Author name code: cho ADS astronomy entries on 2022-09-14 author:"Cho, Kyung Suk" ------------------------------------------------------------------------ Title: Interferometric imaging, and beam-formed study of a moving Type IV Radio burst with LOFAR Authors: Liu, Hongyu; Zucca, Pietro; Cho, Kyung-Suk; Kumari, Anshu; Zhang, Peijin; Magdalenic, Jasmina; Kim, Rok-Soon; Kim, Sujin; Kang, Juhyung Bibcode: 2022arXiv220813670L Altcode: Type IV radio burst has been studied for over 50 years. However, the specifics of the radio emission mechanisms is still an open question. In order to provide more information about the emission mechanisms, we studied a moving type IV radio burst with fine structures (spike group) by using the high resolution capability of Low-Frequency Array (LOFAR) on Aug 25, 2014\textbf{ (SOLA-D-21-00188)}. We present a comparison of Nançay RadioHeliograph (NRH) and the first LOFAR imaging data of type IV radio burst. The degree of circular polarization (DCP) is calculated at frequencies in the range 20$\sim$180 MHz using LOFAR data, and it was found that the value of DCP gradually increased during the event, with values of 10\%$\sim$20\%. LOFAR interferometric data were combined with white light observations in order to track the propagation of this type IV. The kinematics shows a westward motion of the radio sources, slower than the CME leading edge. The dynamic spectrum of LOFAR shows a large number of fine structures with duration of less than 1s and high brightness temperature ($T_\mathrm{B}$), i.e. $10^{12}$$\sim$$10^{13}$ K. The gradual increase of DCP supports gyrosynchrotron emission as the most plausible mechanism for the type IV. However, coherent emissions such as Electron Cyclotron Maser (ECM) instability can be responsible for small scale fine structures. Countless fine structures altogether were responsible for such high $T_\mathrm{B}$. Title: Reconstruction of Coronal Magnetic Fields Using a Poloidal-Toroidal Representation Authors: Yi, Sibaek; Choe, G. S.; Cho, Kyung-Suk; Solanki, Sami K.; Büchner, Jörg Bibcode: 2022arXiv220607189Y Altcode: A new method for reconstruction of coronal magnetic fields as force-free fields (FFFs) is presented. Our method employs poloidal and toroidal functions to describe divergence-free magnetic fields. This magnetic field representation naturally enables us to implement the boundary conditions at the photospheric boundary, i.e., the normal magnetic field and the normal current density there, in a straightforward manner. At the upper boundary of the corona, a source-surface condition can be employed, which accommodates magnetic flux imbalance at the bottom boundary. Although our iteration algorithm is inspired by extant variational methods, it is non-variational and requires much less iteration steps than most of them. The computational code based on our new method is tested against the analytical FFF solutions by Titov & Démoulin (1999). It is found to excel in reproducing a tightly wound flux rope, a bald patch and quasi-separatrix layers with a hyperbolic flux tube. Title: Kink Oscillation of a Flux Rope During a Failed Solar Eruption Authors: Kumar, Pankaj; Nakariakov, Valery M.; Karpen, Judith T.; Richard DeVore, C.; Cho, Kyung-Suk Bibcode: 2022ApJ...932L...9K Altcode: 2022arXiv220503480K We report a decaying kink oscillation of a flux rope during a confined eruptive flare, observed off the solar limb by the Solar Dynamics Observatory's Atmospheric Imaging Assembly (AIA), which lacked a detectable white-light coronal mass ejection. The erupting flux rope underwent kinking, rotation, and apparent leg-leg interaction during the event. The oscillations were observed simultaneously in multiple AIA channels at 304, 171, and 193 Å, indicating that multithermal plasma was entrained in the rope. After reaching the overlying loops in the active region, the flux rope exhibited large-amplitude, decaying kink oscillations with an apparent initial amplitude of 30 Mm, a period of about 16 minutes, and a decay time of about 17 minutes. We interpret these oscillations as a fundamental standing kink mode of the flux rope. The oscillation polarization has a clear vertical component, while the departure of the detected waveform from a sinusoidal signal suggests that the oscillation could be circularly or elliptically polarized. The estimated kink speed is 1080 km s-1, corresponding to an Alfvén speed of about 760 km s-1. This speed, together with the estimated electron density in the rope from our differential emission measure analysis, n e ≍ (1.5-2.0) × 109 cm-3, yields a magnetic-field strength of about 15 G. To the best of our knowledge, decaying kink oscillations of a flux rope with nonhorizontal polarization during a confined eruptive flare have not been reported before. These oscillations provide unique opportunities for indirect measurements of the magnetic-field strength in low-coronal flux ropes during failed eruptions. Title: Application of NASA core Flight System to Telescope Control Software for 2017 Total Solar Eclipse Observation Authors: Park, Jongyeob; Lee, Jae-Ok; Kim, Jihun; Bong, Su-Chan; Cho, Kyung-Suk; Choi, Seonghwan; Jang, Bi-Ho; Park, Young-Deuk; Moon, Yong-Jae; Baek, Ji-Hye; Yang, Heesu; Kim, Sujin; Kim, Yeon-Han; Timmons, Elizabeth; Swinski, Joseph-paul A. Bibcode: 2022PASP..134c4504P Altcode: The core Flight System (cFS), developed by NASA, is a reusable software framework and a set of pluggable software applications that take advantage of the rich heritage of NASA's successful space missions. We applied the cFS to the development of telescope control software for the observation of the 2017 total solar eclipse. Four main modules were developed: imaging control, mechanism control, data handling, and automated observation. Other modules, such as communication and scheduler, were reused from the cFS. Using an integrated observation system, we successfully observed the total solar eclipse, in which the linearly polarized brightness of the solar corona and sky background were measured at four different wavelengths. In this study, we demonstrated the usefulness of the cFS to develop telescope control software through an eclipse observation system, the so-called DICE (DIagnostic Coronagraph Experiment) mission. Our experience and knowledge of the cFS were expanded to a flight software BITSE (Balloon-borne Investigation of Temperature and Speed of Electrons in the corona), the high-altitude scientific balloon mission in 2019. We plan to apply this approach to future solar coronagraph observations, such as CODEX (COronal Diagnostic EXperiment), on the International Space Station. We expect that the cFS can also be applied in telescope control software for ground-and space-based observations. Title: Building on Stories to Engage Children in Spatial Thinking Authors: Plummer, J.; Cho, K.; Botch, M. Bibcode: 2021ASPC..531...14P Altcode: Early development of spatial thinking has the potential to increase children's achievement in science and math, and may increase children's potential for STEM careers. Spatial thinking involves how we manipulate information, both mentally and through representations in the world around us, to understand the location of objects, their relative locations, how they move with respect to each other, and estimating their shapes and sizes. One promising, though under-researched strategy to improve STEM learning is the use of storytelling in programs for young learners. This interactive session will begin by introducing participants to research on how stories shape learning and how this can be leveraged to engage learners with strategies that support spatial thinking. We will then introduce participants to a new program for early childhood audiences that combine a children's storybook ("Lunar Craters" by Kyungjin Cho) with activities designed to support spatial thinking through the use of spatial language, gestures, object-manipulation, and whole-body movement. We will briefly share results from a recent study completed with 3-5 year-old audiences in preschool and museum settings to illustrate how story and story-driven programs may support children's spatial thinking. Finally, participants will have the opportunity to try their hand at planning for spatial thinking with story-based programming. Participants will be provided with an astronomy-based storybook narrative (appropriate for PreK or elementary-age students) and will engage collaboratively to consider ways to use the narrative as inspiration for activities designed to engage children in spatial thinking. Title: Observational Kinematic Characteristics of Blobs in Solar Coronal Helmet and Pseudo Streamers Authors: Lee, Jae-Ok; Cho, Kyung-Suk; An, Junmo; Lee, Hwanhee; Seough, Jungjoon; Kim, Yeon-Han; Kumar, Pankaj Bibcode: 2021ApJ...920L...6L Altcode: We examine two helmet and two pseudo streamers (HSs and PSs) observed on 2018 and 2019. The HSs (PSs) have dark coronal cavities and stretched loop structures (twin coronal cavities and narrow plasma sheet) at their bases, which are well observed in K-Coronagraph (K-Cor). Their outer-corona structures (top of core, cusp, and stalk) are also clearly identified in LASCO-C2. By investigating LASCO-C2 images, we find the following characteristics. (1) Blobs persistently move outward along the centers of HSs and PSs as well as their legs until the base of a stalk. We also detect outward-moving blobs along their outsides. (2) Blobs along the HS centers formed below tops of cores (~2.6 R⊙), while the other HS and PS blobs might be generated below 2.0 R⊙. (3) HS blob speeds are generally similar to or smaller than the solar wind speed based on Parker's model, while PS ones are larger. (4) HS (PS) blob speeds along the streamer centers are slightly smaller (larger) than those along the streamer legs, might be explained by the expansion-factor model. The blob speeds inside streamer structures (centers and legs) are larger than outside ones closer to solar equator, similar to typical solar wind speed distributions at solar minimum. (5) Several blobs along the HS centers only show sudden speed jumps at streamer cusps. These might be caused by sunward tension forces of overlying stretched closed fields and/or bidirectional outflows by magnetic reconnections in the cusps. Title: Searching for solar KDAR with DUNE Authors: Abed Abud, A.; Abi, B.; Acciarri, R.; Acero, M. A.; Adames, M. R.; Adamov, G.; Adams, D.; Adinolfi, M.; Aduszkiewicz, A.; Aguilar, J.; Ahmad, Z.; Ahmed, J.; Ali-Mohammadzadeh, B.; Alion, T.; Allison, K.; Alonso Monsalve, S.; Alrashed, M.; Alt, C.; Alton, A.; Amedo, P.; Anderson, J.; Andreopoulos, C.; Andreotti, M.; Andrews, M. P.; Andrianala, F.; Andringa, S.; Anfimov, N.; Ankowski, A.; Antoniassi, M.; Antonova, M.; Antoshkin, A.; Antusch, S.; Aranda-Fernandez, A.; Ariga, A.; Arnold, L. O.; Arroyave, M. A.; Asaadi, J.; Asquith, L.; Aurisano, A.; Aushev, V.; Autiero, D.; Ayala-Torres, M.; Azfar, F.; Back, A.; Back, H.; Back, J. J.; Backhouse, C.; Baesso, P.; Bagaturia, I.; Bagby, L.; Balashov, N.; Balasubramanian, S.; Baldi, P.; Baller, B.; Bambah, B.; Barao, F.; Barenboim, G.; Barker, G. J.; Barkhouse, W.; Barnes, C.; Barr, G.; Barranco Monarca, J.; Barros, A.; Barros, N.; Barrow, J. L.; Basharina-Freshville, A.; Bashyal, A.; Basque, V.; Belchior, E.; Battat, J. B. R.; Battisti, F.; Bay, F.; Bazo Alba, J. L.; Beacom, J. F.; Bechetoille, E.; Behera, B.; Bellantoni, L.; Bellettini, G.; Bellini, V.; Beltramello, O.; Belver, D.; Benekos, N.; Benitez Montiel, C.; Bento Neves, F.; Berger, J.; Berkman, S.; Bernardini, P.; Berner, R. M.; Berns, H.; Bertolucci, S.; Betancourt, M.; Betancur Rodríguez, A.; Bevan, A.; Bezerra, T. J. C.; Bhatnagar, V.; Bhattacharjee, M.; Bhuller, S.; Bhuyan, B.; Biagi, S.; Bian, J.; Biassoni, M.; Biery, K.; Bilki, B.; Bishai, M.; Bitadze, A.; Blake, A.; Blaszczyk, F. D. M.; Blazey, G. C.; Blucher, E.; Boissevain, J.; Bolognesi, S.; Bolton, T.; Bomben, L.; Bonesini, M.; Bongrand, M.; Bonini, F.; Booth, A.; Booth, C.; Boran, F.; Bordoni, S.; Borkum, A.; Boschi, T.; Bostan, N.; Bour, P.; Bourgeois, C.; Boyd, S. B.; Boyden, D.; Bracinik, J.; Braga, D.; Brailsford, D.; Branca, A.; Brandt, A.; Bremer, J.; Brew, C.; Brianne, E.; Brice, S. J.; Brizzolari, C.; Bromberg, C.; Brooijmans, G.; Brooke, J.; Bross, A.; Brunetti, G.; Brunetti, M.; Buchanan, N.; Budd, H.; Butorov, I.; Cagnoli, I.; Caiulo, D.; Calabrese, R.; Calafiura, P.; Calcutt, J.; Calin, M.; Calvez, S.; Calvo, E.; Caminata, A.; Campanelli, M.; Cankocak, K.; Caratelli, D.; Carini, G.; Carlus, B.; Carneiro, M. F.; Carniti, P.; Caro Terrazas, I.; Carranza, H.; Carroll, T.; Castaño Forero, J. F.; Castillo, A.; Castromonte, C.; Catano-Mur, E.; Cattadori, C.; Cavalier, F.; Cavanna, F.; Centro, S.; Cerati, G.; Cervelli, A.; Cervera Villanueva, A.; Chalifour, M.; Chappell, A.; Chardonnet, E.; Charitonidis, N.; Chatterjee, A.; Chattopadhyay, S.; Chen, H.; Chen, M.; Chen, Y.; Chen, Z.; Cheon, Y.; Cherdack, D.; Chi, C.; Childress, S.; Chiriacescu, A.; Chisnall, G.; Cho, K.; Choate, S.; Chokheli, D.; Chong, P. S.; Choubey, S.; Christensen, A.; Christian, D.; Christodoulou, G.; Chukanov, A.; Chung, M.; Church, E.; Cicero, V.; Clarke, P.; Coan, T. E.; Cocco, A. G.; Coelho, J. A. B.; Conley, E.; Conley, R.; Conrad, J. M.; Convery, M.; Copello, S.; Corwin, L.; Valentim, R.; Cremaldi, L.; Cremonesi, L.; Crespo-Anadón, J. I.; Crisler, M.; Cristaldo, E.; Cross, R.; Cudd, A.; Cuesta, C.; Cui, Y.; Cussans, D.; Dalager, O.; da Motta, H.; Da Silva Peres, L.; David, C.; David, Q.; Davies, G. S.; Davini, S.; Dawson, J.; De, K.; Debbins, P.; De Bonis, I.; Decowski, M. P.; de Gouvêa, A.; De Holanda, P. C.; De Icaza Astiz, I. L.; Deisting, A.; De Jong, P.; Delbart, A.; Delepine, D.; Delgado, M.; Dell'Acqua, A.; De Lurgio, P.; de Mello Neto, J. R. T.; DeMuth, D. M.; Dennis, S.; Densham, C.; Deptuch, G. W.; De Roeck, A.; De Romeri, V.; De Souza, G.; Devi, R.; Dharmapalan, R.; Dias, M.; Diaz, F.; Díaz, J. S.; Di Domizio, S.; Di Giulio, L.; Ding, P.; Di Noto, L.; Distefano, C.; Diurba, R.; Diwan, M.; Djurcic, Z.; Doering, D.; Dolan, S.; Dolek, F.; Dolinski, M. J.; Domine, L.; Douglas, D.; Douillet, D.; Drake, G.; Drielsma, F.; Duarte, L.; Duchesneau, D.; Duffy, K.; Dunne, P.; Durkin, T.; Duyang, H.; Dvornikov, O.; Dwyer, D. A.; Dyshkant, A. S.; Eads, M.; Earle, A.; Edmunds, D.; Eisch, J.; Emberger, L.; Emery, S.; Ereditato, A.; Erjavec, T.; Escobar, C. O.; Eurin, G.; Evans, J. J.; Ewart, E.; Ezeribe, A. C.; Fahey, K.; Falcone, A.; Fani', M.; Farnese, C.; Farzan, Y.; Fedoseev, D.; Felix, J.; Feng, Y.; Fernandez-Martinez, E.; Fernandez Menendez, P.; Fernandez Morales, M.; Ferraro, F.; Fields, L.; Filip, P.; Filthaut, F.; Fiorentini, A.; Fiorini, M.; Fitzpatrick, R. S.; Flanagan, W.; Fleming, B.; Flight, R.; Forero, D. V.; Fowler, J.; Fox, W.; Franc, J.; Francis, K.; Franco, D.; Freeman, J.; Freestone, J.; Fried, J.; Friedland, A.; Fuentes Robayo, F.; Fuess, S.; Furic, I. K.; Furmanski, A. P.; Gabrielli, A.; Gago, A.; Gallagher, H.; Gallas, A.; Gallego-Ros, A.; Gallice, N.; Galymov, V.; Gamberini, E.; Gamble, T.; Ganacim, F.; Gandhi, R.; Gandrajula, R.; Gao, F.; Gao, S.; Garcia B., A. C.; Garcia-Gamez, D.; García-Peris, A.; Gardiner, S.; Gastler, D.; Gauvreau, J.; Ge, G.; Gelli, B.; Gendotti, A.; Gent, S.; Ghorbani-Moghaddam, Z.; Giammaria, P.; Giammaria, T.; Gibin, D.; Gil-Botella, I.; Gilligan, S.; Girerd, C.; Giri, A. K.; Gnani, D.; Gogota, O.; Gold, M.; Gollapinni, S.; Gollwitzer, K.; Gomes, R. A.; Gomez Bermeo, L. V.; Gomez Fajardo, L. S.; Gonnella, F.; Gonzalez-Cuevas, J. A.; Gonzalez Diaz, D.; Gonzalez-Lopez, M.; Goodman, M. C.; Goodwin, O.; Goswami, S.; Gotti, C.; Goudzovski, E.; Grace, C.; Graham, M.; Gran, R.; Granados, E.; Granger, P.; Grant, A.; Grant, C.; Gratieri, D.; Green, P.; Greenler, L.; Greer, J.; Grenard, J.; Griffith, W. C.; Groh, M.; Grudzinski, J.; Grzelak, K.; Gu, W.; Guardincerri, E.; Guarino, V.; Guarise, M.; Guenette, R.; Guerard, E.; Guerzoni, M.; Guglielmi, A.; Guo, B.; Guthikonda, K. K.; Gutierrez, R.; Guzowski, P.; Guzzo, M. M.; Gwon, S.; Ha, C.; Habig, A.; Hadavand, H.; Haenni, R.; Hahn, A.; Haiston, J.; Hamacher-Baumann, P.; Hamernik, T.; Hamilton, P.; Han, J.; Harris, D. A.; Hartnell, J.; Harton, J.; Hasegawa, T.; Hasnip, C.; Hatcher, R.; Hatfield, K. W.; Hatzikoutelis, A.; Hayes, C.; Hayrapetyan, K.; Hays, J.; Hazen, E.; He, M.; Heavey, A.; Heeger, K. M.; Heise, J.; Hennessy, K.; Henry, S.; Hernandez Morquecho, M. A.; Herner, K.; Hertel, L.; Hewes, J.; Higuera, A.; Hill, T.; Hillier, S. J.; Himmel, A.; Hirsch, L. R.; Ho, J.; Hoff, J.; Holin, A.; Hoppe, E.; Horton-Smith, G. A.; Hostert, M.; Hourlier, A.; Howard, B.; Howell, R.; Hristova, I.; Hronek, M. S.; Huang, J.; Huang, J.; Hugon, J.; Iles, G.; Ilic, N.; Iliescu, A. M.; Illingworth, R.; Ingratta, G.; Ioannisian, A.; Isenhower, L.; Itay, R.; Izmaylov, A.; Jackson, C. M.; Jain, V.; James, E.; Jang, W.; Jargowsky, B.; Jediny, F.; Jena, D.; Jeong, Y. S.; Jesús-Valls, C.; Ji, X.; Jiang, L.; Jiménez, S.; Jipa, A.; Johnson, R.; Johnston, N.; Jones, B.; Jones, S. B.; Judah, M.; Jung, C. K.; Junk, T.; Jwa, Y.; Kabirnezhad, M.; Kaboth, A.; Kadenko, I.; Kalra, D.; Kakorin, I.; Kalitkina, A.; Kamiya, F.; Kaneshige, N.; Karagiorgi, G.; Karaman, G.; Karcher, A.; Karolak, M.; Karyotakis, Y.; Kasai, S.; Kasetti, S. P.; Kashur, L.; Kazaryan, N.; Kearns, E.; Keener, P.; Kelly, K. J.; Kemp, E.; Kemularia, O.; Ketchum, W.; Kettell, S. H.; Khabibullin, M.; Khotjantsev, A.; Khvedelidze, A.; Kim, D.; King, B.; Kirby, B.; Kirby, M.; Klein, J.; Koehler, K.; Koerner, L. W.; Kohn, S.; Koller, P. P.; Kolupaeva, L.; Korablev, D.; Kordosky, M.; Kosc, T.; Kose, U.; Kostelecký, V. A.; Kothekar, K.; Krennrich, F.; Kreslo, I.; Kropp, W.; Kudenko, Y.; Kudryavtsev, V. A.; Kulagin, S.; Kumar, J.; Kumar, P.; Kunze, P.; Kuruppu, C.; Kus, V.; Kutter, T.; Kvasnicka, J.; Kwak, D.; Lambert, A.; Land, B. J.; Lande, K.; Lane, C. E.; Lang, K.; Langford, T.; Langstaff, M.; Larkin, J.; Lasorak, P.; Last, D.; Lastoria, C.; Laundrie, A.; Laurenti, G.; Lawrence, A.; Lazanu, I.; LaZur, R.; Lazzaroni, M.; Le, T.; Leardini, S.; Learned, J.; LeBrun, P.; LeCompte, T.; Lee, C.; Lee, S. Y.; Lehmann Miotto, G.; Lehnert, R.; Leigui de Oliveira, M. A.; Leitner, M.; Lepin, L. M.; Li, L.; Li, S. W.; Li, T.; Li, Y.; Liao, H.; Lin, C. S.; Lin, Q.; Lin, S.; Ling, J.; Lister, A.; Littlejohn, B. R.; Liu, J.; Lockwitz, S.; Loew, T.; Lokajicek, M.; Lomidze, I.; Long, K.; Loo, K.; Lord, T.; LoSecco, J. M.; Louis, W. C.; Lu, X. -G.; Luk, K. B.; Luo, X.; Luppi, E.; Lurkin, N.; Lux, T.; Luzio, V. P.; MacFarlane, D.; Machado, A. A.; Machado, P.; Macias, C. T.; Macier, J. R.; Maddalena, A.; Madera, A.; Madigan, P.; Magill, S.; Mahn, K.; Maio, A.; Major, A.; Maloney, J. A.; Mandrioli, G.; Mandujano, R. C.; Maneira, J.; Manenti, L.; Manly, S.; Mann, A.; Manolopoulos, K.; Manrique Plata, M.; Manyam, V. N.; Manzanillas, L.; Marchan, M.; Marchionni, A.; Marciano, W.; Marfatia, D.; Mariani, C.; Maricic, J.; Marie, R.; Marinho, F.; Marino, A. D.; Marsden, D.; Marshak, M.; Marshall, C. M.; Marshall, J.; Marteau, J.; Martin-Albo, J.; Martinez, N.; Martinez Caicedo, D. A.; Martynenko, S.; Mascagna, V.; Mason, K.; Mastbaum, A.; Masud, M.; Matichard, F.; Matsuno, S.; Matthews, J.; Mauger, C.; Mauri, N.; Mavrokoridis, K.; Mawby, I.; Mazza, R.; Mazzacane, A.; Mazzucato, E.; McAskill, T.; McCluskey, E.; McConkey, N.; McFarland, K. S.; McGrew, C.; McNab, A.; Mefodiev, A.; Mehta, P.; Melas, P.; Mena, O.; Menary, S.; Mendez, H.; Mendez, P.; M, D. P.; Menegolli, A.; Meng, G.; Messier, M. D.; Metcalf, W.; Mettler, T.; Mewes, M.; Meyer, H.; Miao, T.; Michna, G.; Miedema, T.; Mikola, V.; Milincic, R.; Miller, G.; Miller, W.; Mills, J.; Milne, C.; Mineev, O.; Miranda, O. G.; Miryala, S.; Mishra, C. S.; Mishra, S. R.; Mislivec, A.; Mladenov, D.; Mocioiu, I.; Moffat, K.; Moggi, N.; Mohanta, R.; Mohayai, T. A.; Mokhov, N.; Molina, J.; Molina Bueno, L.; Montagna, E.; Montanari, A.; Montanari, C.; Montanari, D.; Montano Zetina, L. M.; Moon, J.; Moon, S. H.; Mooney, M.; Moor, A. F.; Moreno, D.; Morris, C.; Mossey, C.; Motuk, E.; Moura, C. A.; Mousseau, J.; Mouster, G.; Mu, W.; Mualem, L.; Mueller, J.; Muether, M.; Mufson, S.; Muheim, F.; Muir, A.; Mulhearn, M.; Munford, D.; Muramatsu, H.; Murphy, S.; Musser, J.; Nachtman, J.; Nagu, S.; Nalbandyan, M.; Nandakumar, R.; Naples, D.; Narita, S.; Nath, A.; Navas-Nicolás, D.; Navrer-Agasson, A.; Nayak, N.; Nebot-Guinot, M.; Negishi, K.; Nelson, J. K.; Nesbit, J.; Nessi, M.; Newbold, D.; Newcomer, M.; Newhart, D.; Newton, H.; Nichol, R.; Nicolas-Arnaldos, F.; Niner, E.; Nishimura, K.; Norman, A.; Norrick, A.; Northrop, R.; Novella, P.; Nowak, J. A.; Oberling, M.; Ochoa-Ricoux, J. P.; Olivares Del Campo, A.; Olivier, A.; Olshevskiy, A.; Onel, Y.; Onishchuk, Y.; Ott, J.; Pagani, L.; Pakvasa, S.; Palacio, G.; Palamara, O.; Palestini, S.; Paley, J. M.; Pallavicini, M.; Palomares, C.; Palomino-Gallo, J. L.; Panduro Vazquez, W.; Pantic, E.; Paolone, V.; Papadimitriou, V.; Papaleo, R.; Papanestis, A.; Paramesvaran, S.; Parke, S.; Parozzi, E.; Parsa, Z.; Parvu, M.; Pascoli, S.; Pasqualini, L.; Pasternak, J.; Pater, J.; Patrick, C.; Patrizii, L.; Patterson, R. B.; Patton, S. J.; Patzak, T.; Paudel, A.; Paulos, B.; Paulucci, L.; Pavlovic, Z.; Pawloski, G.; Payne, D.; Pec, V.; Peeters, S. J. M.; Pennacchio, E.; Penzo, A.; Peres, O. L. G.; Perry, J.; Pershey, D.; Pessina, G.; Petrillo, G.; Petta, C.; Petti, R.; Pia, V.; Piastra, F.; Pickering, L.; Pietropaolo, F.; Plunkett, R.; Poling, R.; Pons, X.; Poonthottathil, N.; Poppi, F.; Pordes, S.; Porter, J.; Potekhin, M.; Potenza, R.; Potukuchi, B. V. K. S.; Pozimski, J.; Pozzato, M.; Prakash, S.; Prakash, T.; Prest, M.; Prince, S.; Psihas, F.; Pugnere, D.; Qian, X.; Queiroga Bazetto, M. C.; Raaf, J. L.; Radeka, V.; Rademacker, J.; Radics, B.; Rafique, A.; Raguzin, E.; Rai, M.; Rajaoalisoa, M.; Rakhno, I.; Rakotonandrasana, A.; Rakotondravohitra, L.; Ramachers, Y. A.; Rameika, R.; Ramirez Delgado, M. A.; Ramson, B.; Rappoldi, A.; Raselli, G.; Ratoff, P.; Raut, S.; Razakamiandra, R. F.; Rea, E.; Real, J. S.; Rebel, B.; Reggiani-Guzzo, M.; Rehak, T.; Reichenbacher, J.; Reitzner, S. D.; Rejeb Sfar, H.; Renshaw, A.; Rescia, S.; Resnati, F.; Reynolds, A.; Ribas, M.; Riboldi, S.; Riccio, C.; Riccobene, G.; Rice, L. C. J.; Ricol, J.; Rigamonti, A.; Rigaut, Y.; Rivera, D.; Robert, A.; Rochester, L.; Roda, M.; Rodrigues, P.; Rodriguez Alonso, M. J.; Rodriguez Bonilla, E.; Rodriguez Rondon, J.; Rosauro-Alcaraz, S.; Rosenberg, M.; Rosier, P.; Roskovec, B.; Rossella, M.; Rossi, M.; Rott, C.; Rout, J.; Roy, P.; Roy, S.; Rubbia, A.; Rubbia, C.; Rubio, F. C.; Russell, B.; Ruterbories, D.; Rybnikov, A.; Saa-Hernandez, A.; Saakyan, R.; Sacerdoti, S.; Safford, T.; Sahu, N.; Sala, P.; Samios, N.; Samoylov, O.; Sanchez, M. C.; Sandberg, V.; Sanders, D. A.; Sankey, D.; Santana, S.; Santos-Maldonado, M.; Saoulidou, N.; Sapienza, P.; Sarasty, C.; Sarcevic, I.; Savage, G.; Savinov, V.; Scaramelli, A.; Scarff, A.; Scarpelli, A.; Schaffer, T.; Schellman, H.; Schifano, S.; Schlabach, P.; Schmitz, D.; Scholberg, K.; Schukraft, A.; Segreto, E.; Selyunin, A.; Senise, C. R.; Sensenig, J.; Seoane, M.; Seong, I.; Sergi, A.; Sgalaberna, D.; Shaevitz, M. H.; Shafaq, S.; Shamma, M.; Sharankova, R.; Sharma, H. R.; Sharma, R.; Kumar, R.; Shaw, T.; Shepherd-Themistocleous, C.; Sheshukov, A.; Shin, S.; Shoemaker, I.; Shooltz, D.; Shrock, R.; Siegel, H.; Simard, L.; Simon, F.; Sinclair, J.; Sinev, G.; Singh, J.; Singh, J.; Singh, L.; Singh, V.; Sipos, R.; Sippach, F. W.; Sirri, G.; Sitraka, A.; Siyeon, K.; Skarpaas, K.; Smith, A.; Smith, E.; Smith, P.; Smolik, J.; Smy, M.; Snider, E. L.; Snopok, P.; Snowden-Ifft, D.; Soares Nunes, M.; Sobel, H.; Soderberg, M.; Sokolov, S.; Solano Salinas, C. J.; Söldner-Rembold, S.; Soleti, S. R.; Solomey, N.; Solovov, V.; Sondheim, W. E.; Sorel, M.; Sotnikov, A.; Soto-Oton, J.; Sousa, A.; Soustruznik, K.; Spagliardi, F.; Spanu, M.; Spitz, J.; Spooner, N. J. C.; Spurgeon, K.; Staley, R.; Stancari, M.; Stanco, L.; Stanley, R.; Stein, R.; Steiner, H. M.; Steklain Lisbôa, A. F.; Stewart, J.; Stillwell, B.; Stock, J.; Stocker, F.; Stokes, T.; Strait, M.; Strauss, T.; Striganov, S.; Stuart, A.; Suarez, J. G.; Sullivan, H.; Summers, D.; Surdo, A.; Susic, V.; Suter, L.; Sutera, C. M.; Svoboda, R.; Szczerbinska, B.; Szelc, A. M.; Tanaka, H. A.; Tapia