel applications to semiconductor annealing Authors: Grun, J.; Laming, M.; Manka, C.; Donnelly, D. W.; Covington, B. C.; Fischer, R. P.; Velikovich, A.; Khokhlov, A. Bibcode: 2003LPB....21..529G Altcode: At the frontier of plasma physics and technology are applications of laser-generated plasmas to laboratory simulations of astrophysical phenomena and to industrial processing. This article presents work at the Naval Research Laboratory in both of these areas. We show how laser plasmas are used to measure a blast wave corrugation overstability important in astrophysics. Detailed atomic physics calculations of radiative cooling within the blast front are used to develop a criterion of the existence of the overstability and are used to explain the experimental results. The criterion depends on quantities such as element abundances, densities, temperatures, and blast wave velocities—quantities which can be measured spectroscopically—and therefore used to infer whether astrophysical blast wave nonuniformities are the result of this instability. In other experiments, high-velocity jets are formed in the laboratory using miniature hollow cones. Jets produced by these cones are used to study the physics of jets occurring in supernovae and in star-forming accretion disks. In industrial semiconductor processing, annealing, that is, removing crystal damage and electrically activating the semiconductor, is a critical step. Industrial annealing techniques most often utilize heat generated by an oven, flash lamps, or a low-power laser. During such heating dopants within the semiconductor lattice diffuse and spread. This degrades the performance of circuits in which the individual circuit elements are very close to each other. We are developing an annealing technique in which shock or sound waves generated by a laser plasma are used to anneal the semiconductor. We have demonstrated that the method works over small areas and that it does not lead to significant dopant diffusion. Title: EBIT diagnostics using X-ray spectra of highly ionized Ne Authors: Matranga, Marco; Barbera, Marco; Maggio, Antonio; Peres, Giovanni; Serio, Salvatore; Takács, Endre; Silver, Eric; Gillaspy, John; Schnopper, Herbert; Laming, Martin; Beeman, Jeff; Haller, Eugen; Madden, Norman Bibcode: 2003NIMPB.205..244M Altcode: We have carried out a detailed analysis of highly ionized neon spectra collected at the NIST EBIT using an NTD germanium X-ray microcalorimeter developed at the Harvard-Smithsonian Center for Astrophysics [Nucl. Instr. and Meth. A 444 (2000) 156]. Our attention was focused especially on the Ne IX He-like triplet to check electron density diagnostics through the intercombination/forbidden line ratio. We have investigated possible effects of the ion dynamics on the plasma emission line intensities, looking at the dependence of the count-rate and the charge state distribution on the electron beam energy and current. The temperature and spatial distribution of the neon ions, and hence the overlap between the electron beam and the ion cloud, depend on the electron beam operating parameters. The overlap affects the average electron density seen by the ions, and in turn the measured line ratio. These results underscore the value of future improved studies of the trapped ion dynamics, both for understanding the EBIT performance and for allowing experimenters to take full advantage of its potential for astrophysical plasma diagnostics. Title: A synoptic spectral study of Cassiopeia-A based on XMM-Newton and BeppoSax observations Authors: Bleeker, Johan; Vink, Jacco; van der Heyden, Kurt; Willingale, Dick; Kaastra, Jelle; Laming, Martin Bibcode: 2002astro.ph..2207B Altcode: In this paper we present recent image and spectral data of Cas-A obtained with XMM-Newton and BeppoSAX. Analysis of the hard X-ray continuum does not support an interpretation of the hard X-radiation as synchrotron emission produced in the primary shock, non-thermal Bremsstrahlung is a plausible alternative. Moreover, a recent 500 kilosecond deep observation of the hard X-ray continuum by BeppoSAX has revealed the positive detection of the 44Sc nuclear decay lines at 67.9 and 78.4 keV. Appropriate modelling of the hard X-ray continuum leads to an estimate of the initial 44Ti mass of (0.8-2.5)E-4 solar masses. We also present ionisation age, temperature, abundances maps. The observed elemental abundance ratio patterns can be reconciled best with a type Ib SNe, arising from a 60 solar mass progenitor (ZAMS) with high-mass-loss. The accurate modeling of the image-resolved emission line spectra has enabled us to derive reliable Doppler velocities for the bright Si-K, S-K, and Fe-K line complexes. Title: Galactic abundances: Report of working group 3 Authors: Klecker, B.; Bothmer, V.; Cummings, A. C.; George, J. S.; Keller, J. W.; Salerno, E.; Sofia, U. J.; Stone, E. C.; Thielemann, F. -K.; Wiedenbeck, M. E.; Buclin, F.; Christian, E. R.; Flückiger, E. O.; Hofer, M. Y.; Jones, F. C.; Kirilova, D.; Kunow, H.; Laming, M.; Tranquille, C.; Wenzel, K. -P. Bibcode: 2001AIPC..598..207K Altcode: 2001sgc..conf..207K We summarize the various methods and their limitations and strengths to derive galactic abundances