Oregui, B.; Tapper, A.; Tariq, S.; Tatar, E.; Tayloe, R.; Teklu, A. M.; Tenti, M.; Terao, K.; Ternes, C. A.; Terranova, F.; Testera, G.; Thakore, T.; Thea, A.; Thompson, J. L.; Thorn, C.; Timm, S. C.; Tishchenko, V.; Todd, J.; Tomassetti, L.; Tonazzo, A.; Torbunov, D.; Torti, M.; Tortola, M.; Tortorici, F.; Tosi, N.; Totani, D.; Toups, M.; Touramanis, C.; Travaglini, R.; Trevor, J.; Trilov, S.; Tripathi, A.; Trzaska, W. H.; Tsai, Y.; Tsai, Y. -T.; Tsamalaidze, Z.; Tsang, K. V.; Tsverava, N.; Tufanli, S.; Tull, C.; Tyley, E.; Tzanov, M.; Uboldi, L.; Uchida, M. A.; Urheim, J.; Usher, T.; Uzunyan, S.; Vagins, M. R.; Vahle, P.; Valdiviesso, G. A.; Valencia, E.; Vallari, Z.; Vallazza, E.; Valle, J. W. F.; Vallecorsa, S.; Van Berg, R.; Van de Water, R. G.; Varanini, F.; Vargas, D.; Varner, G.; Vasel, J.; Vasina, S.; Vasseur, G.; Vaughan, N.; Vaziri, K.; Ventura, S.; Verdugo, A.; Vergani, S.; Vermeulen, M. A.; Verzocchi, M.; Vicenzi, M.; Vieira de Souza, H.; Vignoli, C.; Vilela, C.; Viren, B.; Vrba, T.; Wachala, T.; Waldron, A. V.; Wallbank, M.; Wallis, C.; Wang, H.; Wang, J.; Wang, L.; Wang, M. H. L. S.; Wang, Y.; Wang, Y.; Warburton, K.; Warner, D.; Wascko, M. O.; Waters, D.; Watson, A.; Weatherly, P.; Weber, A.; Weber, M.; Wei, H.; Weinstein, A.; Wenman, D.; Wetstein, M.; White, A.; Whitehead, L. H.; Whittington, D.; Wilking, M. J.; Wilkinson, C.; Williams, Z.; Wilson, F.; Wilson, R. J.; Wisniewski, W.; Wolcott, J.; Wongjirad, T.; Wood, A.; Wood, K.; Worcester, E.; Worcester, M.; Wret, C.; Wu, W.; Wu, W.; Xiao, Y.; Xie, F.; Yandel, E.; Yang, G.; Yang, K.; Yang, S.; Yang, T.; Yankelevich, A.; Yershov, N.; Yonehara, K.; Young, T.; Yu, B.; Yu, H.; Yu, H.; Yu, J.; Yuan, W.; Zaki, R.; Zalesak, J.; Zambelli, L.; Zamorano, B.; Zani, A.; Zazueta, L.; Zeller, G. P.; Zennamo, J.; Zeug, K.; Zhang, C.; Zhao, M.; Zhivun, E.; Zhu, G.; Zilberman, P.; Zimmerman, E. D.; Zito, M.; Zucchelli, S.; Zuklin, J.; Zutshi, V.; Zwaska, R.; DUNE Collaboration Bibcode: 2021JCAP...10..065A Altcode: The observation of 236 MeV muon neutrinos from kaon-decay-at-rest (KDAR) originating in the core of the Sun would provide a unique signature of dark matter annihilation. Since excellent angle and energy reconstruction are necessary to detect this monoenergetic, directional neutrino flux, DUNE with its vast volume and reconstruction capabilities, is a promising candidate for a KDAR neutrino search. In this work, we evaluate the proposed KDAR neutrino search strategies by realistically modeling both neutrino-nucleus interactions and the response of DUNE. We find that, although reconstruction of the neutrino energy and direction is difficult with current techniques in the relevant energy range, the superb energy resolution, angular resolution, and particle identification offered by DUNE can still permit great signal/background discrimination. Moreover, there are non-standard scenarios in which searches at DUNE for KDAR in the Sun can probe dark matter interactions. Title: DH Type II Radio Bursts During Solar Cycles 23 and 24: Frequency-Dependent Classification and Their Flare-CME Associations Authors: Patel, Binal D.; Joshi, Bhuwan; Cho, Kyung-Suk; Kim, Rok-Soon Bibcode: 2021SoPh..296..142P Altcode: 2021arXiv210812990P We present the characteristics of DH type II bursts for the Solar Cycles 23 and 24. The bursts are classified according to their end frequencies into three categories: Low-Frequency Group (LFG; 20 kHz ≤ f ≤ 200 kHz), Medium-Frequency Group (MFG; 200 kHz <f ≤1 MHz), and High-Frequency Group (HFG; 1 MHz <f ≤16 MHz). We find that the sources for LFG, MFG, and HFG events are homogeneously distributed over the active region belt. Our analysis shows a drastic reduction of the DH type II events during Solar Cycle 24, which includes only 35% of the total events (i.e., 179 out of 514). Despite having smaller number of DH type II events in the Solar Cycle 24, it contains a significantly higher fraction of LFG events compared to the previous cycle (32% versus 24%). However, within the LFG group, the cycle 23 exhibits significant dominance of type II bursts that extend below 50 kHz, suggesting rich population of powerful CMEs traveling beyond half of the Sun-Earth distance. The events of LFG group display strongest association with faster and wider (more than 82% events are halo) CMEs, whereas at the source location, they predominantly trigger large M/X class flares (in more than 83% cases). Our analysis also indicates that CME initial speed or flare energetics is partly related to the duration of type II burst and that survival of CME-associated shock is determined by multiple factors/parameters related to CMEs, flares, and state of coronal and interplanetary medium. The profiles relating CME heights with respect to the end frequencies of DH type II bursts suggest that for HFG and MFG categories, the location for majority of CMEs (≈ 65%-70%) is in well compliance with ten-fold Leblanc coronal density model, whereas for LFG events, a lower value of density multiplier (≈ 3) seems to be compatible. Title: Searching for solar KDAR with DUNE Authors: DUNE Collaboration; Abed Abud, A.; Abi, B.; Acciarri, R.; Acero, M. A.; Adames, M. R.; Adamov, G.; Adams, D.; Adinolfi, M.; Aduszkiewicz, A.; Aguilar, J.; Ahmad, Z.; Ahmed, J.; Ali-Mohammadzadeh, B.; Alion, T.; Allison, K.; Alonso Monsalve, S.; Alrashed, M.; Alt, C.; Alton, A.; Amedo, P.; Anderson, J.; Andreopoulos, C.; Andreotti, M.; Andrews, M. P.; Andrianala, F.; Andringa, S.; Anfimov, N.; Ankowski, A.; Antoniassi, M.; Antonova, M.; Antoshkin, A.; Antusch, S.; Aranda-Fernandez, A.; Ariga, A.; Arnold, L. O.; Arroyave, M. A.; Asaadi, J.; Asquith, L.; Aurisano, A.; Aushev, V.; Autiero, D.; Ayala-Torres, M.; Azfar, F.; Back, A.; Back, H.; Back, J. J.; Backhouse, C.; Baesso, P.; Bagaturia, I.; Bagby, L.; Balashov, N.; Balasubramanian, S.; Baldi, P.; Baller, B.; Bambah, B.; Barao, F.; Barenboim, G.; Barker, G. J.; Barkhouse, W.; Barnes, C.; Barr, G.; Barranco Monarca, J.; Barros, A.; Barros, N.; Barrow, J. L.; Basharina-Freshville, A.; Bashyal, A.; Basque, V.; Belchior, E.; Battat, J. B. R.; Battisti, F.; Bay, F.; Bazo Alba, J. L.; Beacom, J. 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K.; Nesbit, J.; Nessi, M.; Newbold, D.; Newcomer, M.; Newhart, D.; Newton, H.; Nichol, R.; Nicolas-Arnaldos, F.; Niner, E.; Nishimura, K.; Norman, A.; Norrick, A.; Northrop, R.; Novella, P.; Nowak, J. A.; Oberling, M.; Ochoa-Ricoux, J. P.; Olivares Del Campo, A.; Olivier, A.; Olshevskiy, A.; Onel, Y.; Onishchuk, Y.; Ott, J.; Pagani, L.; Pakvasa, S.; Palacio, G.; Palamara, O.; Palestini, S.; Paley, J. M.; Pallavicini, M.; Palomares, C.; Palomino-Gallo, J. L.; Panduro Vazquez, W.; Pantic, E.; Paolone, V.; Papadimitriou, V.; Papaleo, R.; Papanestis, A.; Paramesvaran, S.; Parke, S.; Parozzi, E.; Parsa, Z.; Parvu, M.; Pascoli, S.; Pasqualini, L.; Pasternak, J.; Pater, J.; Patrick, C.; Patrizii, L.; Patterson, R. B.; Patton, S. J.; Patzak, T.; Paudel, A.; Paulos, B.; Paulucci, L.; Pavlovic, Z.; Pawloski, G.; Payne, D.; Pec, V.; Peeters, S. J. M.; Pennacchio, E.; Penzo, A.; Peres, O. L. G.; Perry, J.; Pershey, D.; Pessina, G.; Petrillo, G.; Petta, C.; Petti, R.; Pia, V.; Piastra, F.; Pickering, L.; Pietropaolo, F.; Plunkett, R.; Poling, R.; Pons, X.; Poonthottathil, N.; Poppi, F.; Pordes, S.; Porter, J.; Potekhin, M.; Potenza, R.; Potukuchi, B. V. K. S.; Pozimski, J.; Pozzato, M.; Prakash, S.; Prakash, T.; Prest, M.; Prince, S.; Psihas, F.; Pugnere, D.; Qian, X.; Queiroga Bazetto, M. C.; Raaf, J. L.; Radeka, V.; Rademacker, J.; Radics, B.; Rafique, A.; Raguzin, E.; Rai, M.; Rajaoalisoa, M.; Rakhno, I.; Rakotonandrasana, A.; Rakotondravohitra, L.; Ramachers, Y. A.; Rameika, R.; Ramirez Delgado, M. A.; Ramson, B.; Rappoldi, A.; Raselli, G.; Ratoff, P.; Raut, S.; Razakamiandra, R. F.; Rea, E.; Real, J. S.; Rebel, B.; Reggiani-Guzzo, M.; Rehak, T.; Reichenbacher, J.; Reitzner, S. D.; Rejeb Sfar, H.; Renshaw, A.; Rescia, S.; Resnati, F.; Reynolds, A.; Ribas, M.; Riboldi, S.; Riccio, C.; Riccobene, G.; Rice, L. C. J.; Ricol, J.; Rigamonti, A.; Rigaut, Y.; Rivera, D.; Robert, A.; Rochester, L.; Roda, M.; Rodrigues, P.; Rodriguez Alonso, M. J.; Rodriguez Bonilla, E.; Rodriguez Rondon, J.; Rosauro-Alcaraz, S.; Rosenberg, M.; Rosier, P.; Roskovec, B.; Rossella, M.; Rossi, M.; Rott, C.; Rout, J.; Roy, P.; Roy, S.; Rubbia, A.; Rubbia, C.; Rubio, F. C.; Russell, B.; Ruterbories, D.; Rybnikov, A.; Saa-Hernandez, A.; Saakyan, R.; Sacerdoti, S.; Safford, T.; Sahu, N.; Sala, P.; Samios, N.; Samoylov, O.; Sanchez, M. C.; Sandberg, V.; Sanders, D. A.; Sankey, D.; Santana, S.; Santos-Maldonado, M.; Saoulidou, N.; Sapienza, P.; Sarasty, C.; Sarcevic, I.; Savage, G.; Savinov, V.; Scaramelli, A.; Scarff, A.; Scarpelli, A.; Schaffer, T.; Schellman, H.; Schifano, S.; Schlabach, P.; Schmitz, D.; Scholberg, K.; Schukraft, A.; Segreto, E.; Selyunin, A.; Senise, C. R.; Sensenig, J.; Seoane, M.; Seong, I.; Sergi, A.; Sgalaberna, D.; Shaevitz, M. H.; Shafaq, S.; Shamma, M.; Sharankova, R.; Sharma, H. R.; Sharma, R.; Kumar, R.; Shaw, T.; Shepherd-Themistocleous, C.; Sheshukov, A.; Shin, S.; Shoemaker, I.; Shooltz, D.; Shrock, R.; Siegel, H.; Simard, L.; Simon, F.; Sinclair, J.; Sinev, G.; Singh, J.; Singh, J.; Singh, L.; Singh, V.; Sipos, R.; Sippach, F. W.; Sirri, G.; Sitraka, A.; Siyeon, K.; Skarpaas, K.; Smith, A.; Smith, E.; Smith, P.; Smolik, J.; Smy, M.; Snider, E. L.; Snopok, P.; Snowden-Ifft, D.; Soares Nunes, M.; Sobel, H.; Soderberg, M.; Sokolov, S.; Solano Salinas, C. J.; Söldner-Rembold, S.; Soleti, S. R.; Solomey, N.; Solovov, V.; Sondheim, W. E.; Sorel, M.; Sotnikov, A.; Soto-Oton, J.; Sousa, A.; Soustruznik, K.; Spagliardi, F.; Spanu, M.; Spitz, J.; Spooner, N. J. C.; Spurgeon, K.; Staley, R.; Stancari, M.; Stanco, L.; Stanley, R.; Stein, R.; Steiner, H. M.; Steklain Lisbôa, A. F.; Stewart, J.; Stillwell, B.; Stock, J.; Stocker, F.; Stokes, T.; Strait, M.; Strauss, T.; Striganov, S.; Stuart, A.; Suarez, J. G.; Sullivan, H.; Summers, D.; Surdo, A.; Susic, V.; Suter, L.; Sutera, C. M.; Svoboda, R.; Szczerbinska, B.; Szelc, A. M.; Tanaka, H. A.; Tapia Oregui, B.; Tapper, A.; Tariq, S.; Tatar, E.; Tayloe, R.; Teklu, A. M.; Tenti, M.; Terao, K.; Ternes, C. A.; Terranova, F.; Testera, G.; Thakore, T.; Thea, A.; Thompson, J. L.; Thorn, C.; Timm, S. C.; Tishchenko, V.; Todd, J.; Tomassetti, L.; Tonazzo, A.; Torbunov, D.; Torti, M.; Tortola, M.; Tortorici, F.; Tosi, N.; Totani, D.; Toups, M.; Touramanis, C.; Travaglini, R.; Trevor, J.; Trilov, S.; Tripathi, A.; Trzaska, W. H.; Tsai, Y.; Tsai, Y. -T.; Tsamalaidze, Z.; Tsang, K. V.; Tsverava, N.; Tufanli, S.; Tull, C.; Tyley, E.; Tzanov, M.; Uboldi, L.; Uchida, M. A.; Urheim, J.; Usher, T.; Uzunyan, S.; Vagins, M. R.; Vahle, P.; Valdiviesso, G. A.; Valencia, E.; Vallari, Z.; Vallazza, E.; Valle, J. W. F.; Vallecorsa, S.; Van Berg, R.; Van de Water, R. G.; Varanini, F.; Vargas, D.; Varner, G.; Vasel, J.; Vasina, S.; Vasseur, G.; Vaughan, N.; Vaziri, K.; Ventura, S.; Verdugo, A.; Vergani, S.; Vermeulen, M. A.; Verzocchi, M.; Vicenzi, M.; Vieira de Souza, H.; Vignoli, C.; Vilela, C.; Viren, B.; Vrba, T.; Wachala, T.; Waldron, A. V.; Wallbank, M.; Wallis, C.; Wang, H.; Wang, J.; Wang, L.; Wang, M. H. L. S.; Wang, Y.; Wang, Y.; Warburton, K.; Warner, D.; Wascko, M. O.; Waters, D.; Watson, A.; Weatherly, P.; Weber, A.; Weber, M.; Wei, H.; Weinstein, A.; Wenman, D.; Wetstein, M.; White, A.; Whitehead, L. H.; Whittington, D.; Wilking, M. J.; Wilkinson, C.; Williams, Z.; Wilson, F.; Wilson, R. J.; Wisniewski, W.; Wolcott, J.; Wongjirad, T.; Wood, A.; Wood, K.; Worcester, E.; Worcester, M.; Wret, C.; Wu, W.; Wu, W.; Xiao, Y.; Xie, F.; Yandel, E.; Yang, G.; Yang, K.; Yang, S.; Yang, T.; Yankelevich, A.; Yershov, N.; Yonehara, K.; Young, T.; Yu, B.; Yu, H.; Yu, H.; Yu, J.; Yuan, W.; Zaki, R.; Zalesak, J.; Zambelli, L.; Zamorano, B.; Zani, A.; Zazueta, L.; Zeller, G. P.; Zennamo, J.; Zeug, K.; Zhang, C.; Zhao, M.; Zhivun, E.; Zhu, G.; Zilberman, P.; Zimmerman, E. D.; Zito, M.; Zucchelli, S.; Zuklin, J.; Zutshi, V.; Zwaska, R. Bibcode: 2021arXiv210709109D Altcode: The observation of 236 MeV muon neutrinos from kaon-decay-at-rest (KDAR) originating in the core of the Sun would provide a unique signature of dark matter annihilation. Since excellent angle and energy reconstruction are necessary to detect this monoenergetic, directional neutrino flux, DUNE with its vast volume and reconstruction capabilities, is a promising candidate for a KDAR neutrino search. In this work, we evaluate the proposed KDAR neutrino search strategies by realistically modeling both neutrino-nucleus interactions and the response of DUNE. We find that, although reconstruction of the neutrino energy and direction is difficult with current techniques in the relevant energy range, the superb energy resolution, angular resolution, and particle identification offered by DUNE can still permit great signal/background discrimination. Moreover, there are non-standard scenarios in which searches at DUNE for KDAR in the Sun can probe dark matter interactions. Title: Spectroscopic Detection of Alfvénic Waves in the Chromosphere of Sunspot Regions Authors: Chae, Jongchul; Cho, Kyuhyoun; Nakariakov, Valery M.; Cho, Kyung-Suk; Kwon, Ryun-Young Bibcode: 2021ApJ...914L..16C Altcode: Transverse magnetohydrodynamic waves often called Alfvénic (or kink) waves have been often theoretically put forward to solve the outstanding problems of the solar corona like coronal heating, solar wind acceleration, and chemical abundance enhancement. Here we report the first spectroscopic detection of Alfvénic waves around a sunspot at chromospheric heights. By analyzing the spectra of the Hα line and Ca II 854.2 nm line, we determined line-of-sight velocity and temperature as functions of position and time. As a result, we identified transverse magnetohydrodynamic waves pervading the superpenumbral fibrils. These waves are characterized by the periods of 2.5 to 4.5 minutes, and the propagation direction parallel to the fibrils, the supersonic propagation speeds of 45 to 145 km s-1, and the close association with umbral oscillations and running penumbral waves in sunspots. Our results support the notion that the chromosphere around sunspots abounds with Alfvénic waves excited by the mode conversion of the upward-propagating slow magnetoacoustic waves. Title: Supernova neutrino burst detection with the deep underground neutrino experiment Authors: Abi, B.; Acciarri, R.; Acero, M. A.; Adamov, G.; Adams, D.; Adinolfi, M.; Ahmad, Z.; Ahmed, J.; Alion, T.; Alonso Monsalve, S.; Alt, C.; Anderson, J.; Andreopoulos, C.; Andrews, M. P.; Andrianala, F.; Andringa, S.; Ankowski, A.; Antonova, M.; Antusch, S.; Aranda-Fernandez, A.; Ariga, A.; Arnold, L. O.; Arroyave, M. A.; Asaadi, J.; Aurisano, A.; Aushev, V.; Autiero, D.; Azfar, F.; Back, H.; Back, J. J.; Backhouse, C.; Baesso, P.; Bagby, L.; Bajou, R.; Balasubramanian, S.; Baldi, P.; Bambah, B.; Barao, F.; Barenboim, G.; Barker, G. J.; Barkhouse, W.; Barnes, C.; Barr, G.; Barranco Monarca, J.; Barros, N.; Barrow, J. L.; Bashyal, A.; Basque, V.; Bay, F.; Alba, J. L. Bazo; Beacom, J. F.; Bechetoille, E.; Behera, B.; Bellantoni, L.; Bellettini, G.; Bellini, V.; Beltramello, O.; Belver, D.; Benekos, N.; Bento Neves, F.; Berger, J.; Berkman, S.; Bernardini, P.; Berner, R. M.; Berns, H.; Bertolucci, S.; Betancourt, M.; Bezawada, Y.; Bhattacharjee, M.; Bhuyan, B.; Biagi, S.; Bian, J.; Biassoni, M.; Biery, K.; Bilki, B.; Bishai, M.; Bitadze, A.; Blake, A.; Blanco Siffert, B.; Blaszczyk, F. D. M.; Blazey, G. C.; Blucher, E.; Boissevain, J.; Bolognesi, S.; Bolton, T.; Bonesini, M.; Bongrand, M.; Bonini, F.; Booth, A.; Booth, C.; Bordoni, S.; Borkum, A.; Boschi, T.; Bostan, N.; Bour, P.; Boyd, S. B.; Boyden, D.; Bracinik, J.; Braga, D.; Brailsford, D.; Brandt, A.; Bremer, J.; Brew, C.; Brianne, E.; Brice, S. J.; Brizzolari, C.; Bromberg, C.; Brooijmans, G.; Brooke, J.; Bross, A.; Brunetti, G.; Buchanan, N.; Budd, H.; Caiulo, D.; Calafiura, P.; Calcutt, J.; Calin, M.; Calvez, S.; Calvo, E.; Camilleri, L.; Caminata, A.; Campanelli, M.; Caratelli, D.; Carini, G.; Carlus, B.; Carniti, P.; Caro Terrazas, I.; Carranza, H.; Castillo, A.; Castromonte, C.; Cattadori, C.; Cavalier, F.; Cavanna, F.; Centro, S.; Cerati, G.; Cervelli, A.; Cervera Villanueva, A.; Chalifour, M.; Chang, C.; Chardonnet, E.; Chatterjee, A.; Chattopadhyay, S.; Chaves, J.; Chen, H.; Chen, M.; Chen, Y.; Cherdack, D.; Chi, C.; Childress, S.; Chiriacescu, A.; Cho, K.; Choubey, S.; Christensen, A.; Christian, D.; Christodoulou, G.; Church, E.; Clarke, P.; Coan, T. E.; Cocco, A. G.; Coelho, J. A. B.; Conley, E.; Conrad, J. M.; Convery, M.; Corwin, L.; Cotte, P.; Cremaldi, L.; Cremonesi, L.; Crespo-Anadón, J. I.; Cristaldo, E.; Cross, R.; Cuesta, C.; Cui, Y.; Cussans, D.; Dabrowski, M.; da Motta, H.; Da Silva Peres, L.; David, C.; David, Q.; Davies, G. S.; Davini, S.; Dawson, J.; De, K.; De Almeida, R. M.; Debbins, P.; De Bonis, I.; Decowski, M. P.; de Gouvêa, A.; De Holanda, P. C.; De Icaza Astiz, I. L.; Deisting, A.; De Jong, P.; Delbart, A.; Delepine, D.; Delgado, M.; Dell-Acqua, A.; De Lurgio, P.; de Mello Neto, J. R. T.; DeMuth, D. M.; Dennis, S.; Densham, C.; Deptuch, G.; De Roeck, A.; De Romeri, V.; De Vries, J. J.; Dharmapalan, R.; Dias, M.; Diaz, F.; Díaz, J. S.; Di Domizio, S.; Di Giulio, L.; Ding, P.; Di Noto, L.; Distefano, C.; Diurba, R.; Diwan, M.; Djurcic, Z.; Dokania, N.; Dolinski, M. J.; Domine, L.; Douglas, D.; Drielsma, F.; Duchesneau, D.; Duffy, K.; Dunne, P.; Durkin, T.; Duyang, H.; Dvornikov, O.; Dwyer, D. A.; Dyshkant, A. S.; Eads, M.; Edmunds, D.; Eisch, J.; Emery, S.; Ereditato, A.; Escobar, C. O.; Escudero Sanchez, L.; Evans, J. J.; Ewart, E.; Ezeribe, A. C.; Fahey, K.; Falcone, A.; Farnese, C.; Farzan, Y.; Felix, J.; Fernandez-Martinez, E.; Fernandez Menendez, P.; Ferraro, F.; Fields, L.; Filkins, A.; Filthaut, F.; Fitzpatrick, R. S.; Flanagan, W.; Fleming, B.; Flight, R.; Fowler, J.; Fox, W.; Franc, J.; Francis, K.; Franco, D.; Freeman, J.; Freestone, J.; Fried, J.; Friedland, A.; Fuess, S.; Furic, I.; Furmanski, A. P.; Gago, A.; Gallagher, H.; Gallego-Ros, A.; Gallice, N.; Galymov, V.; Gamberini, E.; Gamble, T.; Gandhi, R.; Gandrajula, R.; Gao, S.; Garcia-Gamez, D.; García-Peris, M. Á.; Gardiner, S.; Gastler, D.; Ge, G.; Gelli, B.; Gendotti, A.; Gent, S.; Ghorbani-Moghaddam, Z.; Gibin, D.; Gil-Botella, I.; Girerd, C.; Giri, A. K.; Gnani, D.; Gogota, O.; Gold, M.; Gollapinni, S.; Gollwitzer, K.; Gomes, R. A.; Gomez Bermeo, L. V.; Gomez Fajardo, L. S.; Gonnella, F.; Gonzalez-Cuevas, J. A.; Goodman, M. C.; Goodwin, O.; Goswami, S.; Gotti, C.; Goudzovski, E.; Grace, C.; Graham, M.; Gramellini, E.; Gran, R.; Granados, E.; Grant, A.; Grant, C.; Gratieri, D.; Green, P.; Green, S.; Greenler, L.; Greenwood, M.; Greer, J.; Griffith, W. C.; Groh, M.; Grudzinski, J.; Grzelak, K.; Gu, W.; Guarino, V.; Guenette, R.; Guglielmi, A.; Guo, B.; Guthikonda, K. K.; Gutierrez, R.; Guzowski, P.; Guzzo, M. M.; Gwon, S.; Habig, A.; Hackenburg, A.; Hadavand, H.; Haenni, R.; Hahn, A.; Haigh, J.; Haiston, J.; Hamernik, T.; Hamilton, P.; Han, J.; Harder, K.; Harris, D. A.; Hartnell, J.; Hasegawa, T.; Hatcher, R.; Hazen, E.; Heavey, A.; Heeger, K. M.; Heise, J.; Hennessy, K.; Henry, S.; Hernandez Morquecho, M. A.; Herner, K.; Hertel, L.; Hesam, A. S.; Hewes, J.; Higuera, A.; Hill, T.; Hillier, S. J.; Himmel, A.; Hoff, J.; Hohl, C.; Holin, A.; Hoppe, E.; Horton-Smith, G. A.; Hostert, M.; Hourlier, A.; Howard, B.; Howell, R.; Huang, J.; Huang, J.; Hugon, J.; Iles, G.; Ilic, N.; Iliescu, A. M.; Illingworth, R.; Ioannisian, A.; Itay, R.; Izmaylov, A.; James, E.; Jargowsky, B.; Jediny, F.; Jesùs-Valls, C.; Ji, X.; Jiang, L.; Jiménez, S.; Jipa, A.; Joglekar, A.; Johnson, C.; Johnson, R.; Jones, B.; Jones, S.; Jung, C. K.; Junk, T.; Jwa, Y.; Kabirnezhad, M.; Kaboth, A.; Kadenko, I.; Kamiya, F.; Karagiorgi, G.; Karcher, A.; Karolak, M.; Karyotakis, Y.; Kasai, S.; Kasetti, S. P.; Kashur, L.; Kazaryan, N.; Kearns, E.; Keener, P.; Kelly, K. J.; Kemp, E.; Ketchum, W.; Kettell, S. H.; Khabibullin, M.; Khotjantsev, A.; Khvedelidze, A.; Kim, D.; King, B.; Kirby, B.; Kirby, M.; Klein, J.; Koehler, K.; Koerner, L. W.; Kohn, S.; Koller, P. P.; Kordosky, M.; Kosc, T.; Kose, U.; Kostelecký, V. A.; Kothekar, K.; Krennrich, F.; Kreslo, I.; Kudenko, Y.; Kudryavtsev, V. A.; Kulagin, S.; Kumar, J.; Kumar, R.; Kuruppu, C.; Kus, V.; Kutter, T.; Lambert, A.; Lande, K.; Lane, C. E.; Lang, K.; Langford, T.; Lasorak, P.; Last, D.; Lastoria, C.; Laundrie, A.; Lawrence, A.; Lazanu, I.; LaZur, R.; Le, T.; Learned, J.; LeBrun, P.; Lehmann Miotto, G.; Lehnert, R.; Leigui de Oliveira, M. A.; Leitner, M.; Leyton, M.; Li, L.; Li, S.; Li, S. W.; Li, T.; Li, Y.; Liao, H.; Lin, C. S.; Lin, S.; Lister, A.; Littlejohn, B. R.; Liu, J.; Lockwitz, S.; Loew, T.; Lokajicek, M.; Lomidze, I.; Long, K.; Loo, K.; Lorca, D.; Lord, T.; LoSecco, J. M.; Louis, W. C.; Luk, K. B.; Luo, X.; Lurkin, N.; Lux, T.; Luzio, V. P.; MacFarland, D.; Machado, A. A.; Machado, P.; Macias, C. T.; Macier, J. R.; Maddalena, A.; Madigan, P.; Magill, S.; Mahn, K.; Maio, A.; Major, A.; Maloney, J. A.; Mandrioli, G.; Maneira, J.; Manenti, L.; Manly, S.; Mann, A.; Manolopoulos, K.; Manrique Plata, M.; Marchionni, A.; Marciano, W.; Marfatia, D.; Mariani, C.; Maricic, J.; Marinho, F.; Marino, A. D.; Marshak, M.; Marshall, C.; Marshall, J.; Marteau, J.; Martin-Albo, J.; Martinez, N.; Martinez Caicedo, D. A.; Martynenko, S.; Mason, K.; Mastbaum, A.; Masud, M.; Matsuno, S.; Matthews, J.; Mauger, C.; Mauri, N.; Mavrokoridis, K.; Mazza, R.; Mazzacane, A.; Mazzucato, E.; McCluskey, E.; McConkey, N.; McFarland, K. S.; McGrew, C.; McNab, A.; Mefodiev, A.; Mehta, P.; Melas, P.; Mellinato, M.; Mena, O.; Menary, S.; Mendez, H.; Menegolli, A.; Meng, G.; Messier, M. D.; Metcalf, W.; Mewes, M.; Meyer, H.; Miao, T.; Michna, G.; Miedema, T.; Migenda, J.; Milincic, R.; Miller, W.; Mills, J.; Milne, C.; Mineev, O.; Miranda, O. G.; Miryala, S.; Mishra, C. S.; Mishra, S. R.; Mislivec, A.; Mladenov, D.; Mocioiu, I.; Moffat, K.; Moggi, N.; Mohanta, R.; Mohayai, T. A.; Mokhov, N.; Molina, J.; Molina Bueno, L.; Montanari, A.; Montanari, C.; Montanari, D.; Montano Zetina, L. M.; Moon, J.; Mooney, M.; Moor, A.; Moreno, D.; Morgan, B.; Morris, C.; Mossey, C.; Motuk, E.; Moura, C. A.; Mousseau, J.; Mu, W.; Mualem, L.; Mueller, J.; Muether, M.; Mufson, S.; Muheim, F.; Muir, A.; Mulhearn, M.; Muramatsu, H.; Murphy, S.; Musser, J.; Nachtman, J.; Nagu, S.; Nalbandyan, M.; Nandakumar, R.; Naples, D.; Narita, S.; Navas-Nicolás, D.; Nayak, N.; Nebot-Guinot, M.; Necib, L.; Negishi, K.; Nelson, J. K.; Nesbit, J.; Nessi, M.; Newbold, D.; Newcomer, M.; Newhart, D.; Nichol, R.; Niner, E.; Nishimura, K.; Norman, A.; Norrick, A.; Northrop, R.; Novella, P.; Nowak, J. A.; Oberling, M.; Olivares Del Campo, A.; Olivier, A.; Onel, Y.; Onishchuk, Y.; Ott, J.; Pagani, L.; Pakvasa, S.; Palamara, O.; Palestini, S.; Paley, J. M.; Pallavicini, M.; Palomares, C.; Pantic, E.; Paolone, V.; Papadimitriou, V.; Papaleo, R.; Papanestis, A.; Paramesvaran, S.; Parke, S.; Parsa, Z.; Parvu, M.; Pascoli, S.; Pasqualini, L.; Pasternak, J.; Pater, J.; Patrick, C.; Patrizii, L.; Patterson, R. B.; Patton, S. J.; Patzak, T.; Paudel, A.; Paulos, B.; Paulucci, L.; Pavlovic, Z.; Pawloski, G.; Payne, D.; Pec, V.; Peeters, S. J. M.; Penichot, Y.; Pennacchio, E.; Penzo, A.; Peres, O. L. G.; Perry, J.; Pershey, D.; Pessina, G.; Petrillo, G.; Petta, C.; Petti, R.; Piastra, F.; Pickering, L.; Pietropaolo, F.; Pillow, J.; Pinzino, J.; Plunkett, R.; Poling, R.; Pons, X.; Poonthottathil, N.; Pordes, S.; Potekhin, M.; Potenza, R.; Potukuchi, B. V. K. S.; Pozimski, J.; Pozzato, M.; Prakash, S.; Prakash, T.; Prince, S.; Prior, G.; Pugnere, D.; Qi, K.; Qian, X.; Raaf, J. L.; Raboanary, R.; Radeka, V.; Rademacker, J.; Radics, B.; Rafique, A.; Raguzin, E.; Rai, M.; Rajaoalisoa, M.; Rakhno, I.; Rakotondramanana, H. T.; Rakotondravohitra, L.; Ramachers, Y. A.; Rameika, R.; Ramirez Delgado, M. A.; Ramson, B.; Rappoldi, A.; Raselli, G.; Ratoff, P.; Ravat, S.; Razafinime, H.; Real, J. S.; Rebel, B.; Redondo, D.; Reggiani-Guzzo, M.; Rehak, T.; Reichenbacher, J.; Reitzner, S. D.; Renshaw, A.; Rescia, S.; Resnati, F.; Reynolds, A.; Riccobene, G.; Rice, L. C. J.; Rielage, K.; Rigaut, Y.; Rivera, D.; Rochester, L.; Roda, M.; Rodrigues, P.; Rodriguez Alonso, M. J.; Rodriguez Rondon, J.; Roeth, A. J.; Rogers, H.; Rosauro-Alcaraz, S.; Rossella, M.; Rout, J.; Roy, S.; Rubbia, A.; Rubbia, C.; Russell, B.; Russell, J.; Ruterbories, D.; Saakyan, R.; Sacerdoti, S.; Safford, T.; Sahu, N.; Sala, P.; Samios, N.; Sanchez, M. C.; Sanders, D. A.; Sankey, D.; Santana, S.; Santos-Maldonado, M.; Saoulidou, N.; Sapienza, P.; Sarasty, C.; Sarcevic, I.; Savage, G.; Savinov, V.; Scaramelli, A.; Scarff, A.; Scarpelli, A.; Schaffer, T.; Schellman, H.; Schlabach, P.; Schmitz, D.; Scholberg, K.; Schukraft, A.; Segreto, E.; Sensenig, J.; Seong, I.; Sergi, A.; Sergiampietri, F.; Sgalaberna, D.; Shaevitz, M. H.; Shafaq, S.; Shamma, M.; Sharma, H. R.; Sharma, R.; Shaw, T.; Shepherd-Themistocleous, C.; Shin, S.; Shooltz, D.; Shrock, R.; Simard, L.; Simos, N.; Sinclair, J.; Sinev, G.; Singh, J.; Singh, J.; Singh, V.; Sipos, R.; Sippach, F. W.; Sirri, G.; Sitraka, A.; Siyeon, K.; Smargianaki, D.; Smith, A.; Smith, E.; Smith, P.; Smolik, J.; Smy, M.; Snopok, P.; Soares Nunes, M.; Sobel, H.; Soderberg, M.; Solano Salinas, C. J.; Söldner-Rembold, S.; Solomey, N.; Solovov, V.; Sondheim, W. E.; Sorel, M.; Soto-Oton, J.; Sousa, A.; Soustruznik, K.; Spagliardi, F.; Spanu, M.; Spitz, J.; Spooner, N. J. C.; Spurgeon, K.; Staley, R.; Stancari, M.; Stanco, L.; Steiner, H. M.; Stewart, J.; Stillwell, B.; Stock, J.; Stocker, F.; Stokes, T.; Strait, M.; Strauss, T.; Striganov, S.; Stuart, A.; Summers, D.; Surdo, A.; Susic, V.; Suter, L.; Sutera, C. M.; Svoboda, R.; Szczerbinska, B.; Szelc, A. M.; Talaga, R.; Tanaka, H. A.; Tapia Oregui, B.; Tapper, A.; Tariq, S.; Tatar, E.; Tayloe, R.; Teklu, A. M.; Tenti, M.; Terao, K.; Ternes, C. A.; Terranova, F.; Testera, G.; Thea, A.; Thompson, J. L.; Thorn, C.; Timm, S. C.; Tonazzo, A.; Torti, M.; Tórtola, M.; Tortorici, F.; Totani, D.; Toups, M.; Touramanis, C.; Trevor, J.; Trzaska, W. H.; Tsai, Y. T.; Tsamalaidze, Z.; Tsang, K. V.; Tsverava, N.; Tufanli, S.; Tull, C.; Tyley, E.; Tzanov, M.; Uchida, M. A.; Urheim, J.; Usher, T.; Vagins, M. R.; Vahle, P.; Valdiviesso, G. A.; Valencia, E.; Vallari, Z.; Valle, J. W. F.; Vallecorsa, S.; Van Berg, R.; Van de Water, R. G.; Vanegas Forero, D.; Varanini, F.; Vargas, D.; Varner, G.; Vasel, J.; Vasseur, G.; Vaziri, K.; Ventura, S.; Verdugo, A.; Vergani, S.; Vermeulen, M. A.; Verzocchi, M.; Vieira de Souza, H.; Vignoli, C.; Vilela, C.; Viren, B.; Vrba, T.; Wachala, T.; Waldron, A. V.; Wallbank, M.; Wang, H.; Wang, J.; Wang, Y.; Wang, Y.; Warburton, K.; Warner, D.; Wascko, M.; Waters, D.; Watson, A.; Weatherly, P.; Weber, A.; Weber, M.; Wei, H.; Weinstein, A.; Wenman, D.; Wetstein, M.; While, M. R.; White, A.; Whitehead, L. H.; Whittington, D.; Wilking, M. J.; Wilkinson, C.; Williams, Z.; Wilson, F.; Wilson, R. J.; Wolcott, J.; Wongjirad, T.; Wood, K.; Wood, L.; Worcester, E.; Worcester, M.; Wret, C.; Wu, W.; Wu, W.; Xiao, Y.; Yang, G.; Yang, T.; Yershov, N.; Yonehara, K.; Young, T.; Yu, B.; Yu, J.; Zaki, R.; Zalesak, J.; Zambelli, L.; Zamorano, B.; Zani, A.; Zazueta, L.; Zeller, G. P.; Zennamo, J.; Zeug, K.; Zhang, C.; Zhao, M.; Zhivun, E.; Zhu, G.; Zimmerman, E. D.; Zito, M.; Zucchelli, S.; Zuklin, J.; Zutshi, V.; Zwaska, R. Bibcode: 2021EPJC...81..423A Altcode: 2020arXiv200806647D; 2020arXiv200806647A The deep underground neutrino experiment (DUNE), a 40-kton underground liquid argon time projection chamber experiment, will be sensitive to the electron-neutrino flavor component of the burst of neutrinos expected from the next Galactic core-collapse supernova. Such an observation will bring unique insight into the astrophysics of core collapse as well as into the properties of neutrinos. The general capabilities of DUNE for neutrino detection in the relevant few- to few-tens-of-MeV neutrino energy range will be described. As an example, DUNE's ability to constrain the νe spectral parameters of the neutrino burst will be considered. Title: Space missions for astronomy and astrophysics in Korea: past, present, and future Authors: Seon, Kwang-Il; Han, Wonyong; Lee, Young-Wook; Lee, Hyung Mok; Kim, Min Bin; Park, I. H.; Jeong, Woong-Seob; Cho, Kyung-Suk; Lee, Jae Jin; Lee, Dae-Hee; Kwak, Kyujin Bibcode: 2021JKPS...78..942S Altcode: 2021JKPS..tmp..132S; 2020arXiv201201120S We review the history of space missions in Korea focusing on the field of astronomy and astrophysics. For each mission, scientific motivation and achievement are reviewed together with some technical details of the program, including mission schedule. This review includes ongoing and currently approved missions, as well as some planned ones. Within the admitted limitations of the authors' perspectives, some comments on the future direction of the space program for astronomy and astrophysics in Korea are made at the end of this review. Title: Comparison of LOS Doppler Velocities and Non-thermal Line Widths in the Off-limb Solar Corona Measured Simultaneously by CoMP and Ninode/EIS Authors: Lee, Jae-Ok; Lee, Kyoung-Sun; Seough, Jungjoon; Cho, Kyung-Suk Bibcode: 2021JKAS...54...49L Altcode: Observations of line of sight (LOS) Doppler velocity and non-thermal line width in the off-limb solar corona are often used for investigating the Alfvén wave signatures in the corona. In this study, we compare LOS Doppler velocities and non-thermal line widths obtained simultaneously from two different instruments, Coronal Multichannel Polarimeter (CoMP) and Hinode/EUV Imaging Spectrometer (EIS), on various off-limb coronal regions: flaring and quiescent active regions, equatorial quiet region, and polar prominence and plume regions observed in 2012-2014. CoMP provides the polarization at the Fe XIII 10747 Å coronal forbidden lines which allows their spectral line intensity, LOS Doppler velocity, and line width to be measured with a low spectral resolution of 1.2 Å in 2-D off limb corona between 1.05 and 1.40 R_Sun, while Hinode/EIS gives us the EUV spectral information with a high spectral resolution (0.025 Å) in a limited field of view raster scan. In order to compare them,
we make pseudo raster scan CoMP maps using information of each EIS scan slit time and position. We compare the CoMP and EIS spectroscopic maps by visual inspection, and examine their pixel to pixel correlations and percentages of pixel numbers satisfying the condition that the differences between CoMP and EIS spectroscopic quantities are within the EIS measurement accuracy: ±3 km/s for LOS Doppler velocity and ±9 km/s for non-thermal width. The main results are summarized as follows. By comparing CoMP and EIS Doppler velocity distributions, we find that they are consistent with each other overall in the active regions and equatorial quiet region (0.25 ≤ CC ≤ 0.7), while they are partially similar to each other in the overlying loops of prominences and near the bottom of the polar plume (0.02 ≤ CC ≤ 0.18). CoMP Doppler velocities are consistent with the EIS ones within the EIS measurement accuracy in most regions (≥ 87% of pixels) except for the polar region (45% of pixels). We find that CoMP and EIS non-thermal width distributions are similar overall in the active regions (0.06 ≤ CC ≤ 0.61), while they seem to be different in the others (-0.1 ≤ CC ≤ 0.00). CoMP non-thermal widths are similar to EIS ones within the EIS measurement accuracy in a quiescent active region (79% of pixels), while they do not match in the other regions (≤ 61% of pixels); the CoMP observations tend to underestimate the widths by about 20% to 40% compared to the EIS ones. Our results demonstrate that CoMP observations can provide reliable 2-D LOS Doppler velocity distributions on active regions and might provide their non-thermal width distributions. Title: Kinematic Oscillations of Post-CME Blobs Detected by K-Cor on 2017 September 10 Authors: Lee, Jae-Ok; Cho, Kyung-Suk; Nakariakov, Valery M.; Lee, Harim; Kim, Rok-Soon; Jang, Soojeong; Yang, Heesu; Kim, Sujin; Kim, Yeon-Han Bibcode: 2021JKAS...54...61L Altcode: We investigate 20 post-coronal mass ejection (CME) blobs formed in the post-CME current sheet (CS) that were observed by K-Cor on 2017 September 10. By visual inspection of the trajectories and projected speed variations of each blob, we find that all blobs except one show irregular "zigzag" trajectories resembling transverse oscillatory motions along the CS, and have at least one oscillatory pattern in their instantaneous radial speeds. Their oscillation periods are ranging from 30 to 91 s and their speed amplitudes from 128 to 902 km/s. Among 19 blobs, 10 blobs have experienced at least two cycles of radial speed oscillations with different speed amplitudes and periods, while 9 blobs undergo one oscillation cycle. To examine whether or not the apparent speed oscillations can be explained by vortex shedding, we estimate the quantitative parameter of vortex shedding, the Strouhal number, by using the observed lateral widths, linear speeds, and oscillation periods of the blobs. We then compare our estimates with theoretical and experimental results from MHD simulations and fluid dynamics experiments. We find that the observed Strouhal numbers range from 0.2 to 2.1, consistent with those (0.15-3.0) from fluid dynamics experiments of bluff spheres, while they are higher than those (0.15-0.25) from MHD simulations of cylindrical shapes. We thus find that blobs formed in a post-CME CS undergo kinematic oscillations caused by fluid dynamic vortex shedding. The vortex shedding is driven by the interaction of the outward-moving blob having a bluff spherical shape with the background plasma in the post-CME CS. Title: On the Nature of Propagating Intensity Disturbances in Polar Plumes during the 2017 Total Solar Eclipse Authors: Cho, Kyung-Suk; Cho, Il-Hyun; Madjarska, Maria S.; Nakariakov, Valery M.; Yang, Heesu; Choi, Seonghwan; Lim, Eun-Kyung; Lee, Kyung-Sun; Seough, Jung-Jun; Lee, Jaeok; Kim, Yeon-Han Bibcode: 2021ApJ...909..202C Altcode: 2021arXiv210202085C The propagating intensity disturbances (PIDs) in plumes are still poorly understood, and their identity (magnetoacoustic waves or flows) remains an open question. We investigate PIDs in five plumes located in the northern polar coronal hole observed during the 2017 total solar eclipse. Three plumes are associated with coronal bright points, jets, and macrospicules at their base (active plumes), and the other two plumes are not (quiet plumes). The electron temperature at the base of the plumes is obtained from the filter ratio of images taken with the X-ray Telescope on board Hinode and the passband ratio around 400 nm from an eclipse instrument, the Diagnostic Coronagraph Experiment. The phase speed (vr), frequency (ω), and wavenumber (k) of the PIDs in the plumes are obtained by applying a Fourier transformation to the spacetime (r - t plane) plots in images taken with the Atmospheric Imaging Assembly (AIA) in three different wavelength channels (171, 193, and 211 Å). We found that the PIDs in the higher-temperature AIA channels, 193 and 211 Å, are faster than that of the cooler AIA 171 Å channel. This tendency is more significant for the active plumes than the quiet ones. The observed speed ratio (∼1.3) between the AIA 171 and 193 Å channels is similar to the theoretical value (1.25) of a slow magnetoacoustic wave. Our results support the idea that PIDs in plumes represent a superposition of slow magnetoacoustic waves and plasma outflows that consist of dense cool flows and hot coronal jets. Title: The Balloon-Borne Investigation of Temperature and Speed of Electrons in the Corona (BITSE): Mission Description and Preliminary Results Authors: Gopalswamy, N.; Newmark, J.; Yashiro, S.; Mäkelä, P.; Reginald, N.; Thakur, N.; Gong, Q.; Kim, Y. -H.; Cho, K. -S.; Choi, S. -H.; Baek, J. -H.; Bong, S. -C.; Yang, H. -S.; Park, J. -Y.; Kim, J. -H.; Park, Y. -D.; Lee, J. -O.; Kim, R. -S.; Lim, E. -K. Bibcode: 2021SoPh..296...15G Altcode: 2020arXiv201106111G We report on the Balloon-borne Investigation of Temperature and Speed of Electrons in the corona (BITSE) mission launched recently to observe the solar corona from ≈3 Rs to 15 Rs at four wavelengths (393.5, 405.0, 398.7, and 423.4 nm). The BITSE instrument is an externally occulted single stage coronagraph developed at NASA's Goddard Space Flight Center in collaboration with the Korea Astronomy and Space Science Institute (KASI). BITSE used a polarization camera that provided polarization and total brightness images of size 1024 ×1024 pixels. The Wallops Arc Second Pointer (WASP) system developed at NASA's Wallops Flight Facility (WFF) was used for Sun pointing. The coronagraph and WASP were mounted on a gondola provided by WFF and launched from the Fort Sumner, New Mexico station of Columbia Scientific Balloon Facility (CSBF) on September 18, 2019. BITSE obtained 17,060 coronal images at a float altitude of ≈128,000 feet (≈39 km) over a period of ≈4 hrs. BITSE flight software was based on NASA's core Flight System, which was designed to help develop flight quality software. We used EVTM (Ethernet Via Telemetry) to download science data during operations; all images were stored on board using flash storage. At the end of the mission, all data were recovered and analyzed. Preliminary analysis shows that BITSE imaged the solar minimum corona with the equatorial streamers on the east and west limbs. The narrow streamers observed by BITSE are in good agreement with the geometric properties obtained by the Solar and Heliospheric Observatory (SOHO) coronagraphs in the overlapping physical domain. In spite of the small signal-to-noise ratio (≈14 ) we were able to obtain the temperature and flow speed of the western steamer. In the heliocentric distance range 4 - 7 Rs on the western streamer, we obtained a temperature of ≈1.0 ±0.3 MK and a flow speed of ≈260 km s−1 with a large uncertainty interval. Title: Understanding Formative Winds of Intracrater Aeolian Dunes on Mars Authors: Cho, K.; Gunn, A.; Jerolmack, D. J. Bibcode: 2020AGUFMEP0180005C Altcode: The modern Martian landscape is primarily dominated by aeolian processes, with dune migrations and sand fluxes comparable to terrestrial values. Despite the significantly lower atmospheric density, many of the same Earth-wind processes and transport laws still apply. Mars is also punctuated with thousands of craters, many containing active dune fields, ripples, and other aeolian landforms. Wind patterns and sediment supply within these craters determine the shape, size, and migration patterns of these dunes. Here we study the end-member atmospheric phenomena that produce these intracrater dunes: katabatic and convective winds. Both are caused by the daily heating and cooling of the near-surface atmosphere, with the former produced by nocturnal gravity flows along crater walls, and the latter by extreme free convection in the afternoon allowing geostrophic momentum transfer to the dunes. Dune orientations collected from NASA's High Resolution Imaging Experiment (HiRISE), which serve as proxies for local wind direction, are compared to slope flow directions inferred from the Mars Orbiter Laser Altimeter (MOLA) and simulated large-scale regional wind directions from the Mars Climate Database (MCD). We find no clear global preferential alignment towards either local slope flows, or non-local climate wind. We develop a simple theory for katabatic flow and the impact threshold of sediment transport, and use it to examine the propensity for katabatic vs. climatic flows to move sand. This theory reveals the relative importance of each in terms of their contribution to dune orientations on Mars. We find that latitude and seasonality play important roles in forming the aeolian dunes that inhabit Martian craters. Title: The Coronal Diagnostic Experiment (CODEX) Authors: Newmark, J. S.; Gopalswamy, N.; Kim, Y. H.; Viall, N. M.; Cho, K. S. F.; Reginald, N. L.; Bong, S. C.; Gong, Q.; Choi, S.; Strachan, L.; Yashiro, S. Bibcode: 2020AGUFMSH0280011N Altcode: Understanding solar wind sources and acceleration mechanisms is an overarching solar physics goal. Current models are highly under-constrained due to the limitations of the existing data, particularly in the ~3-10 Rs range. COronal Diagnostic EXperiment (CODEX) is designed to deliver the first global, comprehensive data sets that will impose crucial constraints and answer targeted essential questions, including: Are there signatures of hot plasma released into the solar wind from previously closed fields? What are the velocities and temperatures of the density structures that are observed so ubiquitously within streamers and coronal holes? To provide these crucial measurements, NASA's Goddard Space Flight Center, in collaboration with the Korea Astronomy and Space Science Institute, will develop a next-generation coronagraph for the International Space Station. This imaging coronagraph uses multiple filters to obtain simultaneous measurements of electron density, temperature, and velocity within a single instrument. This will be the first time all three have been measured simultaneously for this critical field-of-view, and CODEX achieves these measurements multiple times a day. Title: Accelerating and Supersonic Density Disturbances in Solar Polar Plumes Authors: Cho, I. H.; Moon, Y. J.; Nakariakov, V. M.; Lee, J. Y.; Yu, D. J.; Cho, K. S. F.; Yurchyshyn, V.; Lee, H. Bibcode: 2020AGUFMSH0290003C Altcode: Propagating intensity disturbances in solar coronal holes are often considered as wave propagations or mass flows. By applying the differential emission measure technique for the extreme ultraviolet images taken by the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory, we analyze the propagation speed of density disturbances of plume structure in an off-limb coronal hole for a given temperature. We construct the map of cross-correlation between density profile for a given height and the profile at the height of 50 Mm. The evolution of density disturbances is well fitted by the second-order polynomial. The acceleration is calculated to be 36 m s-2. The initial speed is 134 km s-1 which is comparable with the sound speed given by the DEM-weighted temperature. Hence, density disturbances are accelerating and supersonic at around the base of the solar corona. The excess speed relative to the sound speed is ∼ 30 km s-1 at the height of 1.23 solar radii, which is consistent with the Doppler speeds and Doppler dimming speeds observed by different instruments. The extrapolated sonic distance of the excess speed is ∼ 2.16 solar radii which is consistent with those of solar winds. The lower limit of the mass flux corresponds to 7% of the global solar wind. Hence, we interpret that the observed density disturbances are slow magnetoacoustic waves propagating in subsonic and accelerating solar winds. Title: Accelerating and Supersonic Density Fluctuations in Coronal Hole Plumes: Signature of Nascent Solar Winds Authors: Cho, Il-Hyun; Nakariakov, Valery M.; Moon, Yong-Jae; Lee, Jin-Yi; Yu, Dae Jung; Cho, Kyung-Suk; Yurchyshyn, Vasyl; Lee, Harim Bibcode: 2020ApJ...900L..19C Altcode: 2020arXiv200807848C Slow magnetoacoustic waves in a static background provide a seismological tool to probe the solar atmosphere in the analytic frame. By analyzing the spatiotemporal variation of the electron number density of plume structure in coronal holes above the limb for a given temperature, we find that the density perturbations accelerate with supersonic speeds in the distance range from 1.02 to 1.23 solar radii. We interpret them as slow magnetoacoustic waves propagating at about the sound speed with accelerating subsonic flows. The average sonic height of the subsonic flows is calculated to be 1.27 solar radii. The mass flux of the subsonic flows is estimated to be 44.1% relative to the global solar wind. Hence, the subsonic flow is likely to be the nascent solar wind. In other words, the evolution of the nascent solar wind in plumes at the low corona is quantified for the first time from imaging observations. Based on the interpretation, propagating density perturbations present in plumes could be used as a seismological probe of the gradually accelerating solar wind. Title: Toward a Next Generation Solar Coronagraph: Diagnostic Coronagraph Experiment Authors: Cho, Kyung-Suk; Yang, Heesu; Lee, Jae-Ok; Bong, Su-Chan; Kim, Jihun; Choi, Seonghwan; Park, Jongyeob; Cho, Kyuhoun; Baek, Ji-Hye; Kim, Yeon-Han; Park, Young-Deuk Bibcode: 2020JKAS...53...87C Altcode: 2020arXiv200606155C The Korea Astronomy and Space Science Institute (KASI) has been developing a next-generation coronagraph (NGC) in cooperation with NASA to measure the coronal electron density, temperature, and speed simultaneously, using four different optical filters around 400 nm. KASI organized an expedition to demonstrate the coronagraph measurement scheme and the instrumental technology during the 2017 total solar eclipse (TSE) across the USA. The observation site was in Jackson Hole, Wyoming, USA. We built an eclipse observation system, the Diagnostic Coronal Experiment (DICE), composed of two identical telescopes to improve the signal-to-noise ratio. The observation was conducted at four wavelengths and three linear polarization directions in the limited total eclipse time of about 140 seconds. We successfully obtained polarization data for the corona but we were not able to obtain information on the coronal electron temperature and speed due to the low signal-to-noise ratio of the optical system and strong emission from prominences located at the western limb. In this study, we report the development of DICE and the observation results from the eclipse expedition. TSE observation and analysis with our self-developed instrument showed that a coronagraph needs to be designed carefully to achieve its scientific purpose. We gained valuable experience for future follow-up NASA-KASI joint missions: the Balloon-borne Investigation of the Temperature and Speed of Electrons in the Corona (BITSE) and the COronal Diagnostic EXperiment (CODEX). Title: The Application of the Filtered Backprojection Algorithm to Solar Rotational Tomography Authors: Cho, Kyuhyoun; Chae, Jongchul; Kwon, Ryun-Young; Bong, Su-Chan; Cho, Kyung-Suk Bibcode: 2020ApJ...895...55C Altcode: 2020arXiv200506388C Solar rotational tomography (SRT) is an important method to reconstruct the physical parameters of the three-dimensional solar corona. Here we propose an approach to apply the filtered backprojection (FBP) algorithm to the SRT. The FBP algorithm is generally not suitable for SRT due to the several issues with solar extreme ultraviolet (EUV) observations—in particular, a problem caused by missing data because of the unobserved back side of corona hidden behind the Sun. We developed a method to generate a modified sinogram that resolves the blocking problem. The modified sinogram is generated by combining the EUV data at two opposite sites observed by the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory (SDO). We generated the modified sinogram for about one month in 2019 February and reconstructed the three-dimensional corona under the static state assumption. In order to obtain the physical parameters of the corona, we employed a differential emission measure inversion method. We tested the performance of the FBP algorithm with the modified sinogram by comparing the reconstructed data with the observed EUV image, electron density models, previous studies of electron temperature, and an observed coronagraph image. The results illustrate that the FBP algorithm reasonably reconstructs the bright regions and the coronal holes and can reproduce their physical parameters. The main advantage of the FBP algorithm is that it is easy to understand and computationally efficient. Thus, it enables us to easily probe the inhomogeneous coronal electron density and temperature distribution of the solar corona. Title: Formation of Post-CME Blobs Observed by LASCO-C2 and K-Cor on 2017 September 10 Authors: Lee, Jae-Ok; Cho, Kyung-Suk; Lee, Kyoung-Sun; Cho, Il-Hyun; Lee, Junggi; Miyashita, Yukinaga; Kim, Yeon-Han; Kim, Rok-Soon; Jang, Soojeong Bibcode: 2020ApJ...892..129L Altcode: Understanding the formation of post-CME blobs, we investigate 2 blobs in the outer corona observed by LASCO-C2 and 34 blobs in the inner corona by K-Cor on 2017 September 10 from 17:11 to 18:58 UT. By visual inspection of the structure of a post-CME current sheet (CS) and its associated blobs, we find that the CS is well identified in the K-Cor and its radial lengths are nine times longer than lateral widths, indicating the CS is unstable to the linear tearing mode. The inner corona blobs can be classified into two groups: 27 blobs generated in the middle of the CS (Group 1) and 7 blobs occurred above the tips of it (Group 2). Their lateral widths are < 0.02 R⊙ > and < 0.05 R⊙>, which is smaller than, or similar to, those (< 0.06 R⊙ >) of the CS. They have elongated shapes: ratios of lateral to radial widths are < 0.53 > and < 0.40 >, respectively. In the first group, only three blobs propagate above the tip of the CS while the others are located in the CS. In the second group, only two blobs have associations with those