from in-situ and remote-sensing measurements, both from ground-based observations and from instruments in space. Because galactic abundances evolve in time and space it is important to obtain information with a variety of different methods covering different regions from the Very Local Insterstellar Medium (VLISM) to the distant galaxy, and different times throughout the evolution of the galaxy. We discuss the study of the present-day VLISM with neutral gas, pickup ions, and Anomalous Cosmic Rays, the study of the local interstellar medium (ISM) at distances <1.5 kpc utilizing absorption line me asurements in H I clouds, and the study of galactic cosmic rays, sampling contemporary (~15 Myr) sources in the local ISM within a few kiloparsec of the solar system. Solar system abundances, derived from solar abundances and meteorite studies are discussed in several other chapters of this volume. They provide samples of matter from the ISM from the time of solar system format ion, about 4.5 Gyr ago. The evolution of galactic abundances on longer time scales is discussed in the context of nuclear synthesis in the various contributing stellar objects. . Title: Laboratory Astrophysics Survey Of Key X-Ray Diagnostic Lines Using A Microcalorimeter On An Electron Beam Ion Trap Authors: Silver, E.; Schnopper, H.; Bandler, S.; Brickhouse, N.; Murray, S.; Barbera, M.; Takacs, E.; Laming, M.; Kink, I.; Porto, J.; Gillaspy, J. D.; Deslattes, R.; Hudson, L.; Madden, N.; Landis, D.; Beeman, J.; Haller, E. E. Bibcode: 2000HEAD....5.4332S Altcode: 2000BAAS...32.1265S Cosmic plasma conditions created in an Electron Beam Ion Trap (EBIT) make it possible to simulate the dependencies of key diagnostic x-ray lines on density, temperature, and excitation conditions that exist in astrophysical sources. We used a microcalorimeter to measure broad band spectra obtained from the NIST EBIT with an energy resolution approaching that of a Bragg crystal spectrometer. Spectra are presented for nitrogen, oxygen, neon, argon , and iron in various stages of ionization. Title: Laboratory Astrophysics Survey Of Key X-Ray Diagnostic Lines Using A Microcalorimeter On An Electron Beam Ion Trap Authors: Silver, Eric; Schnopper, Herbert; Bandler, Simon; Brickhouse, Nancy; Murray, Stephen; Barbera, Marco; Takacs, Endre; Laming, Martin; Kink, Ilmar; Porto, Trey; Gillaspy, John; Deslattes, Richard; Hudson, Larry; Madden, Norm; Landis, Don; Beeman, Jeffrey; Haller, Eugene Bibcode: 2000APS..DPPWO2003S Altcode: Cosmic plasma conditions created in an Electron Beam Ion Trap (EBIT) make it possible to simulate the dependencies of key diagnostic x-ray lines on density, temperature, and excitation conditions that exist in astrophysical sources. We used a microcalorimeter to measure broad band spectra obtained from the NIST EBIT with an energy resolution approaching that of a Bragg crystal spectrometer. Spectra are presented for nitrogen, oxygen, neon, argon , and iron in various stages of ionization. Title: Laboratory Astrophysics Survey Of Key X-Ray Diagnostic Lines Using A Microcalorimeter On An Electron Beam Ion Trap Authors: Silver, Eric; Schnopper, Herbert; Bandler, Simon; Brickhouse, Nancy; Murray, Stephen; Barbera, Marco; Takacs, Endre; Gillaspy, John D.; Porto, Trey; Kink, Ilmar; Madden, Norm; Landis, Don; Beeman, Jeffrey; Haller, Eugene; Laming, Martin Bibcode: 2000APS..DMP..J602S Altcode: Cosmic plasma conditions created in an Electron Beam Ion Trap (EBIT) make it possible to simulate the dependencies of key diagnostic x-ray lines on density, temperature, and excitation conditions that exist in astrophysical sources. We used a microcalorimeter coupled with an x-ray optic to measure broad band spectra obtained from the NIST EBIT with an energy resolution approaching that of a Bragg crystal spectrometer. Spectra are presented for nitrogen, oxygen, neon, argon , and iron in various stages of ionization. Title: Spectroscopic Study of the Galactic Supernova Remnant RCW 86 Authors: Smith, R. Chris; Ghavamian, Parviz; Long, Knox S.; Hartigan, Pat; Raymond, John; Laming, Martin Bibcode: 1999noao.prop..350S Altcode: We propose to undertake a detailed study of the supernova remnant RCW 86 and its newly discovered Balmer-dominated filaments, involving low-resolution, moderate-resolution and high-resolution spectroscopic observations of both radiative and Balmer-dominated filaments. These observations provide estimates of the reddening, shock velocity and angle to the line of sight, and insights into the physics of Balmer- dominated shocks. In addition, we will search for possible changes of electron-ion equilibration around the remnant, which may be related to the angle the shocks make with respect to the ambient magnetic field. This spectroscopic dataset will be combined with the optical, X-ray (ROSAT PSPC and HRI), and radio data we have in hand. Our multiwavelength study will provide a better overall understanding of the state of the remnant and its history (as the possible remnant of SN 185 A.D.), as well as the physics of the shocks which define its periphery. This is a resubmission of last year's proposal, for which we were assigned time but lost most of the two runs due to bad weather.