of outer corona in their temporal and spatial relationship and their initial heights are 1.81 and 1.95 R⊙, measured from the center of the Sun. The others cannot be identified in the outer corona. Our results first demonstrate that LASCO-C2 blobs could be generated by the tearing mode instability near the tips of post-CME CSs, similar to the magnetic reconnection process in the tail CS of Earth's magnetosphere. Title: Rapid Evolution of Type II Spicules Observed in Goode Solar Telescope On-disk Hα Images Authors: Yurchyshyn, Vasyl; Cao, Wenda; Abramenko, Valentina; Yang, Xu; Cho, Kyung-Suk Bibcode: 2020ApJ...891L..21Y Altcode: 2020arXiv200504253Y We analyze ground-based chromospheric data acquired at a high temporal cadence of 2 s in wings of the Hα spectral line using the Goode Solar Telescope operating at the Big Bear Solar Observatory. We inspected a 30 minute long Hα-0.08 nm data set to find that rapid blueshifted Hα excursions (RBEs), which are a cool component of type II spicules, experience very rapid morphological changes on timescales of the order of 1 s. Unlike typical reconnection jets, RBEs very frequently appear in situ without any clear evidence of Hα material being injected from below. Their evolution includes inverted "Y," "V," "N," and parallel splitting (doubling) patterns as well as sudden formation of a diffuse region followed by branching. We also find that the same feature may undergo several splitting episodes within about a 1 minute time interval. Title: Oscillation of a Small Hα Surge in a Solar Polar Coronal Hole Authors: Cho, K. S. F. Bibcode: 2019AGUFMSH53B3375C Altcode: Hα surges (i.e., cool/dense collimated plasma ejections) may act as a guide for a propagation of magnetohydrodynamic waves. We report a high-resolution observation of a surge observed with 1.6 m Goode Solar Telescope (GST) on 2009 August 26, from 18:20 UT to 18:45 UT. Characteristics of plasma motions in the surge are determined with the normalizing radial gradient filter and the Fourier motion filter. The shape of the surge is found to change from a "C" shape to an inverse "C" shape after a formation of a cusp, a signature of reconnection. There are apparent upflows seen above the cusp top and downflows below it. The upflows show rising and rotational motions in the right-hand direction, with the rotational speed decreasing with height. Near the cusp top, we find a transverse oscillation of the surge, with the period of ∼2 minutes. There is no change of the oscillation phase below the cusp top, but above the top a phase change is identified, giving a vertical phase speed about 86 km s-1. As the height increases, the initial amplitude of the oscillation increases, and the oscillation damping time decreases from 5.13 to 1.18 minutes. We conclude that the oscillation is a propagating kink wave that is possibly excited by the repetitive spontaneous magnetic reconnection. Title: Visualizing Seasons and Moon Phases with WorldWide Telescope Authors: Udomprasert, P.; Houghton, H.; Sunbury, S.; Plummer, J.; Wright, E.; Goodman, A.; Johnson, E.; Zhang, H.; Vaishampayan, A.; Cho, K. Bibcode: 2019ASPC..524..125U Altcode: WorldWide Telescope (WWT) is a powerful visualization program that allows users to connect Earth-based and space-based views of the Sun-Earth-Moon system. By blending hands-on physical activities with WWT's virtual models, students can visualize spatially complex concepts like seasons, Moon phases, and eclipses. In this workshop, we will demonstrate how WWT and the physical models are used together in our WWT ThinkSpace curriculum, developed with funding from the National Science Foundation. We will also present student learning outcomes based on written assessments and student interviews. Title: A New Type of Jet in a Polar Limb of the Solar Coronal Hole Authors: Cho, Il-Hyun; Moon, Yong-Jae; Cho, Kyung-Suk; Nakariakov, Valery M.; Lee, Jin-Yi; Kim, Yeon-Han Bibcode: 2019ApJ...884L..38C Altcode: 2019arXiv191009737C A new type of chromospheric jet in a polar limb of a coronal hole is discovered in the Ca II filtergram of the Solar Optical Telescope on board the Hinode. We identify 30 jets in a filtered Ca II movie with a duration of 53 minutes. The average speed at their maximum heights is found to be 132 ± 44 km s-1 ranging from 57 to 264 km s-1 along the propagation direction. The average lifetime is 20 ± 6 ranging from 11 to 36 s. The speed and lifetime of the jets are located at end-tails of those parameters determined for type II spicules, hence implying a new type of jets. To confirm whether these jets are different from conventional spicules, we construct a time-height image averaged over a horizontal region of 1″, and calculate lagged cross-correlations of intensity profiles at each height with the intensity at 2 Mm. From this, we obtain a cross-correlation map as a function of lag and height. We find that the correlation curve as a function of lag time is well fitted into three different Gaussian functions whose standard deviations of the lag time are 193, 42, and 17 s. The corresponding propagation speeds are calculated to be 9 km s-1, 67 km s-1, and 121 km s-1, respectively. The kinematic properties of the former two components seem to correspond to the 3-minute oscillations and type II spicules, while the latter component to the jets is addressed in this study. Title: Vortex Formations and Its Associated Surges in a Sunspot Light Bridge Authors: Yang, Heesu; Lim, Eun-Kyung; Iijima, Haruhisa; Yurchyshyn, Vasyl; Cho, Kyung-Suk; Lee, Jeongwoo; Schmieder, Brigitte; Kim, Yeon-Han; Kim, Sujin; Bong, Su-Chan Bibcode: 2019ApJ...882..175Y Altcode: We report on the successive occurrence of 0.″5 wide photospheric vortices with strong transverse shear flows at the edge of a sunspot light bridge (LB), and the subsequent ejection of chromospheric surges observed using a Visible Inteferometry Spectrograph, a broadband TiO filter, and a Near InfRared Imaging Spectrograph of the Goode Solar Telescope operating at Big Bear Solar Observatory. The Hα surges ejected at the location of the vortices often appeared in a hollow cylindrical structure. We also observed quasi-periodic vortex-associated bright Hα plasma blobs moving upward with a speed of up to 4 km s-1. In view of the strong shear flow at the edge of the LB, it is likely that the vortices form under the Kelvin-Helmholtz instability. The surges may result from either the magnetic tension generated after magnetic reconnection or an acoustic impulse of a fast photospheric transverse flow. Otherwise, the surges could also be associated with Alfvénic waves, in which case their origin could be torsional magnetic fields generated in the process of the vortex formation. Title: First cryogenic test operation of underground km-scale gravitational-wave observatory KAGRA Authors: Akutsu, T.; Ando, M.; Arai, K.; Arai, Y.; Araki, S.; Araya, A.; Aritomi, N.; Asada, H.; Aso, Y.; Atsuta, S.; Awai, K.; Bae, S.; Baiotti, L.; Barton, M. A.; Cannon, K.; Capocasa, E.; Chen, C. -S.; Chiu, T. -W.; Cho, K.; Chu, Y. -K.; Craig, K.; Creus, W.; Doi, K.; Eda, K.; Enomoto, Y.; Flaminio, R.; Fujii, Y.; Fujimoto, M. -K.; Fukunaga, M.; Fukushima, M.; Furuhata, T.; Hagiwara, A.; Haino, S.; Hasegawa, K.; Hashino, K.; Hayama, K.; Hirobayashi, S.; Hirose, E.; Hsieh, B. H.; Huang, C. -Z.; Ikenoue, B.; Inoue, Y.; Ioka, K.; Itoh, Y.; Izumi, K.; Kaji, T.; Kajita, T.; Kakizaki, M.; Kamiizumi, M.; Kanbara, S.; Kanda, N.; Kanemura, S.; Kaneyama, M.; Kang, G.; Kasuya, J.; Kataoka, Y.; Kawai, N.; Kawamura, S.; Kawasaki, T.; Kim, C.; Kim, J.; Kim, J. C.; Kim, W. S.; Kim, Y. -M.; Kimura, N.; Kinugawa, T.; Kirii, S.; Kitaoka, Y.; Kitazawa, H.; Kojima, Y.; Kokeyama, K.; Komori, K.; Kong, A. K. H.; Kotake, K.; Kozu, R.; Kumar, R.; Kuo, H. -S.; Kuroyanagi, S.; Lee, H. K.; Lee, H. M.; Lee, H. W.; Leonardi, M.; Lin, C. -Y.; Lin, F. -L.; Liu, G. C.; Liu, Y.; Majorana, E.; Mano, S.; Marchio, M.; Matsui, T.; Matsushima, F.; Michimura, Y.; Mio, N.; Miyakawa, O.; Miyamoto, A.; Miyamoto, T.; Miyo, K.; Miyoki, S.; Morii, W.; Morisaki, S.; Moriwaki, Y.; Morozumi, T.; Murakami, I.; Musha, M.; Nagano, K.; Nagano, S.; Nakamura, K.; Nakamura, T.; Nakano, H.; Nakano, M.; Nakao, K.; Namai, Y.; Narikawa, T.; Naticchioni, L.; Nguyen Quynh, L.; Ni, W. -T.; Nishizawa, A.; Obuchi, Y.; Ochi, T.; Oh, J. J.; Oh, S. H.; Ohashi, M.; Ohishi, N.; Ohkawa, M.; Okutomi, K.; Ono, K.; Oohara, K.; Ooi, C. P.; Pan, S. -S.; Park, J.; Peña Arellano, F. E.; Pinto, I.; Sago, N.; Saijo, M.; Saito, Y.; Saitou, S.; Sakai, K.; Sakai, Y.; Sakai, Y.; Sasai, M.; Sasaki, M.; Sasaki, Y.; Sato, N.; Sato, S.; Sato, T.; Sekiguchi, Y.; Seto, N.; Shibata, M.; Shimoda, T.; Shinkai, H.; Shishido, T.; Shoda, A.; Somiya, K.; Son, E. J.; Suemasa, A.; Suzuki, T.; Suzuki, T.; Tagoshi, H.; Tahara, H.; Takahashi, H.; Takahashi, R.; Takamori, A.; Takeda, H.; Tanaka, H.; Tanaka, K.; Tanaka, T.; Tanioka, S.; Tapia San Martin, E. N.; Tatsumi, D.; Terashima, S.; Tomaru, T.; Tomura, T.; Travasso, F.; Tsubono, K.; Tsuchida, S.; Uchikata, N.; Uchiyama, T.; Ueda, A.; Uehara, T.; Ueki, S.; Ueno, K.; Uraguchi, F.; Ushiba, T.; van Putten, M. H. P. M.; Vocca, H.; Wada, S.; Wakamatsu, T.; Watanabe, Y.; Xu, W. -R.; Yamada, T.; Yamamoto, A.; Yamamoto, K.; Yamamoto, K.; Yamamoto, S.; Yamamoto, T.; Yokogawa, K.; Yokoyama, J.; Yokozawa, T.; Yoon, T. H.; Yoshioka, T.; Yuzurihara, H.; Zeidler, S.; Zhu, Z. -H.; KAGRA Collaboration Bibcode: 2019CQGra..36p5008A Altcode: 2019arXiv190103569K KAGRA is a second-generation interferometric gravitational-wave detector with 3 km arms constructed at Kamioka, Gifu, Japan. It is now in its final installation phase, which we call bKAGRA (baseline KAGRA), with scientific observations expected to begin in late 2019. One of the advantages of KAGRA is its underground location of at least 200 m below the ground surface, which reduces seismic motion at low frequencies and increases the stability of the detector. Another advantage is that it cools down the sapphire test mass mirrors to cryogenic temperatures to reduce thermal noise. In April-May 2018, we operated a 3 km Michelson interferometer with a cryogenic test mass for 10 d, which was the first time that km-scale interferometer was operated at cryogenic temperatures. In this article, we report the results of this ‘bKAGRA Phase 1’ operation. We have demonstrated the feasibility of 3 km interferometer alignment and control with cryogenic mirrors. Title: Vibration isolation system with a compact damping system for power recycling mirrors of KAGRA Authors: Akiyama, Y.; Akutsu, T.; Ando, M.; Arai, K.; Arai, Y.; Araki, S.; Araya, A.; Aritomi, N.; Asada, H.; Aso, Y.; Bae, S.; Baiotti, L.; Barton, M. A.; Cannon, K.; Capocasa, E.; Chen, C. -S.; Chiu, T. -W.; Cho, K.; Chu, Y. -K.; Craig, K.; Dattilo, V.; Doi, K.; Enomoto, Y.; Flaminio, R.; Fujii, Y.; Fujimoto, M. -K.; Fukunaga, M.; Fukushima, M.; Furuhata, T.; Haino, S.; Hasegawa, K.; Hashimoto, Y.; Hashino, K.; Hayama, K.; Hirayama, T.; Hirose, E.; Hsieh, B. H.; Huang, C. -Z.; Ikenoue, B.; Inoue, Y.; Ioka, K.; Itoh, Y.; Izumi, K.; Kaji, T.; Kajita, T.; Kakizaki, M.; Kamiizumi, M.; Kanbara, S.; Kanda, N.; Kanemura, S.; Kang, G.; Kasuya, J.; Kawai, N.; Kawasaki, T.; Kim, C.; Kim, W. S.; Kim, J.; Kim, J. C.; Kimura, N.; Kirii, S.; Kitaoka, Y.; Kitazawa, H.; Kojima, Y.; Kokeyama, K.; Komori, K.; Kong, A.; Kotake, K.; Kozu, R.; Kumar, R.; Kuo, H. -S.; Kuroki, S.; Kuroyanagi, S.; Lee, H. K.; Lee, H. M.; Lee, H. W.; Leonardi, M.; Lin, C. -Y.; Lin, F. -L.; Liu, G. C.; Marchio, M.; Matsui, T.; Michimura, Y.; Mio, N.; Miyakawa, O.; Miyamoto, A.; Miyoki, S.; Morii, W.; Morisaki, S.; Moriwaki, Y.; Musha, M.; Nagano, S.; Nagano, K.; Nakamura, K.; Nakamura, T.; Nakano, H.; Nakano, M.; Narikawa, T.; Nguyen Quynh, L.; Ni, W. -T.; Nishizawa, A.; Obuchi, Y.; Oh, J.; Oh, S. H.; Ohashi, M.; Ohishi, N.; Ohkawa, M.; Okutomi, K.; Ono, K.; Oohara, K.; Ooi, C. P.; Pan, S. -S.; Paoletti, F.; Park, J.; Passaquieti, R.; Peña Arellano, F. E.; Sago, N.; Saito, S.; Saito, Y.; Sakai, K.; Sakai, Y.; Sasai, M.; Sato, S.; Sato, T.; Sekiguchi, T.; Sekiguchi, Y.; Shibata, M.; Shimoda, T.; Shinkai, H.; Shishido, T.; Shoda, A.; Someya, N.; Somiya, K.; Son, E. J.; Suemasa, A.; Suzuki, T.; Suzuki, T.; Tagoshi, H.; Tahara, H.; Takahashi, H.; Takahashi, R.; Takeda, H.; Tanaka, H.; Tanaka, K.; Tanaka, T.; Tanioka, S.; Tapia San Martin, E. N.; Tomaru, T.; Tomura, T.; Travasso, F.; Tsubono, K.; Tsuchida, S.; Uchikata, N.; Uchiyama, T.; Uehara, T.; Ueno, K.; Uraguchi, F.; Ushiba, T.; van Putten, M. H. P. M.; Vocca, H.; Wakamatsu, T.; Watanabe, Y.; Xu, W. -R.; Yamada, T.; Yamamoto, K.; Yamamoto, K.; Yamamoto, S.; Yamamoto, T.; Yokogawa, K.; Yokoyama, J.; Yokozawa, T.; Yoshioka, T.; Yuzurihara, H.; Zeidler, S.; Zhu, Z. -H. Bibcode: 2019CQGra..36i5015A Altcode: 2019arXiv190103053A A vibration isolation system called the Type-Bp system used for power recycling mirrors has been developed for KAGRA, the interferometric gravitational-wave observatory in Japan. A suspension of the Type-Bp system passively isolates an optic from seismic vibration using three main pendulum stages equipped with two vertical vibration isolation systems. A compact reaction mass around each of the main stages allows for achieving sufficient damping performance with a simple feedback as well as vibration isolation ratio. Three Type-Bp systems were installed in KAGRA, and were proved to satisfy the requirements on the damping performance, and also on estimated residual displacement of the optics. Title: Oscillation of a Small Hα Surge in a Solar Polar Coronal Hole Authors: Cho, Kyung-Suk; Cho, Il-Hyun; Nakariakov, V. M.; Yurchyshyn, Vasyl B.; Yang, Heesu; Kim, Yeon-Han; Kumar, Pankaj; Magara, Tetsuya Bibcode: 2019ApJ...877L...1C Altcode: Hα surges (i.e., cool/dense collimated plasma ejections) may act as a guide for a propagation of magnetohydrodynamic waves. We report a high-resolution observation of a surge observed with 1.6 m Goode Solar Telescope (GST) on 2009 August 26, from 18:20 UT to 18:45 UT. Characteristics of plasma motions in the surge are determined with the normalizing radial gradient filter and the Fourier motion filter. The shape of the surge is found to change from a “C” shape to an inverse “C” shape after a formation of a cusp, a signature of reconnection. There are apparent upflows seen above the cusp top and downflows below it. The upflows show rising and rotational motions in the right-hand direction, with the rotational speed decreasing with height. Near the cusp top, we find a transverse oscillation of the surge, with the period of ∼2 minutes. There is no change of the oscillation phase below the cusp top, but above the top a phase change is identified, giving a vertical phase speed about 86 km s-1. As the height increases, the initial amplitude of the oscillation increases, and the oscillation damping time decreases from 5.13 to 1.18 minutes. We conclude that the oscillation is a propagating kink wave that is possibly excited by the repetitive spontaneous magnetic reconnection. Title: Interplanetary Coronal Mass Ejections During Solar Cycles 23 and 24: Sun-Earth Propagation Characteristics and Consequences at the Near-Earth Region Authors: Syed Ibrahim, M.; Joshi, Bhuwan; Cho, K. -S.; Kim, R. -S.; Moon, Y. -J. Bibcode: 2019SoPh..294...54S Altcode: In this article, we present a statistical study probing the relation between interplanetary coronal mass ejections (ICMEs) observed at 1 AU and their corresponding coronal mass ejections at the near-Sun region. The work encompasses the ICME activity that occurred during Solar Cycles 23 and 24 (1996 - 2017) while presenting an overall picture of ICME events during the complete Solar Cycle 24 for the first time. The importance of this study further lies in comparing two subsets of ICMEs, i.e. magnetic clouds (MCs) and ejecta (EJ), to explore how the observed structures of ICMEs at 1 AU could be associated with the properties of CMEs during their launch at the Sun. We find that, although Solar Cycle 24 saw a significant reduction in the number of ICME events compared to the previous cycle, the fraction of MCs was much higher during Cycle 24 than Cycle 23 (60% versus 41%). In general, the ICME transit-time decreases with the increase in the CME initial speed, although a broad range of transit times were observed for a given CME speed. We also find that the high-speed ICMEs (≳500 kms−1) form a distinct group in terms of the deficit in their transit times when compared with low-speed events (≲500 kms−1), which means that high-speed ICMEs acquire a much higher internal energy from the source active regions during the initiation process that effectively overcomes the aerodynamic drag force while they transit in the interplanetary medium. The CME propagation from the Sun to the near-Earth environment shows both an overall positive and negative acceleration (i.e. deceleration), although the acceleration is limited to only low-speed CMEs that are launched with a speed comparable with or less than the mean solar wind speed (≈400 -450 kms−1). Within a given cycle, the similarities of MC and EJ profiles with respect to the CME-ICME speed relation as well as interplanetary acceleration support the hypothesis that all CMEs have a flux rope structure and that the trajectory of the CMEs essentially determines the observed ICME structure at 1 AU. Title: Solar activities and climate change during the last millennium recorded in Korean chronicles Authors: Yang, Hong-Jin; Park, Chan-Gyung; Kim, Rok-Soon; Cho, Kyung-Suk; Jeon, Junhyeok Bibcode: 2019JASTP.186..139Y Altcode: Korean chronicles have a large amount of observational records of natural phenomena, including astronomical and meteorological events over two thousand years. Here we examine the correlation of solar activity and climate change from historical sunspot and frost records in the Korean chronicles. There are 42 sunspot records in Goryeo Dynasty (918-1392 CE) and 13 records in Joseon Dynasty (1392-1910 CE). The sunspot records in Goryeo Dynasty show a periodicity in good agreement with the well-known solar activity of 11 years. Korean sunspot records suggest that the solar activity in Joseon Dynasty decreased compared with that in the previous ∼500 years. In order to examine the long-period variation of solar activity, we include Chinese historical sunspot records in our analysis to supplement the lack of Korean records, and find a new ∼240-yr long-period solar activity from the power spectral analysis. Korean chronicles also have about 700 frost records during the last millennium. We investigate these frost records and find a sign of cooling down that can be interpreted as climate change during the last millennium. We also find ∼240-yr cooling period from the historical frost records, which is well in accord with that of solar activity. Therefore, we conclude that the solar activity has decreased during the last one thousand years and also has a long-term variation of ∼240 years. Title: Coronal electron density distributions from simultaneous observations of solar corona with MK4, LASCO-C2, and SECCHI-COR1 Coronagraphs during the period from March 2007 to June 2007 Authors: Lee, Jae-Ok; Cho, Kyung-Suk Bibcode: 2019EGUGA..2112308L Altcode: The coronal electron density is a fundamental and important physical quantity in solar physics for estimating coronal magnetic fields and analyzing solar radio bursts. Many ground- and space-based white-light coronagraphs continuously measure polarized brightness to estimate coronal electron density distributions (CEDDs). To confirm the consistency of white-light coronagraph measurements and determine CEDDs, we compare CEDDs derived from MK4 coronameter and LASCO-C2 with Van de Hulst inversions and SECCHI-COR1A and COR1B with spherically symmetric polynomial approximation (SSPA) by Wang et al., 2014. For this, we consider coronagraph data from January to August 2007 with the following conditions: (1) the separation angle between the either of the STEREO spacecraft and Earth is less than 10 degrees; (2) the observation time differences from one another are less than 1 minutes; and (3) the data can be reasonably inverted to derive CEDDs; (4) bright and faint streamer, and plume and inter-plume regions are well observed in LASCO-C2 field of view. By investigating 15 events, 10 events are simultaneously observed by MK4, LASCO-C2, and SECCHI-COR1A and 5 events are observed by MK4, LASCO-C2, and SECCHI-COR1B, we find the following characteristics: (1) CEDDs are similar to one another at broad- and faint- streamer regions (bright coronal structures) while they are not similar to one another at plume and inter-plume regions (faint coronal structures). Especially, there are very weak polarized brightness near polar regions in SECCHI-COR1 observations, which are similar to those of coronal backgrounds. (2) the average of estimated CEDDs from 1.2 to 6 solar radii is 1.0-Fold Saito's density model at bright streamer regions and 0.5-fold Saito's model at faint streamer regions while it is 0.2-fold Saito's model at plume and inter-plume regions. Our results indicate that not only kinematic studies of bright coronal structures such as streamers and CMEs observed by using white-light coronagraphs with different Field of View are reliable, but also 1-fold Saito's model is a proper CEDDs at bright streamer regions during solar minimum period. Title: Solar farside magnetograms from deep learning analysis of STEREO/EUVI data Authors: Kim, Taeyoung; Park, Eunsu; Lee, Harim; Moon, Yong-Jae; Bae, Sung-Ho; Lim, Daye; Jang, Soojeong; Kim, Lokwon; Cho, Il-Hyun; Choi, Myungjin; Cho, Kyung-Suk Bibcode: 2019NatAs...3..397K Altcode: 2019NatAs.tmp..220K Solar magnetograms are important for studying solar activity and predicting space weather disturbances1. Farside magnetograms can be constructed from local helioseismology without any farside data2-4, but their quality is lower than that of typical frontside magnetograms. Here we generate farside solar magnetograms from STEREO/Extreme UltraViolet Imager (EUVI) 304-Å images using a deep learning model based on conditional generative adversarial networks (cGANs). We train the model using pairs of Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA) 304-Å images and SDO/Helioseismic and Magnetic Imager (HMI) magnetograms taken from 2011 to 2017 except for September and October each year. We evaluate the model by comparing pairs of SDO/HMI magnetograms and cGAN-generated magnetograms in September and October. Our method successfully generates frontside solar magnetograms from SDO/AIA 304-Å images and these are similar to those of the SDO/HMI, with Hale-patterned active regions being well replicated. Thus we can monitor the temporal evolution of magnetic fields from the farside to the frontside of the Sun using SDO/HMI and farside magnetograms generated by our model when farside extreme-ultraviolet data are available. This study presents an application of image-to-image translation based on cGANs to scientific data. Title: Seismological Determination of the Alfvén Speed and Plasma Beta in Solar Photospheric Bright Points Authors: Cho, Il-Hyun; Moon, Yong-Jae; Nakariakov, Valery M.; Yu, Dae Jung; Lee, Jin-Yi; Bong, Su-Chan; Kim, Rok-Soon; Cho, Kyung-Suk; Kim, Yeon-Han; Lee, Jae-Ok Bibcode: 2019ApJ...871L..14C Altcode: 2019arXiv190104144C The Alfvén speed and plasma beta in photospheric bright points (BPs) observed by the Broadband Filter Imager (BFI) of the Solar Optical Telescope on board the Hinode satellite are estimated seismologically. The diagnostics is based on the theory of slow magnetoacoustic waves in a non-isothermally stratified photosphere with a uniform vertical magnetic field. We identify and track BPs in a G-band movie by using the 3D region growing method, and align them with blue continuum images to derive their brightness temperatures. From the Fourier power spectra of 118 continuum light curves made in the BPs, we find that light curves of 91 BPs have oscillations with properties that are significantly different from oscillation in quiet regions, with the periods ranging 2.2-16.2 minutes. We find that the model gives a moderate value of the plasma beta when γ lies at around 5/3. The calculated Alfvén speed is 9.68 ± 2.02 km s-1, ranging in 6.3-17.4 km s-1. The plasma beta is estimated to be of 0.93 ± 0.36, ranging in 0.2-1.9. Title: KAGRA: 2.5 generation interferometric gravitational wave detector Authors: Kagra Collaboration; Akutsu, T.; Ando, M.; Arai, K.; Arai, Y.; Araki, S.; Araya, A.; Aritomi, N.; Asada, H.; Aso, Y.; Atsuta, S.; Awai, K.; Bae, S.; Baiotti, L.; Barton, M. A.; Cannon, K.; Capocasa, E.; Chen, C. -S.; Chiu, T. -W.; Cho, K.; Chu, Y. -K.; Craig, K.; Creus, W.; Doi, K.; Eda, K.; Enomoto, Y.; Flaminio, R.; Fujii, Y.; Fujimoto, M. -K.; Fukunaga, M.; Fukushima, M.; Furuhata, T.; Haino, S.; Hasegawa, K.; Hashino, K.; Hayama, K.; Hirobayashi, S.; Hirose, E.; Hsieh, B. H.; Huang, C. -Z.; Ikenoue, B.; Inoue, Y.; Ioka, K.; Itoh, Y.; Izumi, K.; Kaji, T.; Kajita, T.; Kakizaki, M.; Kamiizumi, M.; Kanbara, S.; Kanda, N.; Kanemura, S.; Kaneyama, M.; Kang, G.; Kasuya, J.; Kataoka, Y.; Kawai, N.; Kawamura, S.; Kawasaki, T.; Kim, C.; Kim, J.; Kim, J. C.; Kim, W. S.; Kim, Y. -M.; Kimura, N.; Kinugawa, T.; Kirii, S.; Kitaoka, Y.; Kitazawa, H.; Kojima, Y.; Kokeyama, K.; Komori, K.; Kong, A. K. H.; Kotake, K.; Kozu, R.; Kumar, R.; Kuo, H. -S.; Kuroyanagi, S.; Lee, H. K.; Lee, H. M.; Lee, H. W.; Leonardi, M.; Lin, C. -Y.; Lin, F. -L.; Liu, G. C.; Liu, Y.; Majorana, E.; Mano, S.; Marchio, M.; Matsui, T.; Matsushima, F.; Michimura, Y.; Mio, N.; Miyakawa, O.; Miyamoto, A.; Miyamoto, T.; Miyo, K.; Miyoki, S.; Morii, W.; Morisaki, S.; Moriwaki, Y.; Morozumi, T.; Musha, M.; Nagano, K.; Nagano, S.; Nakamura, K.; Nakamura, T.; Nakano, H.; Nakano, M.; Nakao, K.; Narikawa, T.; Naticchioni, L.; Nguyen Quynh, L.; Ni, W. -T.; Nishizawa, A.; Obuchi, Y.; Ochi, T.; Oh, J. J.; Oh, S. H.; Ohashi, M.; Ohishi, N.; Ohkawa, M.; Okutomi, K.; Ono, K.; Oohara, K.; Ooi, C. P.; Pan, S. -S.; Park, J.; Peña Arellano, F. E.; Pinto, I.; Sago, N.; Saijo, M.; Saitou, S.; Saito, Y.; Sakai, K.; Sakai, Y.; Sakai, Y.; Sasai, M.; Sasaki, M.; Sasaki, Y.; Sato, S.; Sato, N.; Sato, T.; Sekiguchi, Y.; Seto, N.; Shibata, M.; Shimoda, T.; Shinkai, H.; Shishido, T.; Shoda, A.; Somiya, K.; Son, E. J.; Suemasa, A.; Suzuki, T.; Suzuki, T.; Tagoshi, H.; Tahara, H.; Takahashi, H.; Takahashi, R.; Takamori, A.; Takeda, H.; Tanaka, H.; Tanaka, K.; Tanaka, T.; Tanioka, S.; Tapia San Martin, E. N.; Tatsumi, D.; Tomaru, T.; Tomura, T.; Travasso, F.; Tsubono, K.; Tsuchida, S.; Uchikata, N.; Uchiyama, T.; Uehara, T.; Ueki, S.; Ueno, K.; Uraguchi, F.; Ushiba, T.; van Putten, M. H. P. M.; Vocca, H.; Wada, S.; Wakamatsu, T.; Watanabe, Y.; Xu, W. -R.; Yamada, T.; Yamamoto, A.; Yamamoto, K.; Yamamoto, K.; Yamamoto, S.; Yamamoto, T.; Yokogawa, K.; Yokoyama, J.; Yokozawa, T.; Yoon, T. H.; Yoshioka, T.; Yuzurihara, H.; Zeidler, S.; Zhu, Z. -H. Bibcode: 2019NatAs...3...35K Altcode: 2018arXiv181108079A The recent detections of gravitational waves (GWs) reported by the LIGO and Virgo collaborations have made a significant impact on physics and astronomy. A global network of GW detectors will play a key role in uncovering the unknown nature of the sources in coordinated observations with astronomical telescopes and detectors. Here we introduce KAGRA, a new GW detector with two 3 km baseline arms arranged in an `L' shape. KAGRA's design is similar to the second generations of Advanced LIGO and Advanced Virgo, but it will be operating at cryogenic temperatures with sapphire mirrors. This low-temperature feature is advantageous for improving the sensitivity around 100 Hz and is considered to be an important feature for the third-generation GW detector concept (for example, the Einstein Telescope of Europe or the Cosmic Explorer of the United States). Hence, KAGRA is often called a 2.5-generation GW detector based on laser interferometry. KAGRA's first observation run is scheduled in late 2019, aiming to join the third observation run of the advanced LIGO-Virgo network. When operating along with the existing GW detectors, KAGRA will be helpful in locating GW sources more accurately and determining the source parameters with higher precision, providing information for follow-up observations of GW trigger candidates. Title: Effects of Geometries and Substructures of ICMEs on Geomagnetic Storms Authors: Lee, Jae-Ok; Cho, Kyung-Suk; Kim, Rok-Soon; Jang, Soojeong; Marubashi, Katsuhide Bibcode: 2018SoPh..293..129L Altcode: To better understand geomagnetic storm generations by ICMEs, we consider the effect of substructures (magnetic cloud, MC, and sheath) and geometries (impact location of flux-rope at the Earth) of the ICMEs. We apply the toroidal magnetic flux-rope model to 59 CDAW CME-ICME pairs to identify their substructures and geometries, and select 20 MC-associated and five sheath-associated storm events. We investigate the relationship between the storm strength indicated by minimum Dst index (Dstmin) and solar wind conditions related to a southward magnetic field. We find that all slopes of linear regression lines for sheath-storm events are steeper (≥1.4 ) than those of the MC-storm events in the relationship between Dstmin and solar wind conditions, implying that the efficiency of sheath for the process of geomagnetic storm generations is higher than that of MC. These results suggest that different general solar wind conditions (sheaths have a higher density, dynamic and thermal pressures with a higher fluctuation of the parameters and higher magnetic fields than MCs) have different impact on storm generation. Regarding the geometric encounter of ICMEs, 100% (2/2) of major storms (Dstmin≤−100 nT) occur in the regions at negative PY (relative position of the Earth trajectory from the ICME axis in the Y component of the GSE coordinate) when the eastern flanks of ICMEs encounter the Earth. We find similar statistical trends in solar wind conditions, suggesting that the dependence of geomagnetic storms on 3D ICME-Earth impact geometries is caused by asymmetric distributions of the geoeffective solar wind conditions. For western flank events, 80% (4/5) of the major storms occur in positive PY regions, while intense geoeffective solar wind conditions are not located in the positive PY. These results suggest that the strength of geomagnetic storms depends on ICME-Earth impact geometries as they determine the solar wind conditions at Earth. Title: Two-Dimensional Solar Wind Speeds from 6 to 26 Solar Radii in Solar Cycle 24 by Using Fourier Filtering Authors: Cho, Il-Hyun; Moon, Yong-Jae; Nakariakov, Valery M.; Bong, Su-Chan; Lee, Jin-Yi; Song, Donguk; Lee, Harim; Cho, Kyung-Suk Bibcode: 2018PhRvL.121g5101C Altcode: 2018arXiv180608540C Measurement of the solar wind speed near the Sun is important for understanding the acceleration mechanism of the solar wind. In this Letter, we determine 2D solar wind speeds from 6 to 26 solar radii by applying Fourier motion filters to SOHO/LASCO C3 movies observed from 1999 to 2010. Our method successfully reproduces the original flow speeds in the artificially generated data as well as streamer blobs. We measure 2D solar wind speeds from one-day to one-year timescales and their variation in solar cycle 24. We find that the solar wind speeds at timescales longer than a month in the solar maximum period are relatively uniform in the azimuthal direction, while they are clearly bimodal in the minimum period, as expected from the Ulysses observations and interplanetary radio scintillation reconstruction. The bimodal structure appears at around 2006, becomes most distinctive in 2009, and abruptly disappears in 2010. The radial evolution of the solar wind speeds resembles the Parker's solar wind solution. Title: High-resolution Observations of a White-light Flare with Goode Solar Telescope Authors: Yurchyshyn, Vasyl; Kumar, Pankaj; Abramenko, Valentyna; Xu, Yan; Goode, Philip R.; Cho, Kyung-Suk F. Bibcode: 2018tess.conf21702Y Altcode: Using high resolution data from the Goode Solar Telescope (GST) we studied the fine spatial and temporal structure of an M1.3 white light (WL) flare, which was one of the three homologous solar flares (C6.8, M1.3, and M2.3) observed in a close proximity to the west solar limb. The RHESSI photon spectra for the M1.3 flare showed strongly accelerated electrons with energies above 100 keV. Comparison of HXR photon spectra for the three flares suggests that either thermal energy of order of 1030 ergs and/or high energy electrons (>50 keV) are necessary to produce a WL flare. The strong and compact WL cores were ≈0.15 Mm across with an area of about 1014 cm2 . The observed TiO enhancements are not normally distributed and are structured by the magnetic field of the penumbra. Several of the TiO cores were not co-spatial with the Hα emission, which suggests that the TiO and chromospheric emission did not originate in the same chromospheric volume as some models suggest. We thus conclude that fine temporal and spatial structure of the WL flare was largely defined by the associated magnetic fields, which favors the direct heating models, where the flare energy is directly deposited in the temperature minimum region by the accelerated electrons. Title: Simulation and Quasi-Linear Theory of Whistler Anisotropy Instability Authors: Lee, Sang-Yun; Lee, Ensang; Seough, Jungjoon; Lee, Jung-gi; Hwang, Junga; Lee, Jae-Jin; Cho, Kyung-Suk; Yoon, Peter H. Bibcode: 2018JGRA..123.3277L Altcode: The whistler anisotropy (or electromagnetic electron cyclotron) instability may be operative in many geomagnetic and heliospherical environments, including the radiation belt, solar wind, and the solar corona. The present investigation carries out a comparative analysis between the two-dimensional particle-in-cell simulation of weakly growing whistler anisotropy instability and the velocity moment-based two-dimensional quasi-linear theory under the assumption of bi-Maxwellian electron distribution function. It is shown that the simplified quasi-linear theory provides a qualitative agreement with the more rigorous particle-in-cell simulation, but some discrepancies are also found. Possible causes for the differences in either method are discussed, and future improvements on the theory are suggested. Potential applicability of the present finding in the context of the space and astrophysics is discussed. Title: Toward a Next Generation Solar Coronagraph: Diffracted Light Simulation and Test Results for a Cone Occulter with Tapered Surface Authors: Yang, Heesu; Bong, Su-Chan; Cho, Kyung-Suk; Choi, Seonghwan; Park, Jongyeob; Kim, Jihun; Baek, Ji-Hye; Nah, Jakyoung; Sun, Mingzhe; Gong, Qian Bibcode: 2018JKAS...51...27Y Altcode: In a solar coronagraph, the most important component is an occulter to block the direct light from the disk of the sun Because the intensity of the solar outer corona is 10-6 to 10-10 times of that of the solar disk (\ir), it is necessary to minimize scattering at the optical elements and diffraction at the occulter. Using a Fourier optic simulation and a stray light test, we investigated the performance of a compact coronagraph that uses an external truncated-cone occulter without an internal occulter and Lyot stop. In the simulation, the diffracted light was minimized to the order of 7.6×10-10 \ir when the cone angle θc was about 0.39°. The performance of the cone occulter was then tested by experiment. The level of the diffracted light reached the order of 6×10-9 \ir at θc=0.40°. This is sufficient to observe the outer corona without additional optical elements such as a Lyot stop or inner occulter. We also found the manufacturing tolerance of the cone angle to be 0.05°, the lateral alignment tolerance was 45 \um, and the angular alignment tolerance was 0.043°. Our results suggest that the physical size of coronagraphs can be shortened significantly by using a cone occulter. Title: Observation of the Kelvin-Helmholtz Instability in a Solar Prominence Authors: Yang, Heesu; Xu, Zhi; Lim, Eun-Kyung; Kim, Sujin; Cho, Kyung-Suk; Kim, Yeon-Han; Chae, Jongchul; Cho, Kyuhyoun; Ji, Kaifan Bibcode: 2018ApJ...857..115Y Altcode: Many solar prominences end their lives in eruptions or abrupt disappearances that are associated with dynamical or thermal instabilities. Such instabilities are important because they may be responsible for energy transport and conversion. We present a clear observation of a streaming kink-mode Kelvin-Helmholtz Instability (KHI) taking place in a solar prominence using the Hα Lyot filter installed at the New Vacuum Solar Telescope, Fuxian-lake Solar Observatory in Yunnan, China. On one side of the prominence, a series of plasma blobs floated up from the chromosphere and streamed parallel to the limb. The plasma stream was accelerated to about 20-60 km s-1 and then undulated. We found that 2″- and 5″-size vortices formed, floated along the stream, and then broke up. After the 5″-size vortex, a plasma ejection out of the stream was detected in the Solar Dynamics Observatory/Atmospheric Imaging Assembly images. Just before the formation of the 5″-size vortex, the stream displayed an oscillatory transverse motion with a period of 255 s with the amplitude growing at the rate of 0.001 s-1. We attribute this oscillation of the stream and the subsequent formation of the vortex to the KHI triggered by velocity shear between the stream, guided by the magnetic field and the surrounding media. The plasma ejection suggests the transport of prominence material into the upper layer by the KHI in its nonlinear stage. Title: Construction of KAGRA: an underground gravitational-wave observatory Authors: Akutsu, T.; Ando, M.; Araki, S.; Araya, A.; Arima, T.; Aritomi, N.; Asada, H.; Aso, Y.; Atsuta, S.; Awai, K.; Baiotti, L.; Barton, M. A.; Chen, D.; Cho, K.; Craig, K.; DeSalvo, R.; Doi, K.; Eda, K.; Enomoto, Y.; Flaminio, R.; Fujibayashi, S.; Fujii, Y.; Fujimoto, M. -K.; Fukushima, M.; Furuhata, T.; Hagiwara, A.; Haino, S.; Harita, S.; Hasegawa, K.; Hasegawa, M.; Hashino, K.; Hayama, K.; Hirata, N.; Hirose, E.; Ikenoue, B.; Inoue, Y.; Ioka, K.; Ishizaki, H.; Itoh, Y.; Jia, D.; Kagawa, T.; Kaji, T.; Kajita, T.; Kakizaki, M.; Kakuhata, H.; Kamiizumi, M.; Kanbara, S.; Kanda, N.; Kanemura, S.; Kaneyama, M.; Kasuya, J.; Kataoka, Y.; Kawaguchi, K.; Kawai, N.; Kawamura, S.; Kawazoe, F.; Kim, C.; Kim, J.; Kim, J. C.; Kim, W.; Kimura, N.; Kitaoka, Y.; Kobayashi, K.; Kojima, Y.; Kokeyama, K.; Komori, K.; Kotake, K.; Kubo, K.; Kumar, R.; Kume, T.; Kuroda, K.; Kuwahara, Y.; Lee, H. -K.; Lee, H. -W.; Lin, C. -Y.; Liu, Y.; Majorana, E.; Mano, S.; Marchio, M.; Matsui, T.; Matsumoto, N.; Matsushima, F.; Michimura, Y.; Mio, N.; Miyakawa, O.; Miyake, K.; Miyamoto, A.; Miyamoto, T.; Miyo, K.; Miyoki, S.; Morii, W.; Morisaki, S.; Moriwaki, Y.; Muraki, Y.; Murakoshi, M.; Musha, M.; Nagano, K.; Nagano, S.; Nakamura, K.; Nakamura, T.; Nakano, H.; Nakano, M.; Nakano, M.; Nakao, H.; Nakao, K.; Narikawa, T.; Ni, W. -T.; Nonomura, T.; Obuchi, Y.; Oh, J. J.; Oh, S. -H.; Ohashi, M.; Ohishi, N.; Ohkawa, M.; Ohmae, N.; Okino, K.; Okutomi, K.; Ono, K.; Ono, Y.; Oohara, K.; Ota, S.; Park, J.; Peña Arellano, F. E.; Pinto, I. M.; Principe, M.; Sago, N.; Saijo, M.; Saito, T.; Saito, Y.; Saitou, S.; Sakai, K.; Sakakibara, Y.; Sasaki, Y.; Sato, S.; Sato, T.; Sato, Y.; Sekiguchi, T.; Sekiguchi, Y.; Shibata, M.; Shiga, K.; Shikano, Y.; Shimoda, T.; Shinkai, H.; Shoda, A.; Someya, N.; Somiya, K.; Son, E. J.; Starecki, T.; Suemasa, A.; Sugimoto, Y.; Susa, Y.; Suwabe, H.; Suzuki, T.; Tachibana, Y.; Tagoshi, H.; Takada, S.; Takahashi, H.; Takahashi, R.; Takamori, A.; Takeda, H.; Tanaka, H.; Tanaka, K.; Tanaka, T.; Tatsumi, D.; Telada, S.; Tomaru, T.; Tsubono, K.; Tsuchida, S.; Tsukada, L.; Tsuzuki, T.; Uchikata, N.; Uchiyama, T.; Uehara, T.; Ueki, S.; Ueno, K.; Uraguchi, F.; Ushiba, T.; van Putten, M. H. P. M.; Wada, S.; Wakamatsu, T.; Yaginuma, T.; Yamamoto, K.; Yamamoto, S.; Yamamoto, T.; Yano, K.; Yokoyama, J.; Yokozawa, T.; Yoon, T. H.; Yuzurihara, H.; Zeidler, S.; Zhao, Y.; Zheng, L.; Agatsuma, K.; Akiyama, Y.; Arai, N.; Asano, M.; Bertolini, A.; Fujisawa, M.; Goetz, R.; Guscott, J.; Hashimoto, Y.; Hayashida, Y.; Hennes, E.; Hirai, K.; Hirayama, T.; Ishitsuka, H.; Kato, J.; Khalaidovski, A.; Koike, S.; Kumeta, A.; Miener, T.; Morioka, M.; Mueller, C. L.; Narita, T.; Oda, Y.; Ogawa, T.; Sekiguchi, T.; Tamura, H.; Tanner, D. B.; Tokoku, C.; Toritani, M.; Utsuki, T.; Uyeshima, M.; van den Brand, J. F. J.; van Heijningen, J. V.; Yamaguchi, S.; Yanagida, A. Bibcode: 2018PTEP.2018a3F01A Altcode: 2017arXiv171200148A The major construction and initial-phase operation of a second-generation gravitational-wave detector, KAGRA, has been completed. The entire 3 km detector is installed underground in a mine in order to be isolated from background seismic vibrations on the surface. This allows us to achieve a good sensitivity at low frequencies and high stability of the detector. Bare-bones equipment for the interferometer operation has been installed and the first test run was accomplished in March and April of 2016 with a rather simple configuration. The initial configuration of KAGRA is called iKAGRA. In this paper, we summarize the construction of KAGRA, including a study of the advantages and challenges of building an underground detector, and the operation of the iKAGRA interferometer together with the geophysics interferometer that has been constructed in the same tunnel. Title: Observation of a Large-scale Quasi-circular Secondary Ribbon Associated with Successive Flares and a Halo CME Authors: Lim, Eun-Kyung; Yurchyshyn, Vasyl; Kumar, Pankaj; Cho, Kyuhyoun; Jiang, Chaowei; Kim, Sujin; Yang, Heesu; Chae, Jongchul; Cho, Kyung-Suk; Lee, Jeongwoo Bibcode: 2017ApJ...850..167L Altcode: 2017arXiv171100622L Solar flare ribbons provide an important clue to the magnetic reconnection process and associated magnetic field topology in the solar corona. We detected a large-scale secondary flare ribbon of a circular shape that developed in association with two successive M-class flares and one coronal mass ejection. The ribbon revealed interesting properties such as (1) a quasi-circular shape and enclosing the central active region (AR); (2) the size as large as 500″ by 650″ (3) successive brightenings in the clockwise direction at a speed of 160 km s-1 starting from the nearest position to the flaring sunspots; (4) radial contraction and expansion in the northern and the southern part, respectively, at speeds of ≤10 km s-1. Using multi-wavelength data from Solar Dynamics Observatory, RHESSI, XRT, and Nobeyama, along with magnetic field extrapolations, we found that: (1) the secondary ribbon location is consistent with those of the field line footpoints of a fan-shaped magnetic structure that connects the flaring region and the ambient decaying field; (2) the second M2.6 flare occurred when the expanding coronal loops driven by the first M2.0 flare encountered the background decayed field; (3) immediately after the second flare, the secondary ribbon developed along with dimming regions. Based on our findings, we suggest that interaction between the expanding sigmoid field and the overlying fan-shaped field triggered the secondary reconnection that resulted in the field opening and formation of the quasi-circular secondary ribbon. We thus conclude that interaction between the AR and the ambient large-scale fields should be taken into account to fully understand the entire eruption process. Title: Interplanetary Magnetic Flux Ropes as Agents Connecting Solar Eruptions and Geomagnetic Activities Authors: Marubashi, K.; Cho, K. -S.; Ishibashi, H. Bibcode: 2017SoPh..292..189M Altcode: We investigate the solar wind structure for 11 cases that were selected for the campaign study promoted by the International Study of Earth-affecting Solar Transients (ISEST) MiniMax24 Working Group 4. We can identify clear flux rope signatures in nine cases. The geometries of the nine interplanetary magnetic flux ropes (IFRs) are examined with a model-fitting analysis with cylindrical and toroidal force-free flux rope models. For seven cases in which magnetic fields in the solar source regions were observed, we compare the IFR geometries with magnetic structures in their solar source regions. As a result, we can confirm the coincidence between the IFR orientation and the orientation of the magnetic polarity inversion line (PIL) for six cases, as well as the so-called helicity rule as regards the handedness of the magnetic chirality of the IFR, depending on which hemisphere of the Sun the IFR originated from, the northern or southern hemisphere; namely, the IFR has right-handed (left-handed) magnetic chirality when it is formed in the southern (northern) hemisphere of the Sun. The relationship between the orientation of IFRs and PILs can be taken as evidence that the flux rope structure created in the corona is in most cases carried through interplanetary space with its orientation maintained. In order to predict magnetic field variations on Earth from observations of solar eruptions, further studies are needed about the propagation of IFRs because magnetic fields observed at Earth significantly change depending on which part of the IFR hits the Earth. Title: Toward a Next Generation Solar Coronagraph: Development of a Compact Diagnostic Coronagraph on the ISS Authors: Cho, K. -S.; Bong, S. -C.; Choi, S.; Yang, H.; Kim, J.; Baek, J. -H.; Park, J.; Lim, E. -K.; Kim, R. -S.; Kim, S.; Kim, Y. -H.; Park, Y. -D.; Clarke, S. W.; Davila, J. M.; Gopalswamy, N.; Nakariakov, V. M.; Li, B.; Pinto, R. F. Bibcode: 2017JKAS...50..139C Altcode: The Korea Astronomy and Space Science Institute plans to develop a coronagraph in collaboration with National Aeronautics and Space Administration (NASA) and to install it on the International Space Station (ISS). The coronagraph is an externally occulted one-stage coronagraph with a field of view from 3 to 15 solar radii. The observation wavelength is approximately 400 nm, where strong Fraunhofer absorption lines from the photosphere experience thermal broadening and Doppler shift through scattering by coronal electrons. Photometric filter observations around this band enable the estimation of 2D electron temperature and electron velocity distribution in the corona. Together with a high time cadence (<12 min) of corona images used to determine the geometric and kinematic parameters of coronal mass ejections, the coronagraph will yield the spatial distribution of electron density by measuring the polarized brightness. For the purpose of technical demonstration, we intend to observe the total solar eclipse in August 2017 with the filter system and to perform a stratospheric balloon experiment in 2019 with the engineering model of the coronagraph. The coronagraph is planned to be installed on the ISS in 2021 for addressing a number of questions (e.g., coronal heating and solar wind acceleration) that are both fundamental and practically important in the physics of the solar corona and of the heliosphere. Title: A New Method for Coronal Magnetic Field Reconstruction Authors: Yi, Sibaek; Choe, Gwang-Son; Cho, Kyung-Suk; Kim, Kap-Sung Bibcode: 2017SPD....4810604Y Altcode: A precise way of coronal magnetic field reconstruction (extrapolation) is an indispensable tool for understanding of various solar activities. A variety of reconstruction codes have been developed so far and are available to researchers nowadays, but they more or less bear this and that shortcoming. In this paper, a new efficient method for coronal magnetic field reconstruction is presented. The method imposes only the normal components of magnetic field and current density at the bottom boundary to avoid the overspecification of the reconstruction problem, and employs vector potentials to guarantee the divergence-freeness. In our method, the normal component of current density is imposed, not by adjusting the tangential components of A, but by adjusting its normal component. This allows us to avoid a possible numerical instability that on and off arises in codes using A. In real reconstruction problems, the information for the lateral and top boundaries is absent. The arbitrariness of the boundary conditions imposed there as well as various preprocessing brings about the diversity of resulting solutions. We impose the source surface condition at the top boundary to accommodate flux imbalance, which always shows up in magnetograms. To enhance the convergence rate, we equip our code with a gradient-method type accelerator. Our code is tested on two analytical force-free solutions. When the solution is given only at the bottom boundary, our result surpasses competitors in most figures of merits devised by Schrijver et al. (2006). We have also applied our code to a real active region NOAA 11974, in which two M-class flares and a halo CME took place. The EUV observation shows a sudden appearance of an erupting loop before the first flare. Our numerical solutions show that two entwining flux tubes exist before the flare and their shackling is released after the CME with one of them opened up. We suggest that the erupting loop is created by magnetic reconnection between two entwining flux tubes and later appears in the coronagraph as the major constituent of the observed CME. Title: Comparison of coronal electron density distributions from MLSO/MK4, STEREO/SECCHI-COR1, SOHO/LASCO-C2, and SOHO/UVCS Authors: Lee, Jae-Ok; Cho, Kyung-Suk; Lee, Jin-Yi; Lee, Kyoung-Sun; Jang, Soojeong; Kim, Roksoon; Moon, Yong-Jae Bibcode: 2017SPD....4810635L Altcode: The coronal electron density is a fundamental and important physical quantity in solar physics. In this study, we compare coronal electron density distributions (CEDDs) derived from polarized brightness (pB) observations (MLSO/MK4 coronameter, STEREO/SECCHI-COR1 and SOHO/LASCO-C2 Coronagraphs) and one spectroscopic observation (SOHO/UVCS). For this, we consider data from January to August 2007 with the following conditions: the separation angle between the either of the STEREO spacecraft and Earth is less than 10 degrees and the observation time differences from one another are less than 1 minutes. In the pB observations, the CEDDs can be estimated by using inversion methods (Van de Hulst inversion for MK4 and LASCO-C2 pB data, and spherically symmetric polynomial approximation inversion for COR1 pB data). In the spectroscopic observation, we use the ratio of radiative and collisional components of the O vi doublet (O vi 1032 Å and 1037.6 Å) to estimate the CEDDs. We will show you some results about the estimated CEDDs and their dependence on different coronal regions such as backgournd corona and streamers. Title: Quasi-periodic Radio Bursts Associated with Fast-mode Waves near a Magnetic Null Point Authors: Kumar, Pankaj; Nakariakov, Valery M.; Cho, Kyung-Suk Bibcode: 2017ApJ...844..149K Altcode: 2017arXiv170609988K This paper presents an observation of quasi-periodic rapidly propagating waves observed in the Atmospheric Image Assembly (AIA) 171/193 Å channels during the impulsive phase of an M1.9 flare that occurred on 2012 May 7. The instant period was found to decrease from 240 to 120 s, and the speed of the wavefronts was in the range of ∼664-1416 km s-1. Almost simultaneously, quasi-periodic bursts with similar instant periods, ∼70 and ∼140 s, occur in the microwave emission and in decimetric type IV and type III radio bursts, and in the soft X-ray emission. The magnetic field configuration of the flare site was consistent with a breakout topology, I.e., a quadrupolar field along with a magnetic null point. The quasi-periodic rapidly propagating wavefronts of the EUV emission are interpreted as a fast magnetoacoustic wave train. The observations suggest that the fast-mode waves are generated during the quasi-periodic magnetic reconnection in the cusp region above the flare arcade loops. For the first time, we provide evidence of a tadpole wavelet signature at about 70-140 s in decimetric (245/610 MHz) radio bursts, along with the direct observation of a coronal fast-mode wave train in EUV. In addition, at AIA 131/193 Å we observed quasi-periodic EUV disturbances with periods of 95 and 240 s propagating downward at apparent speeds of 172-273 km s-1. The nature of these downward propagating disturbances is not revealed, but they could be connected to magnetoacoustic waves or periodically shrinking loops. Title: Multi-wavelength Observation of M-class Flare associated with Filament eruption Authors: Kim, Sujin; Yurchyshyn, Vasyl B.; Jiang, Chaowei; Cho, Kyung-Suk Bibcode: 2017SPD....4810822K Altcode: We have investigated a M-class flare associated with filament eruption which developed into a Halo CME. The M-class flare occurred in 2011 August 4. For this study, we used the Nobryama Radioheliograph (NoRH) 17 and 34 GHz, RHESSI Hard X-ray satellite, and Atmo- spheric Imaging Assembly (AIA) and the Heliospheric Magentic Imager(HMI) onboard the Solar Dynamic Observatory (SDO). During the pre-eruption phase, clear nonthermal emission was detected in microwaves of NoRH and hard-X-ray of RHESSI. At the moment that the nonthermal emission start, the nonthermal sources appeared at the one edge of the filament structure on a polarity inversion line, and the slowing rising filament structure in AIA 94A underwent a sudden acceleration on its ascendance. Magnetograms showed converging motion of magnetic elements at the source position of HXR and MW. Based on the results, we conjecture that the plausible trigger of the filament eruption is magnetic reconnections at the HXR source position by converging motion of magnetic elements. In addition, we will discuss on the magnetic flux variation before and after the eruption based on the result of Nonlinear force-free field model. Title: Multiwavelength observations of a flux rope formation by series of magnetic reconnection in the chromosphere Authors: Kumar, Pankaj; Yurchyshyn, Vasyl; Cho, Kyung-Suk; Wang, Haimin Bibcode: 2017A&A...603A..36K Altcode: 2017arXiv170309871K Using high-resolution observations from the 1.6 m New Solar Telescope (NST) operating at the Big Bear Solar Observatory (BBSO), we report direct evidence of merging and reconnection of cool Hα loops in the chromosphere during two homologous flares (B and C class) caused by a shear motion at the footpoints of two loops. The reconnection between these loops caused the formation of an unstable flux rope that showed counterclockwise rotation. The flux rope could not reach the height of torus instability and failed to form a coronal mass ejection. The HMI magnetograms revealed rotation of the negative and positive (N1/P2) polarity sunspots in the opposite directions, which increased the right- and left-handed twist in the magnetic structures rooted at N1/P2. Rapid photospheric flux cancellation (duration 20-30 min, rate ≈3.44 × 1020 Mx h-1) was observed during and even after the first B6.0 flare and continued until the end of the second C2.3 flare. The RHESSI X-ray sources were located at the site of the loop coalescence. To the best of our knowledge, such a clear interaction of chromospheric loops along with rapid flux cancellation has not been reported before. These high-resolution observations suggest the formation of a small flux rope by a series of magnetic reconnections within chromospheric loops that are associated with very rapid flux cancellation. Movies attached to Figs. 2, 7, 8, and 10 are available at http://www.aanda.org Title: Investigating the Origins of Two Extreme Solar Particle Events: Proton Source Profile and Associated Electromagnetic Emissions Authors: Kocharov, Leon; Pohjolainen, Silja; Mishev, Alexander; Reiner, Mike J.; Lee, Jeongwoo; Laitinen, Timo; Didkovsky, Leonid V.; Pizzo, Victor J.; Kim, Roksoon; Klassen, Andreas; Karlicky, Marian; Cho, Kyung-Suk; Gary, Dale E.; Usoskin, Ilya; Valtonen, Eino; Vainio, Rami Bibcode: 2017ApJ...839...79K Altcode: We analyze the high-energy particle emission from the Sun in two extreme solar particle events in which protons are accelerated to relativistic energies and can cause a significant signal even in the ground-based particle detectors. Analysis of a relativistic proton event is based on modeling of the particle transport and interaction, from a near-Sun source through the solar wind and the Earth’s magnetosphere and atmosphere to a detector on the ground. This allows us to deduce the time profile of the proton source at the Sun and compare it with observed electromagnetic emissions. The 1998 May 2 event is associated with a flare and a coronal mass ejection (CME), which were well observed by the Nançay Radioheliograph, thus the images of the radio sources are available. For the 2003 November 2 event, the low corona images of the CME liftoff obtained at the Mauna Loa Solar Observatory are available. Those complementary data sets are analyzed jointly with the broadband dynamic radio spectra, EUV images, and other data available for both events. We find a common scenario for both eruptions, including the flare’s dual impulsive phase, the CME-launch-associated decimetric-continuum burst, and the late, low-frequency type III radio bursts at the time of the relativistic proton injection into the interplanetary medium. The analysis supports the idea that the two considered events start with emission of relativistic protons previously accelerated during the flare and CME launch, then trapped in large-scale magnetic loops and later released by the expanding CME. Title: Impact of the Icme-Earth Geometry on the Strength of the Associated Geomagnetic Storm: The September 2014 and March 2015 Events Authors: Cho, K. S.; Marubashi, K.; Kim, R. S.; Park, S. H.; Lim, E. K.; Kim, S. J.; Kumar, P.; Yurchyshyn, V.; Moon, Y. J.; Lee, J. O. Bibcode: 2017JKAS...50...29C Altcode: No abstract at ADS Title: Relation of CME Speed and Magnetic Helicity in CME Source Regions on the Sun during the Early Phase of Solar Cycles 23 and 24 Authors: Kim, R. -S.; Park, S. -H.; Jang, S.; Cho, K. -S.; Lee, B. S. Bibcode: 2017SoPh..292...66K Altcode: To investigate the relations between coronal mass ejection (CME) speed and magnetic field properties measured in the photospheric surface of CME source regions, we selected 22 disk CMEs in the rising and early maximum phases of the current Solar Cycle 24. For the CME speed, we used two-dimensional (2D) projected speed observed by the Large Angle and Spectroscopic Coronagraph onboard the Solar and Heliospheric Observatory (SOHO/LASCO), as well as a 3D speed calculated from the triangulation method using multi-point observations. Two magnetic parameters of CME source regions were considered: the average of magnetic helicity injection rate and the total unsigned magnetic flux. We then classified the selected CMEs into two groups, showing: i) a monotonically increasing pattern with one sign of helicity (group A: 16 CMEs) and ii) a pattern of significant helicity injection followed by its sign reversal (group B: 6 CMEs). We found that: 1) 3D speed generally shows better correlations with the magnetic parameters than the 2D speed for 22 CME events in Solar Cycle 24; 2) 2D speed and the magnetic parameters of 22 CME events in this solar cycle have lower values than those of 47 CME events in Solar Cycle 23; 3) all events of group B in Solar Cycle 24 occur only after the beginning of the maximum phase, a trend well consistent with that shown in Solar Cycle 23; 4) the 2D speed and the helicity parameter of group B events continue to increase in the declining phase of Solar Cycle 23, while those of group A events abruptly decrease in the same period. Our results indicate that the two CME groups have a different tendency in the solar cycle variations of CME speed and the helicity parameters. Active regions that show a complex helicity evolution pattern tend to appear in the maximum and declining phases, while active regions with a relatively simple helicity evolution pattern appear throughout the whole solar cycle. Title: Which Bow Shock Theory, Gasdynamic or Magnetohydrodynamic, Better Explains CME Stand-off Distance Ratios from LASCO-C2 Observations ? Authors: Lee, Jae-Ok; Moon, Y. -J.; Lee, Jin-Yi; Kim, R. -S.; Cho, K. -S. Bibcode: 2017ApJ...838...70L Altcode: It is generally believed that fast coronal mass ejections (CMEs) can generate their associated shocks, which are characterized by faint structures ahead of CMEs in white-light coronagraph images. In this study, we examine whether the observational stand-off distance ratio, defined as the CME stand-off distance divided by its radius, can be explained by bow shock theories. Of 535 SOHO/LASCO CMEs (from 1996 to 2015) with speeds greater than 1000 km s-1 and angular widths wider than 60°, we select 18 limb CMEs with the following conditions: (1) their Alfvénic Mach numbers are greater than one under Mann’s magnetic field and Saito’s density distributions; and (2) the shock structures ahead of the CMEs are well identified. We determine observational CME stand-off distance ratios by using brightness profiles from LASCO-C2 observations. We compare our estimates with theoretical stand-off distance ratios from gasdynamic (GD) and magnetohydrodynamic (MHD) theories. The main results are as follows. Under the GD theory, 39% (7/18) of the CMEs are explained in the acceptable ranges of adiabatic gamma (γ) and CME geometry. Under the MHD theory, all the events are well explained when we consider quasi-parallel MHD shocks with γ = 5/3. When we use polarized brightness (pB) measurements for coronal density distributions, we also find similar results: 8% (1/12) under GD theory and 100% (12/12) under MHD theory. Our results demonstrate that the bow shock relationships based on MHD theory are more suitable than those based on GD theory for analyzing CME-driven shock signatures. Title: Characteristics of radio-loud CME Authors: Pankaj Kumar; P. K., Manoharan; Cho, K. S. Bibcode: 2017ursi.confE...1P Altcode: In this paper, we study the characteristics of 46 radio-loud (RL) Coronal Mass Ejections (CMEs) which occurred during 1997-2006. All these RL CMEs were associated with M- and X-class flares. We selected 46 RL CMEs, out of which 26 events (57%) were associated with Solar Energetic Particle (SEP) events detected at 1 AU. Furthermore, we study the link between the flare accelerated electrons in the low corona and protons at 1 AU and found a positive correlation (30%). It suggests the link between the injection sites for electrons and protons, which are most likely accelerated at the flare current sheet. We also study the relationship between the CME speed and peak proton flux (>10 MeV) at 1 AU and found a good correlation ( 60%), which suggests the proton acceleration by CME driven shocks. In addition, we found two branches (lower and upper) of SEP events showing different characteristics. The lower branch SEP events are associated with impulsive rise with more proton flux whereas the upper branch SEP events exhibit gradual rise and less proton flux. We suggest that flares (current sheet) and CMEs (shocks) both are involved in the particle acceleration for the lower branch, whereas in the upper branch mostly CME driven shocks play an important role in the particle acceleration. Title: High-resolution Observations of a White-light Flare with NST Authors: Yurchyshyn, V.; Kumar, P.; Abramenko, V.; Xu, Y.; Goode, P. R.; Cho, K. -S.; Lim, E. -K. Bibcode: 2017ApJ...838...32Y Altcode: Using high-resolution data from the New Solar Telescope, we studied fine spatial and temporal details of an M1.3 white-light (WL) flare, which was one of three homologous solar flares (C6.8, M1.3, and M2.3) observed in close proximity to the west solar limb on 2014 October 29 in NOAA active region 12192. We report that the TiO WL flare consists of compact and intense cores surrounded by less intense spatial halos. The strong and compact WL cores were measured to be ≈ 0.2 Mm across, with an area of about 1014 cm2. Several TiO features were not cospatial with Hα flare ribbons and were displaced toward the disk center by about 500 km, which suggests that the TiO and Hα radiation probably did not originate in the same chromospheric volume. The observed TiO intensity enhancements are not normally distributed and are structured by the magnetic field of the penumbra. Title: Determination of the Alfvén Speed and Plasma-beta Using the Seismology of Sunspot Umbra Authors: Cho, I. -H.; Cho, K. -S.; Bong, S. -C.; Moon, Y. -J.; Nakariakov, V. M.; Park, J.; Baek, J. -H.; Choi, S.; Kim, Y. -H.; Lee, J. Bibcode: 2017ApJ...837L..11C Altcode: For 478 centrally located sunspots observed in the optical continuum with Solar Dynamics Observatory/Helioseismic Magnetic Imager, we perform seismological diagnostics of the physical parameters of umbral photospheres. The new technique is based on the theory of slow magnetoacoustic waves in a non-isothermally stratified photosphere with a uniform vertical magnetic field. We construct a map of the weighted frequency of three-minute oscillations inside the umbra and use it for the estimation of the Alfvén speed, plasma-beta, and mass density within the umbra. We find the umbral mean Alfvén speed ranges between 10.5 and 7.5 km s-1 and is negatively correlated with magnetic field strength. The umbral mean plasma-beta is found to range approximately between 0.65 and 1.15 and does not vary significantly from pores to mature sunspots. The mean density ranges between (1-6) × 10-4 kg m-3 and shows a strong positive correlation with magnetic field strength. Title: Observation of a Short Period Quasi-periodic Pulsation in Solar X-Ray, Microwave, and EUV Emissions Authors: Kumar, Pankaj; Nakariakov, Valery M.; Cho, Kyung-Suk Bibcode: 2017ApJ...836..121K Altcode: 2017arXiv170102159K This paper presents the multiwavelength analysis of a 13 s quasi-periodic pulsation (QPP) observed in hard X-ray (12-300 keV) and microwave (4.9-34 GHz) emissions during a C-class flare that occurred on 2015 September 21. Atmospheric Image Assembly (AIA) 304 and 171 Å images show an emerging loop/flux tube (L1) moving radially outward, which interacts with the preexisting structures within the active region (AR). The QPP was observed during the expansion of and rising motion of L1. The Nobeyama Radioheliograph microwave images in 17/34 GHz channels reveal a single radio source that was co-spatial with a neighboring loop (L2). In addition, using AIA 304 Å images, we detected intensity oscillations in the legs of L2 with a period of about 26 s. A similar oscillation period was observed in the GOES soft X-ray flux derivative. This oscillation period seems to increase with time. We suggest that the observed QPP is most likely generated by the interaction between L2 and L3 observed in the AIA hot channels (131 and 94 Å). The merging speed of loops L2 and L3 was ∼35 km s-1. L1 was destroyed possibly by its interaction with preexisting structures in the AR, and produced a cool jet with the speed of ∼106-118 km s-1 associated with a narrow CME (∼770 km s-1). Another mechanism of the QPP in terms of a sausage oscillation of the loop (L2) is also possible. Title: Chromospheric Plasma Ejections in a Light Bridge of a Sunspot Authors: Song, Donguk; Chae, Jongchul; Yurchyshyn, Vasyl; Lim, Eun-Kyung; Cho, Kyung-Suk; Yang, Heesu; Cho, Kyuhyoun; Kwak, Hannah Bibcode: 2017ApJ...835..240S Altcode: 2017arXiv170106808S It is well-known that light bridges (LBs) inside a sunspot produce small-scale plasma ejections and transient brightenings in the chromosphere, but the nature and origin of such phenomena are still unclear. Utilizing the high-spatial and high-temporal resolution spectral data taken with the Fast Imaging Solar Spectrograph and the TiO 7057 Å broadband filter images installed at the 1.6 m New Solar Telescope of Big Bear Solar Observatory, we report arcsecond-scale chromospheric plasma ejections (1.″7) inside a LB. Interestingly, the ejections are found to be a manifestation of upwardly propagating shock waves as evidenced by the sawtooth patterns seen in the temporal-spectral plots of the Ca II 8542 Å and Hα intensities. We also found a fine-scale photospheric pattern (1″) diverging with a speed of about 2 km s-1 two minutes before the plasma ejections, which seems to be a manifestation of magnetic flux emergence. As a response to the plasma ejections, the corona displayed small-scale transient brightenings. Based on our findings, we suggest that the shock waves can be excited by the local disturbance caused by magnetic reconnection between the emerging flux inside the LB and the adjacent umbral magnetic field. The disturbance generates slow-mode waves, which soon develop into shock waves, and manifest themselves as the arcsecond-scale plasma ejections. It also appears that the dissipation of mechanical energy in the shock waves can heat the local corona. Title: Pre-eruption Oscillations in Thin and Long Features in a Quiescent Filament Authors: Joshi, Anand D.; Hanaoka, Yoichiro; Suematsu, Yoshinori; Morita, Satoshi; Yurchyshyn, Vasyl; Cho, Kyung-Suk Bibcode: 2016ApJ...833..243J Altcode: 2016arXiv161204917J We investigate the eruption of a quiescent filament located close to an active region. Large-scale activation was observed in only half of the filament in the form of pre-eruption oscillations. Consequently only this half erupted nearly 30 hr after the oscillations commenced. Time-slice diagrams of 171 Å images from the Atmospheric Imaging Assembly were used to study the oscillations. These were observed in several thin and long features connecting the filament spine to the chromosphere below. This study traces the origin of such features and proposes their possible interpretation. Small-scale magnetic flux cancellation accompanied by a brightening was observed at the footpoint of the features shortly before their appearance, in images recorded by the Helioseismic and Magnetic Imager. A slow rise of the filament was detected in addition to the oscillations, indicating a gradual loss of equilibrium. Our analysis indicates that a change in magnetic field connectivity between two neighbouring active regions and the quiescent filament resulted in a weakening of the overlying arcade of the filament, leading to its eruption. It is also suggested that the oscillating features are filament barbs, and the oscillations are a manifestation during the pre-eruption phase of the filaments. Title: Pre-flare Coronal Jet and Evolutionary Phases of a Solar Eruptive Prominence Associated with the M1.8 Flare: SDO and RHESSI Observations Authors: Joshi, Bhuwan; Kushwaha, Upendra; Veronig, Astrid M.; Cho, K. -S. Bibcode: 2016ApJ...832..130J Altcode: 2016arXiv161103629J We investigate the triggering, activation, and ejection of a solar eruptive prominence that occurred in a multi-polar flux system of active region NOAA 11548 on 2012 August 18 by analyzing data from the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory, the Reuven Ramaty High Energy Solar Spectroscopic Imager, and the Extreme Ultraviolet Imager/Sun Earth Connection Coronal and Heliospheric Investigation on board the Solar Terrestrial Relation Observatory. Prior to the prominence activation, we observed striking coronal activities in the form of a blowout jet, which is associated with the rapid eruption of a cool flux rope. Furthermore, the jet-associated flux rope eruption underwent splitting and rotation during its outward expansion. These coronal activities are followed by the prominence activation during which it slowly rises with a speed of ∼12 km s-1 while the region below the prominence emits gradually varying EUV and thermal X-ray emissions. From these observations, we propose that the prominence eruption is a complex, multi-step phenomenon in which a combination of internal (tether-cutting reconnection) and external (I.e., pre-eruption coronal activities) processes are involved. The prominence underwent catastrophic loss of equilibrium with the onset of the impulsive phase of an M1.8 flare, suggesting large-scale energy release by coronal magnetic reconnection. We obtained signatures of particle acceleration in the form of power-law spectra with hard electron spectral index (δ ∼ 3) and strong HXR footpoint sources. During the impulsive phase, a hot EUV plasmoid was observed below the apex of the erupting prominence that ejected in the direction of the prominence with a speed of ∼177 km s-1. The temporal, spatial, and kinematic correlations between the erupting prominence and the plasmoid imply that the magnetic reconnection supported the fast ejection of prominence in the lower corona. Title: The 17 March 2015 storm: the associated magnetic flux rope structure and the storm development Authors: Marubashi, Katsuhide; Cho, Kyung-Suk; Kim, Rok-Soon; Kim, Sujin; Park, Sung-Hong; Ishibashi, Hiromitsu Bibcode: 2016EP&S...68..173M Altcode: The objective of this study is (1) to determine the magnetic cloud (MC) structure associated with the 17 March 2015 storm and (2) to gain an insight into how the storm developed responding to the solar wind conditions. First, we search MC geometries which can explain the observed solar wind magnetic fields by fitting to both cylindrical and toroidal flux rope models. Then, we examine how the resultant MC geometries can be connected to the solar source region to find out the most plausible model for the observed MC. We conclude that the observations are most consistently explained by a toroidal flux rope with the torus plane nearly parallel to the ecliptic plane. It is emphasized that the observations are characterized by the peculiar spacecraft crossing through the MC, in that the magnetic fields to be observed are southward throughout the passage. For understanding of the storm development, we first estimate the injection rate of the storm ring current from the observed Dst variation. Then, we derive an expression to calculate the estimated injection rate from the observed solar wind variations. The point of the method is to evaluate the injection rate by the convolution of the dawn-to-dusk electric field in the solar wind and a response function. By using the optimum response function thus determined, we obtain a modeled Dst variation from the solar wind data, which is in good agreement with the observed Dst variation. The agreement supports the validity of our method to derive an expression for the ring current injection rate as a function of the solar wind variation.[Figure not available: see fulltext.] Title: Pre-Eruption Oscillations in Quiescent Filament Observed in AIA 171 Å Authors: Joshi, Anand D.; Yurchyshyn, Vasyl; Cho, Kyung-Suk Bibcode: 2016usc..confE..62J Altcode: A large quiescent filament located near the south-west limb of the Sun underwent an eruption on 14 August 2013. Shortly before the eruption two flares occur in NOAA Active Region (AR) 11817, located near the filament. The temporal and spatial proximity suggests that the flares caused the filament to erupt. However, there is no extreme ultraviolet (EUV) wave or ejection which seemed to cause this. We use 171 Å images for over two days before the eruption from Atmospheric Imaging Assembly (AIA) on board Solar Dynamics Observatory (SDO) to investigate this event. We observe oscillations in the western portion of the quiescent filament almost 40 hours prior to eruption, but not so much in the eastern portion. For several hours prior to eruption, the western portion is seen to undergo a slow rise. Subsequently, it is this western portion which erupts, while the eastern portion does not. We also use Helioseismic and Magnetic Imager (HMI) to study changes in the active region, and find that along with a continuous emergence of magnetic flux in the region, there was also a migration of polarity producing a large shear. We make use of the hmi.sharp to determine shear in the active region. We suggest that the oscillations are a result of natural perturbation, and the flares acted as a destabilising factor which resulted in the eruption. Title: Comparison of Damped Oscillations in Solar and Stellar X-Ray flares Authors: Cho, I. -H.; Cho, K. -S.; Nakariakov, V. M.; Kim, S.; Kumar, P. Bibcode: 2016ApJ...830..110C Altcode: We explore the similarity and difference of the quasi-periodic pulsations (QPPs) observed in the decay phase of solar and stellar flares at X-rays. We identified 42 solar flares with pronounced QPPs, observed with RHESSI, and 36 stellar flares with QPPs, observed with XMM-Newton. The empirical mode decomposition (EMD) method and least-squares fit by a damped sine function were applied to obtain the periods (P) and damping times (τ) of the QPPs. We found that (1) the periods and damping times of the stellar QPPs are 16.21 ± 15.86 minutes and 27.21 ± 28.73 minutes, while those of the solar QPPs are 0.90 ± 0.56 and 1.53 ± 1.10 minutes, respectively; (2) the ratios of the damping times to the periods (τ /P) observed in the stellar QPPs (1.69 ± 0.56) are statistically identical to those of solar QPPs (1.74 ± 0.77) and (3) the scalings of the QPP damping time with the period are well described by the power law in both solar and stellar cases. The power indices of the solar and stellar QPPs are 0.96 ± 0.10 and 0.98+/- 0.05, respectively. This scaling is consistent with the scalings found for standing slow magnetoacoustic and kink modes in solar coronal loops. Thus, we propose that the underlying mechanism responsible for the stellar QPPs is the natural magnetohydrodynamic oscillation in the flaring or adjacent coronal loops, as in the case of solar flares. Title: Flare-generated Shock Wave Propagation through Solar Coronal Arcade Loops and an Associated Type II Radio Burst Authors: Kumar, Pankaj; Innes, D. E.; Cho, Kyung-Suk Bibcode: 2016ApJ...828...28K Altcode: 2016arXiv160605056K This paper presents multiwavelength observations of a flare-generated type II radio burst. The kinematics of the shock derived from the type II burst closely match a fast extreme ultraviolet (EUV) wave seen propagating through coronal arcade loops. The EUV wave was closely associated with an impulsive M1.0 flare without a related coronal mass ejection, and was triggered at one of the footpoints of the arcade loops in active region NOAA 12035. It was initially observed in the 335 Å images from the Atmospheric Image Assembly with a speed of ∼800 km s-1 and it accelerated to ∼1490 km s-1 after passing through the arcade loops. A fan-spine magnetic topology was revealed at the flare site. A small, confined filament eruption (∼340 km s-1) was also observed moving in the opposite direction to the EUV wave. We suggest that breakout reconnection in the fan-spine topology triggered the flare and associated EUV wave that propagated as a fast shock through the arcade loops. Title: Characteristics of radio-loud CMEs Authors: Kumar, Pankaj; Manoharan, P. K.; Cho, K. S. Bibcode: 2016ursi.confE...2K Altcode: In this paper, we study the characteristics of 46 radio-loud (RL) Coronal Mass Ejections (CMEs) which occurred during 1997-2006. All these RL CMEs were associated with M- and X-class flares. We selected 46 RL CMEs, out of which 26 events (57%) were associated with Solar Energetic Particle (SEP) events detected at 1 AU. Furthermore, we study the link between the flare accelerated electrons in the low corona and protons at 1 AU and found a positive correlation (30%). It suggests the link between the injection sites for electrons and protons, which are most likely accelerated at the flare current sheet. We also study the relation between the CME speed and peak proton flux (>10 MeV) at 1 AU and found a good correlation (~60%), which suggests the proton acceleration by CME-driven shocks. In addition, we found two branches (lower and upper) of SEP events showing different characteristics. The lower branch SEP events are associated with impulsive rise with more proton flux whereas the upper branch SEP events exhibit gradual rise and less proton flux. We suggest that flares (current sheet) and CMEs (shocks) both are involved in the particle acceleration for the lower branch, whereas in the upper branch mostly CME-driven shocks play an important role in the particle acceleration. Title: Ultra-Narrow Negative Flare Front Observed in Helium-10830 Å Using the1.6m New Solar Telescope Authors: Xu, Yan; Cao, Wenda; Ding, Mingde; Kleint, Lucia; Su, Jiangtao; Liu, Chang; Ji, Haisheng; Chae, Jongchul; Jing, Ju; Cho, Kyuhyoun; Cho, Kyung-Suk; Gary, Dale E.; Wang, Haimin Bibcode: 2016SPD....47.0633X Altcode: Solar flares are sudden flashes of brightness on the Sun and are often associated with coronal mass ejections and solar energetic particles that have adverse effects on the near-Earth environment. By definition, flares are usually referred to as bright features resulting from excess emission. Using the newly commissioned 1.6-m New Solar Telescope at Big Bear Solar Observatory, we show a striking “negative” flare with a narrow but unambiguous “dark” moving front observed in He I 10830 Å, which is as narrow as 340 km and is associated with distinct spectral characteristics in Hα and Mg II lines. Theoretically, such negative contrast in He I 10830 Å can be produced under special circumstances by nonthermal electron collisions or photoionization followed by recombination. Our discovery, made possible due to unprecedented spatial resolution, confirms the presence of the required plasma conditions and provides unique information in understanding the energy release and radiative transfer in solar flares. Title: Observation of a Quasiperiodic Pulsation in Hard X-Ray, Radio, and Extreme-ultraviolet Wavelengths Authors: Kumar, Pankaj; Nakariakov, Valery M.; Cho, Kyung-Suk Bibcode: 2016ApJ...822....7K Altcode: 2016arXiv160303121K We present a multiwavelength analysis of a quasiperiodic pulsation (QPP) observed in the hard X-ray (HXR), radio, and extreme-ultraviolet (EUV) channels during an M1.9 flare that occurred on 2011 September 23-24. The nonthermal HXR emission in 25-50 keV observed by RHESSI shows five distinct impulsive peaks of decaying amplitude with a period of about 3 minutes. A similar QPP was observed in the microwave emission recorded by the Nobeyama Radioheliograph and Polarimeter in the 2, 3.75, 9.4, and 17 GHz channels. Interestingly, the 3-minute QPP was also observed in the metric and decimetric radio frequencies (25-180, 245, 610 MHz) as repetitive type III bursts. Multiwavelength observations from the Solar Dynamics Observatory/Atmospheric Image Assembly, Hinode/SOT, and Solar TErrestrial RElations Observatory/SECCHI suggest a fan-spine topology at the eruption site, associated with the formation of a quasi-circular ribbon during the flare. A small filament was observed below the fan loops before the flare onset. The filament rose slowly and interacted with the ambient field. This behavior was followed by an untwisting motion of the filament. Two different structures of the filament showed an approximately 3-minute periodic alternate rotation in the clockwise and counterclockwise directions. The 3-minute QPP was found to highly correlate with 3-minute oscillations in a nearby sunspot. We suggest that the periodic reconnection (modulated either by a sunspot slow-mode wave or by an untwisting filament) at a magnetic null point most likely causes the repetitive particle acceleration, generating the QPP observed in HXR, microwave, and type III radio bursts. Title: Comparison between 2D and 3D Parameters of 306 Front-side Halo CMEs from 2009 to 2013 Authors: Jang, Soojeong; Moon, Y. -J.; Kim, R. -S.; Lee, Harim; Cho, K. -S. Bibcode: 2016ApJ...821...95J Altcode: We investigate 306 LASCO front-side halo (partial and full) CMEs from 2009 to 2013, which are well-observed by both the Solar and Heliospheric Observatory (SOHO) and the Solar TErrestrial RElations Observatory (STEREO). These CMEs have two-dimensional (2D) parameters, such as speed, angular width, and propagation direction, from a single spacecraft (SOHO), as well as three-dimensional (3D) parameters from a multi-spacecraft (STEREO). These 2D CME parameters, which are based on plane-of-sky observations, are taken from the SOHO LASCO CME catalog and the NGDC flare catalog. We have determined their 3D CME parameters using the Stereoscopic CME analysis tool (StereoCAT) provided by the Community Coordinated Modeling Center at NASA. We compare 2D and 3D CME parameters, making this the most comprehensive statistical study on CME 3D parameters. As a result, we find that 2D speeds underestimate the 3D speed by about 20%. The 3D width ranges from 30° to 158°, values which are much smaller than the 2D widths with a mean value of 225°. We also find that the ratio between the 2D and 3D widths decreases with central meridian distance. The 3D propagation directions are similar to the flare locations, with a mean absolute difference of about 13°. The width-speed relationship in 3D is much stronger than that in 2D. Title: a New Method to Determine the Temperature of CMES Using a Coronagraph Filter System Authors: Cho, Kyuhyoun; Chae, Jongchul; Lim, Eun-Kyung; Cho, Kyung-Suk; Bong, Su-Chan; Yang, Heesu Bibcode: 2016JKAS...49...45C Altcode: 2016arXiv160307047C The coronagraph is an instrument enables the investigation of faint features in the vicinity of the Sun, particularly coronal mass ejections (CMEs). So far coronagraphic observations have been mainly used to determine the geometric and kinematic parameters of CMEs. Here, we introduce a new method for the determination of CME temperature using a two filter (4025 A and 3934 A) coronagraph system. The thermal motion of free electrons in CMEs broadens the absorption lines in the optical spectra that are produced by the Thomson scattering of visible light originating in the photosphere, which affects the intensity ratio at two different wavelengths. Thus the CME temperature can be inferred from the intensity ratio measured by the two filter coronagraph system. We demonstrate the method by invoking the graduated cylindrical shell (GCS) model for the 3 dimensional CME density distribution and discuss its significance. Title: Observations of a Series of Flares and Associated Jet-like Eruptions Driven by the Emergence of Twisted Magnetic Fields Authors: Lim, Eun-Kyung; Yurchyshyn, Vasyl; Park, Sung-Hong; Kim, Sujin; Cho, Kyung-Suk; Kumar, Pankaj; Chae, Jongchul; Yang, Heesu; Cho, Kyuhyoun; Song, Donguk; Kim, Yeon-Han Bibcode: 2016ApJ...817...39L Altcode: 2015arXiv151201330L We studied temporal changes of morphological and magnetic properties of a succession of four confined flares followed by an eruptive flare using the high-resolution New Solar Telescope (NST) operating at the Big Bear Solar Observatory (BBSO) and Helioseismic and Magnetic Imager (HMI) magnetograms and Atmospheric Image Assembly (AIA) EUV images provided by the Solar Dynamics Observatory (SDO). From the NST/Hα and the SDO/AIA 304 Å observations we found that each flare developed a jet structure that evolved in a manner similar to evolution of the blowout jet: (1) an inverted-Y-shaped jet appeared and drifted away from its initial position; (2) jets formed a curtain-like structure that consisted of many fine threads accompanied by subsequent brightenings near the footpoints of the fine threads; and finally, (3) the jet showed a twisted structure visible near the flare maximum. Analysis of the HMI data showed that both the negative magnetic flux and the magnetic helicity have been gradually increasing in the positive-polarity region, indicating the continuous injection of magnetic twist before and during the series of flares. Based on these results, we suggest that the continuous emergence of twisted magnetic flux played an important role in producing successive flares and developing a series of blowout jets. Title: Non-Uniqueness of the Geometry of Interplanetary Magnetic Flux Ropes Obtained from Model-Fitting Authors: Marubashi, K.; Cho, K. -S. Bibcode: 2015SunGe..10..119M Altcode: Since the early recognition of the important role of interplanetary magnetic flux ropes (IPFRs) to carry the southward magnetic fields to the Earth, many attempts have been made to determine the structure of the IPFRs by model-fitting analyses to the interplanetary magnetic field variations. This paper describes the results of fitting analyses for three selected solar wind structures in the latter half of 2014. In the fitting analysis a special attention was paid to identification of all the possible models or geometries that can reproduce the observed magnetic field variation. As a result, three or four geometries have been found for each of the three cases. The non-uniqueness of the fitted results include (1) the different geometries naturally stemming from the difference in the models used for fitting, and (2) an unexpected result that either of magnetic field chirality, left-handed and right-handed, can reproduce the observation in some cases. Thus we conclude that the model-fitting cannot always give us a unique geometry of the observed magnetic flux rope. In addition, we have found that the magnetic field chirality of a flux rope cannot be uniquely inferred from the sense of field vector rotation observed in the plane normal to the Earth-Sun line; the sense of rotation changes depending on the direction of the flux rope axis. These findings exert an important impact on the studies aimed at the geometrical relationships between the flux ropes and the magnetic field structures in the solar corona where the flux ropes were produced, such studies being an important step toward predicting geomagnetic storms based on observations of solar eruption phenomena. Title: Development of AN Automatic Observation System for Korean e-CALLISTO Station Authors: Park, Jongyeob; Choi, Seonghwan; Bong, Su-Chan; Kwon, Yongjun; Baek, Ji-Hye; Jang, Bi-Ho; Cho, Kyung-Suk; Moon, Yong-Jae; Monstein, Christian Bibcode: 2015PKAS...30..811P Altcode: No abstract at ADS Title: Transfer of Real-time Dynamic Radiation Environment Assimilation Model; Research to Operation Authors: Cho, K. S. F.; Hwang, J.; Shin, D. K.; Kim, G. J.; Morley, S.; Henderson, M. G.; Friedel, R. H.; Reeves, G. D. Bibcode: 2015AGUFMSM41A2477C Altcode: Real-time Dynamic Radiation Environment Assimilation Model (rtDREAM) was developed by LANL for nowcast of energetic electrons' flux at the radiation belt to quantify potential risks from radiation damage at the satellites. Assimilated data are from multiple sources including LANL assets (GEO, GPS). For transfer from research to operation of the rtDREAM code, LANL/KSWC/NOAA makes a Memorandum Of Understanding (MOU) on the collaboration between three parts. By this MOU, KWSC/RRA provides all the support for transitioning the research version of DREAM to operations. KASI is primarily responsible for providing all the interfaces between the current scientific output formats of the code and useful space weather products that can be used and accessed through the web. In the second phase, KASI will be responsible in performing the work needed to transform the Van Allen Probes beacon data into "DREAM ready" inputs. KASI will also provide the "operational" code framework and additional data preparation, model output, display and web page codes back to LANL and SWPC. KASI is already a NASA partnering ground station for the Van Allen Probes' space weather beacon data and can here show use and utility of these data for comparison between rtDREAM and observations by web. NOAA has offered to take on some of the data processing tasks specific to the GOES data. Title: Multiwavelength Observations of a Slow-rise, Multistep X1.6 Flare and the Associated Eruption Authors: Yurchyshyn, V.; Kumar, P.; Cho, K. -S.; Lim, E. -K.; Abramenko, V. I. Bibcode: 2015ApJ...812..172Y Altcode: Using multiwavelength observations, we studied a slow-rise, multistep X1.6 flare that began on 2014 November 7 as a localized eruption of core fields inside a δ-sunspot and later engulfed the entire active region (AR). This flare event was associated with formation of two systems of post-eruption arcades (PEAs) and several J-shaped flare ribbons showing extremely fine details, irreversible changes in the photospheric magnetic fields, and it was accompanied by a fast and wide coronal mass ejection. Data from the Solar Dynamics Observatory and IRIS spacecraft, along with the ground-based data from the New Solar Telescope, present evidence that (i) the flare and the eruption were directly triggered by a flux emergence that occurred inside a δ-sunspot at the boundary between two umbrae; (ii) this event represented an example of the formation of an unstable flux rope observed only in hot AIA channels (131 and 94 Å) and LASCO C2 coronagraph images; (iii) the global PEA spanned the entire AR and was due to global-scale reconnection occurring at heights of about one solar radius, indicating the global spatial and temporal scale of the eruption. Title: Detection of a Fine-scale Discontinuity of Photospheric Magnetic Fields Associated with Solar Coronal Loop Brightenings Authors: Song, Donguk; Chae, Jongchul; Park, Soyoung; Cho, Kyung-Suk; Lim, Eun-Kyung; Ahn, Kwangsu; Cao, Wenda Bibcode: 2015ApJ...810L..16S Altcode: We present the transient brightening of a coronal loop and an associated fine-scale magnetic discontinuity detected in the photosphere. Utilizing the high-resolution data taken with the Fast Imaging Solar Spectrograph and InfraRed Imaging Magnetograph of the New Solar Telescope at Big Bear Solar Observatory, we detect a narrow lane of intense horizontal magnetic field representing a magnetic discontinuity. It was visible as a dark lane partially encircling a pore in the continuum image, and was located near one of the footpoints of a small coronal loop that experienced transient brightenings. The horizontal field strength gradually increased before the loop brightening, and then rapidly decreased in the impulsive phase of the brightening, suggesting the increase of the magnetic non-potentiality at the loop footpoint and the sudden release of magnetic energy via magnetic reconnection. Our results support the nanoflare theory that coronal heating events are caused by magnetic reconnection events at fine-scale magnetic discontinuities. Title: Simultaneous observation of a hot explosion by NST and IRIS Authors: Kim, Yeon-Han; Yurchyshyn, Vasyl; Bong, Su-Chan; Cho, Il-Hyun; Cho, Kyung-Suk; Lee, Jaejin; Lim, Eun-Kyung; Park, Young-Deuk; Yang, Heesu; Ahn, Kwangsu; Goode, Philip R.; Jang, Bi-Ho Bibcode: 2015ApJ...810...38K Altcode: We present the first simultaneous observations of so-called “hot explosions” in the cool atmosphere of the Sun made by the New Solar Telescope (NST) of Big Bear Solar Observatory and the Interface Region Imaging Spectrograph (IRIS) in space. The data were obtained during the joint IRIS-NST observations on 2014 July 30. The explosion of interest started around 19:20 UT and lasted for about 10 minutes. Our findings are as follows: (1) the IRIS brightening was observed in three channels of slit-jaw images, which cover the temperature range from 4000 to 80,000 K; (2) during the brightening, the Si iv emission profile showed a double-peaked shape with highly blue and redshifted components (-40 and 80 km s-1) (3) wing brightening occurred in Hα and Ca ii 8542 Å bands and related surges were observed in both bands of the NST Fast Imaging Solar Spectrograph (FISS) instrument; (4) the elongated granule, seen in NST TiO data, is clear evidence of the emergence of positive flux to trigger the hot explosion; (5) the brightening in Solar Dynamics Observatory/Atmospheric Imaging Assembly 1600 Å images is quite consistent with the IRIS brightening. These observations suggest that our event is a hot explosion that occurred in the cool atmosphere of the Sun. In addition, our event appeared as an Ellerman bomb (EB) in the wing of Hα, although its intensity is weak and the vertical extent of the brightening seems to be relatively high compared with the typical EBs. Title: Characteristics of four SPE groups with different origins and acceleration processes Authors: Kim, R. -S.; Cho, K. -S.; Lee, J.; Bong, S. -C.; Joshi, A. D.; Park, Y. -D. Bibcode: 2015JGRA..120.7083K Altcode: Solar proton events (SPEs) can be categorized into four groups based on their associations with flare or CME inferred from onset timings as well as acceleration patterns using multienergy observations. In this study, we have investigated whether there are any typical characteristics of associated events and acceleration sites in each group using 42 SPEs from 1997 to 2012. We find the following: (i) if the proton acceleration starts from a lower energy, a SPE has a higher chance to be a strong event (> 5000 particle flux per unit (pfu)) even if its associated flare and/or CME are not so strong. The only difference between the SPEs associated with flare and CME is the location of the acceleration site. (ii) For the former (Group A), the sites are very low (∼ 1 Rs) and close to the western limb, while the latter (Group C) have relatively higher (mean = 6.05 Rs) and wider acceleration sites. (iii) When the proton acceleration starts from the higher energy (Group B), a SPE tends to be a relatively weak event (< 1000 pfu), although its associated CME is relatively stronger than previous groups. (iv) The SPEs categorized by the simultaneous acceleration in whole energy range within 10 min (Group D) tend to show the weakest proton flux (mean = 327 pfu) in spite of strong associated eruptions. Based on those results, we suggest that the different characteristics of SPEs are mainly due to the different conditions of magnetic connectivity and particle density, which are changed with longitude and height as well as their origin. Title: Solar Dynamics Observatory Data Search using Metadata in the KDC Authors: Hwang, E.; Choi, S.; Baek, J. -H.; Park, J.; Lee, J.; Cho, K. Bibcode: 2015ASPC..495..539H Altcode: 2015adass..24..539H We have constructed the Korean Data Center (KDC) for the Solar Dynamics Observatory (SDO) in the Korea Astronomy and Space Science Institute (KASI). The SDO comprises three instruments; the Atmospheric Imaging Assembly (AIA), the Helioseismic and Magnetic Imager (HMI), and the Extreme Ultraviolet Variability Experiment (EVE). We archive AIA and HMI FITS data. The size of data is about 1 TB of a day. The goal of KDC for SDO is to provide easy and fast access service to the data for researchers in Asia. In order to improve the data search rate, we designed the system to search data without going through a process of database query. The fields of instrument, wavelength, data path, date, and time are saved as a text file. This metadata file and SDO FITS data can be simply accessed via HTTP and are open to the public. We present a process of creating metadata and a way to access SDO FITS data in detail. Title: Statistical Comparison Between Pores and Sunspots by Using SDO/HMI Authors: Cho, I. -H.; Cho, K. -S.; Bong, S. -C.; Lim, E. -K.; Kim, R. -S.; Choi, S.; Kim, Y. -H.; Yurchyshyn, V. Bibcode: 2015ApJ...811...49C Altcode: We carried out an extensive statistical study of the properties of pores and sunspots, and investigated the relationship among their physical parameters such as size, intensity, magnetic field, and the line-of-sight (LOS) velocity in the umbrae. For this, we classified 9881 samples into three groups of pores, transitional sunspots, and mature sunspots. As a result, (1) we find that the total magnetic flux inside the umbra of pores, transitional sunspots, and mature sunspots increases proportionally to the powers of the area and the power indices in the three groups significantly differ from each other. (2) The umbral area distribution of each group shows a Gaussian distribution and they are clearly separated, displaying three distinct peak values. All of the quantities significantly overlap among the three groups. (3) The umbral intensity shows a rapid decrease with increasing area, and their magnetic field strength shows a rapid increase with decreasing intensity. (4) The LOS velocity in pores is predominantly redshifted and its magnitude decreases with increasing magnetic field strength. The decreasing trend becomes nearly constant with marginal blueshift in the case of mature sunspots. The dispersion of LOS velocities in mature sunspots is significantly suppressed compared to pores. From our results, we conclude that the three groups have different characteristics in their area, intensity, magnetic field, and LOS velocity as well in their relationships. Title: A Prestudy for the Development of a Compact Coronagraph Authors: Bong, Su-Chan; Yang, Heesu; Cho, Kyuhyoun; Cho, Kyung-Suk; Lim, Eun-Kyung; Park, Young-Deuk; Chae, Jongchul Bibcode: 2015IAUGA..2254511B Altcode: We are conducting a prestudy for the development of a compact coronagraph. The coronagraph is comprised of the external occulter, lens, filter, and the CCD. We focus on the performance of the external occulter, and the measurement of the coronal temperature and velocity using a set of filters. We have tested the diffraction of a singlet occulter and a cone occulter using laser. Compared to the singlet occulter, the cone occulter gave rather symmetric, smooth and weak diffraction pattern. We also have calculated the Thomson scattering of the K corona to form coronal spectra in various temperature and velocity conditions. We found the optimized wavelength set (393.4, 399.0, 402.5, and 482.7 nm) for temperature and velocity measurement. We plan to build a prototype coronagraph and make a test observation during the total eclipse in 2016 without the occulter. Title: Formation and Eruption of a Small Flux Rope in the Chromosphere Observed by NST, IRIS, and SDO Authors: Kumar, Pankaj; Yurchyshyn, Vasyl; Wang, Haimin; Cho, Kyung-Suk Bibcode: 2015ApJ...809...83K Altcode: 2015arXiv150701761K Using high-resolution images from the 1.6 m New Solar Telescope at Big Bear Solar Observatory, we report the direct evidence of chromospheric reconnection at the polarity inversion line between two small opposite polarity sunspots. Small jetlike structures (with velocities of ∼20-55 km s-1) were observed at the reconnection site before the onset of the first M1.0 flare. The slow rise of untwisting jets was followed by the onset of cool plasma inflow (∼10 km s-1) at the reconnection site, causing the onset of a two-ribbon flare. The reconnection between two sheared J-shaped cool Hα loops causes the formation of a small twisted (S-shaped) flux rope in the chromosphere. In addition, Helioseismic and Magnetic Imager magnetograms show the flux cancellation (both positive and negative) during the first M1.0 flare. The emergence of negative flux and the cancellation of positive flux (with shear flows) continue until the successful eruption of the flux rope. The newly formed chromospheric flux rope becomes unstable and rises slowly with a speed of ∼108 km s-1 during a second C8.5 flare that occurred after ∼3 hr of the first M1.0 flare. The flux rope was destroyed by repeated magnetic reconnection induced by its interaction with the ambient field (fan-spine topology) and looks like an untwisting surge (∼170 km s-1) in the coronal images recorded by the Solar Dynamics Observatory/Atmospheric Imaging Assembly. These observations suggest the formation of a chromospheric flux rope (by magnetic reconnection associated with flux cancellation) during the first M1.0 flare and its subsequent eruption/disruption during the second C8.5 flare. Title: Causes of the Sep. 12-13, 2014 geomagnetic storms Authors: Cho, Kyung-Suk; Kim, Rooksoon; Park, Sung-Hong; Kim, Sujin Bibcode: 2015IAUGA..2249582C Altcode: Solar cycle 24 is very modest compared to previous solar cycles. The solar maximum phase may have been reached in the middle of 2014 and the sunspot number has decreased since the beginning of 2015. During this period, it has been reported that only few events produced strong X-class flares, solar proton events, and geomagnetic storms. In this study we have investigated causes of the multiple geomagnetic storms occurred on September 12-13, 2014. The geomagnetic storm forecast model based on the CME observations was used for identification of the causes of the geomagnetic storms. Details of the solar source region were investigated to give an answer why the geomagnetic storms were not so strong even though they were related to fast coronal mass ejections with large earth-ward direction. As a result, we found that the first weak storm was driven by the CME related to M4.6 flare and the second minor storm was driven by one of the fast CMEs related to strong X1.6 flare. Our result shows that the reason why the second storm was not strong is that it was caused by the CME with northward magnetic field. Therefore we suggest that one of the essential ingredients for geomagnetic storm forecasting is to find out the magnetic field direction of earth-ward CMEs, which can be accomplished by investigating magnetic fields of their solar source regions a few days before their arrival to the earth. Title: A comprehensive catalog of 3D parameters of front-side halo CMEs using STEREO and SOHO from 2009 to 2013 Authors: Jang, Soojeong; Moon, Yong-Jae; Kim, Rok-Soon; Lee, Harim; Cho, Kyung-Suk Bibcode: 2015shin.confE..85J Altcode: We present a comprehensive catalog of 308 front-side halo (partial and full) CMEs from 2009 to 2013 observed by both SOHO and STEREO. This catalog includes 2D CME parameters from single spacecraft (SOHO) as well as 3D ones from multi-spacecraft. To determine the 3D CME parameters (speed, angular width, and source location), we use the STEREO CME analysis tool based on a triangulation method. In this paper, we compare between 2D and 3D CME parameters, which is the first statistical comparison between them. As a result, we find that 2D speeds tend to be about 20% underestimated when compared to 3D ones. The 3D angular width ranges from 30° to 158°, which are much smaller than the 2D angular widths with the mean value of 225°. We also find that a ratio between 3D and 2D angular width increase with central meridian distance. The 3D propagation directions are similar to the flare locations. The angular width-speed relationship in 3D is much stronger than that in 2D. Title: Detection of Shock Merging in the Chromosphere of a Solar Pore Authors: Chae, Jongchul; Song, Donguk; Seo, Minju; Cho, Kyung-Suk; Park, Young-Deuk; Yurchyshyn, Vasyl Bibcode: 2015ApJ...805L..21C Altcode: It was theoretically demonstrated that a shock propagating in the solar atmosphere can overtake another and merge with it. We provide clear observational evidence that shock merging does occur quite often in the chromosphere of sunspots. Using Hα imaging spectral data taken by the Fast Imaging Solar Spectrograph of the 1.6 m New Solar Telescope at the Big Bear Soar Observatory, we construct time-distance maps of line-of-sight velocities along two appropriately chosen cuts in a pore. The maps show a number of alternating redshift and blueshift ridges, and we identify each interface between a preceding redshift ridge and the following blueshift ridge as a shock ridge. The important finding of ours is that two successive shock ridges often merge with each other. This finding can be theoretically explained by the merging of magneto-acoustic shock waves propagating with lower speeds of about 10 km s-1 and those propagating at higher speeds of about 16-22 km s-1. The shock merging is an important nonlinear dynamical process of the solar chromosphere that can bridge the gap between higher-frequency chromospheric oscillations and lower-frequency dynamic phenomena such as fibrils. Title: X-Ray and EUV Observations of Simultaneous Short and Long Period Oscillations in Hot Coronal Arcade Loops Authors: Kumar, Pankaj; Nakariakov, Valery M.; Cho, Kyung-Suk Bibcode: 2015ApJ...804....4K Altcode: 2015arXiv150207117K We report decaying quasi-periodic intensity oscillations in the X-ray (6-12 keV) and extreme-ultraviolet (EUV) channels (131, 94, 1600, 304 Å) observed by the Fermi Gamma-ray Burst Monitor and Solar Dynamics Observatory/Atmospheric Imaging Assembly (AIA), respectively, during a C-class flare. The estimated periods of oscillation and decay time in the X-ray channel (6-12 keV) were about 202 and 154 s, respectively. A similar oscillation period was detected at the footpoint of the arcade loops in the AIA 1600 and 304 Å channels. Simultaneously, AIA hot channels (94 and 131 Å) reveal propagating EUV disturbances bouncing back and forth between the footpoints of the arcade loops. The period of the oscillation and decay time were about 409 and 1121 s, respectively. The characteristic phase speed of the wave is about 560 km s-1 for about 115 Mm of loop length, which is roughly consistent with the sound speed at the temperature about 10-16 MK (480-608 km s-1). These EUV oscillations are consistent with the Solar and Heliospheric Observatory/Solar Ultraviolet Measurement of Emitted Radiation Doppler-shift oscillations interpreted as the global standing slow magnetoacoustic wave excited by a flare. The flare occurred at one of the footpoints of the arcade loops, where the magnetic topology was a 3D fan-spine with a null-point. Repetitive reconnection at this footpoint could have caused the periodic acceleration of non-thermal electrons that propagated to the opposite footpoint along the arcade and that are precipitating there, causing the observed 202 s periodicity. Other possible interpretations, e.g., the second harmonics of the slow mode, are also discussed. Title: Search for the Dark Photon and the Dark Higgs Boson at Belle Authors: Jaegle, I.; Adachi, I.; Aihara, H.; Al Said, S.; Asner, D. M.; Aushev, T.; Ayad, R.; Bakich, A. M.; Bansal, V.; Barrett, M.; Bhuyan, B.; Bozek, A.; Bračko, M.; Browder, T. E.; Červenkov, D.; Chang, M. -C.; Cheon, B. G.; Chilikin, K.; Cho, K.; Chobanova, V.; Choi, S. -K.; Choi, Y.; Cinabro, D.; Dalseno, J.; Doležal, Z.; Drásal, Z.; Drutskoy, A.; Dutta, D.; Eidelman, S.; Epifanov, D.; Farhat, H.; Fast, J. E.; Ferber, T.; Frost, O.; Gaur, V.; Gabyshev, N.; Ganguly, S.; Garmash, A.; Getzkow, D.; Gillard, R.; Goh, Y. M.; Golob, B.; Grzymkowska, O.; Hayasaka, K.; Hayashii, H.; He, X. H.; Hedges, M.; Hou, W. -S.; Iijima, T.; Inami, K.; Ishikawa, A.; Iwasaki, Y.; Julius, T.; Kang, K. H.; Kato, E.; Kawasaki, T.; Kim, D. Y.; Kim, J. B.; Kim, J. H.; Kim, S. H.; Kinoshita, K.; Ko, B. R.; Kodyš, P.; Korpar, S.; Križan, P.; Krokovny, P.; Kuzmin, A.; Kwon, Y. -J.; Lange, J. S.; Lee, I. S.; Lewis, P.; Li Gioi, L.; Libby, J.; Liventsev, D.; Matvienko, D.; Miyata, H.; Mizuk, R.; Mohanty, G. B.; Moll, A.; Mussa, R.; Nakano, E.; Nakao, M.; Nisar, N. K.; Nishida, S.; Ogawa, S.; Pakhlov, P.; Pakhlova, G.; Park, H.; Pedlar, T. K.; Pesántez, L.; Petrič, M.; Piilonen, L. E.; Ritter, M.; Rostomyan, A.; Sakai, Y.; Sandilya, S.; Santelj, L.; Sanuki, T.; Sato, Y.; Savinov, V.; Schneider, O.; Schnell, G.; Schwanda, C.; Semmler, D.; Senyo, K.; Seon, O.; Seong, I.; Sevior, M. E.; Shebalin, V.; Shibata, T. -A.; Shiu, J. -G.; Shwartz, B.; Simon, F.; Sinha, R.; Sohn, Y. -S.; Starič, M.; Sumihama, M.; Sumisawa, K.; Tamponi, U.; Tatishvili, G.; Teramoto, Y.; Thorne, F.; Uchida, M.; Uehara, S.; Unno, Y.; Uno, S.; Vahsen, S. E.; Van Hulse, C.; Vanhoefer, P.; Varner, G.; Vinokurova, A.; Wagner, M. N.; Wang, C. H.; Wang, M. -Z.; Wang, P.; Wang, X. L.; Watanabe, M.; Watanabe, Y.; Williams, K. M.; Won, E.; Yamaoka, J.; Yashchenko, S.; Yook, Y.; Yusa, Y.; Zhilich, V.; Zhulanov, V.; Zupanc, A.; Belle Collaboration Bibcode: 2015PhRvL.114u1801J Altcode: 2015arXiv150200084T The dark photon A' and the dark Higgs boson h' are hypothetical constituents featured in a number of recently proposed dark sector models. Assuming prompt decays of both dark particles, we search for their production in the so-called Higgstrahlung channel e+e-→A'h' , with h'→A'A'. We investigate ten exclusive final states with A'→e+e-, μ+μ-, or π+π- in the mass ranges 0.1 GeV /c2 <mA'<3.5 GeV /c2 and 0.2 GeV /c2 <mh'<10.5 GeV /c2 . We also investigate three inclusive final states 2 (e+e-)X , 2 (μ+μ-)X , and (e+e-)(μ+μ-)X , where X denotes a dark photon candidate detected via missing mass, in the mass ranges 1.1 GeV /c2 <mA'<3.5 GeV /c2 and 2.2 GeV /c2 <mh'<10.5 GeV /c2 . Using the entire 977 fb-1 data set collected by Belle, we observe no significant signal. We obtain individual and combined 90% credibility level upper limits on the branching fraction times the Born cross section, B ×σBorn , on the Born cross section σBorn, and on the dark photon coupling to the dark Higgs boson times the kinetic mixing between the standard model photon and the dark photon, αD×ɛ2 . These limits improve upon and cover wider mass ranges than previous experiments. The limits from the final states 3 (π+π-) and 2 (e+e-)X are the first placed by any experiment. For αD equal to 1 /137 , mh'< 8 GeV /c2 , and mA'<1 GeV /c2 , we exclude values of the mixing parameter ɛ above ∼8 ×10-4. Title: Geometrical Relationship Between Interplanetary Flux Ropes and Their Solar Sources Authors: Marubashi, K.; Akiyama, S.; Yashiro, S.; Gopalswamy, N.; Cho, K. -S.; Park, Y. -D. Bibcode: 2015SoPh..290.1371M Altcode: 2015SoPh..tmp...46M We investigated the physical connection between interplanetary flux ropes (IFRs) near Earth and coronal mass ejections (CMEs) by comparing the magnetic field structures of IFRs and CME source regions. The analysis is based on the list of 54 pairs of ICMEs (interplanetary coronal mass ejections) and CMEs that are taken to be the most probable solar source events. We first attempted to identify the flux rope structure in each of the 54 ICMEs by fitting models with a cylinder and torus magnetic field geometry, both with a force-free field structure. This analysis determined the possible geometries of the identified flux ropes. Then we compared the flux rope geometries with the magnetic field structure of the solar source regions. We obtained the following results: (1) Flux rope structures are seen in 51 ICMEs out of the 54. The result implies that all ICMEs have an intrinsic flux rope structure, if the three exceptional cases are attributed to unfavorable observation conditions. (2) It is possible to find flux rope geometries with the main axis orientation close to the orientation of the magnetic polarity inversion line (PIL) in the solar source regions, the differences being less than 25°. (3) The helicity sign of an IFR is strongly controlled by the location of the solar source: flux ropes with positive (negative) helicity are associated with sources in the southern (northern) hemisphere (six exceptions were found). (4) Over two-thirds of the sources in the northern hemisphere are concentrated along PILs with orientations of 45° ± 30° (measured clockwise from the east), and over two-thirds in the southern hemisphere along PILs with orientations of 135° ± 30°, both corresponding to the Hale boundaries. These results strongly support the idea that a flux rope with the main axis parallel to the PIL erupts in a CME and that the erupted flux rope propagates through the interplanetary space with its orientation maintained and is observed as an IFR. Title: Intensity and Doppler Velocity Oscillations in Pore Atmospheres Authors: Cho, K. -S.; Bong, S. -C.; Nakariakov, V. M.; Lim, E. -K.; Park, Y. -D.; Chae, J. C.; Yang, H. -S.; Park, H. -M.; Yurchyshyn, V. Bibcode: 2015ApJ...802...45C Altcode: We have investigated chromospheric traveling features running across two merged pores from their centers at speeds of about 55 km s-1, in the active region AR 11828. The pores were observed on 2013 August 24 by using high-time, spatial, and spectral resolution data from the Fast Imaging Solar Spectrograph of the 1.6 m New Solar Telescope. We infer a line-of-sight (LOS) velocity by applying the lambdameter method to the Ca ii 8542 Å band and Hα band, and investigate intensity and LOS velocity changes at different wavelengths and different positions at the pores. We find that they have three-minute oscillations, and the intensity oscillation from the line center (0.0 \overset{\circ}A ) is preceded by that from the core (-0.3 \overset{\circ}A ) of the bands. There is no phase difference between the intensity and the LOS velocity oscillations at a given wavelength. The amplitude of LOS velocity from the near core spectra ({Δ }λ =0.10-0.21 \overset{\circ}A ) is greater than that from the far core spectra ({Δ }λ =0.24-0.36 \overset{\circ}A ). These results support the interpretation of the observed wave as a slow magnetoacoustic wave propagating along the magnetic field lines in the pores. The apparent horizontal motion and a sudden decrease of its speed beyond the pores can be explained by the projection effect caused by inclination of the magnetic field with a canopy structure. We conclude that the observed wave properties of the pores are quite similar to those from the sunspot observations. Title: Burst Locating Capability of the Korean Solar Radio Burst Locator (KSRBL) Authors: Hwangbo, Jung-Eun; Bong, Su-Chan; Park, Sung-Hong; Lee, Dae-Young; Cho, Kyung-Suk; Lee, Jaejin; Park, Young-Deuk Bibcode: 2015JASS...32...91H Altcode: The Korean Solar Radio Burst Locator (KSRBL) is a solar radio spectrograph observing the broad frequency range from 0.245 to 18 GHz with the capability of locating wideband gyrosynchrotron bursts. Due to the characteristics of a spiral feed, the beam center varies in a spiral pattern with frequency, making a modulation pattern over the wideband spectrum. After a calibration process, we obtained dynamic spectra consistent with the Nobeyama Radio Polarimeter (NoRP). We compared and analyzed the locations of bursts observed by KSRBL with results from the Nobeyama Radioheliograph (NoRH) and Atmospheric Imaging Assembly (AIA). As a result, we found that the KSRBL provides the ability to locate flaring sources on the Sun within around 2'. Title: A Trio of Confined Flares in AR 11087 Authors: Joshi, Anand D.; Forbes, Terry G.; Park, Sung-Hong; Cho, Kyung-Suk Bibcode: 2015ApJ...798...97J Altcode: We investigate three flares that occurred in active region, AR 11087, observed by the Dutch Open Telescope (DOT) on 2010 July 13, in a span of three hours. The first two flares have soft X-ray class B3, whereas the third flare has class C3. The third flare not only was the largest in terms of area and brightness but also showed a very faint coronal mass ejection (CME) associated with it, while the earlier two flares had no associated CME. The active region, located at 27° N, 26° E, has a small U-shaped active region filament to the south of the sunspot, and a quiescent filament is located to its west. Hα observations from DOT, as well as extreme-ultraviolet images and magnetograms from the STEREO spacecraft and Solar Dynamics Observatory, are used to study the dynamics of the active region during the three flares. Our observations imply that the first two flares are confined and that some filament material drains to the surface during these flares. At the onset of the third flare downflows are again observed within the active region, but a strong upflow is also observed at the northern end of the adjacent quiescent filament to the west. It is at the latter location that the CME originates. The temporal evolution of the flare ribbons and the dynamics of the filaments are both consistent with the idea that reconnection in a pre-existing current sheet leads to a loss of equilibrium. Title: Statistical Study on Personal Reduction Coefficients of Sunspot Numbers Since 1981 Authors: Cho, Il-Hyun; Bong, Su-Chan; Cho, Kyung-Suk; Lee, Jaejin; Kim, Rok-Soon; Park, Young-Deuk; Kim, Yeon-Han Bibcode: 2014JKAS...47..255C Altcode: No abstract at ADS Title: A refined classification of SPEs based on the multienergy channel observations Authors: Kim, R. -S.; Cho, K. -S.; Lee, J.; Bong, S. -C.; Park, Y. -D. Bibcode: 2014JGRA..119.9419K Altcode: We have investigated characteristics of solar proton events (SPEs) and their association with other types of solar eruption using 42 SPEs observed with SOlar and Heliospheric Observatory/Energetic and Relativistic Nuclei and Electron detector from 1997 to 2012. A velocity dispersion analysis was performed to correctly estimate the onset times of proton flux increase at the solar vicinity. These SPE onset times were compared with those of associated flares, coronal mass ejections (CMEs), and interplanetary type II radio bursts. We found that (i) the proton flux of 13 SPEs (31%) increase during the flare X-ray intensity is increasing, and the rest 29 SPEs (69%) show onsets well coincident with the first appearance of CMEs in Large Angle and Spectrometric COronagraph field of view. (ii) All flare-associated SPEs show the flux enhancements starting from the lower energy, while the CME-associated SPEs show the flux enhancements starting from either the higher or the lower energies. In the other events, the flux enhancement occurs simultaneously at all energies within 10 min. (iii) For the former, large flux enhancements occur in a short time, while the latter tend to show relatively weak and slow flux enhancements. Our classification uses two criteria, SPE onset timing relative to flares and energy-dependent flux enhancement, unlike the conventional classification of SPEs based on whether the flux time profile is impulsive or gradual. Nevertheless our classification scheme refines the distinction between the flare-associated SPEs and the CME-associated SPEs in terms of the onset timing. Additional information on the proton acceleration as implied by the energy-dependent patterns of flux enhancement is briefly discussed. Title: Vertical Kink Oscillation of a Magnetic Flux Rope Structure in the Solar Corona Authors: Kim, S.; Nakariakov, V. M.; Cho, K. -S. Bibcode: 2014ApJ...797L..22K Altcode: Vertical transverse oscillations of a coronal magnetic rope, observed simultaneously in the 171 Å and 304 Å bandpasses of the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory (SDO), are detected. The oscillation period is about 700 s and the displacement amplitude is about 1 Mm. The oscillation amplitude remains constant during the observation. Simultaneous observation of the rope in the bandpasses corresponding to the coronal and chromospheric temperatures suggests that it has a multi-thermal structure. Oscillatory patterns in 171 Å and 304 Å are coherent, which indicates that the observed kink oscillation is collective, in which the rope moves as a single entity. We interpret the oscillation as a fundamental standing vertically polarized kink mode of the rope, while the interpretation in terms of a perpendicular fast wave could not be entirely ruled out. In addition, the arcade situated above the rope and seen in the 171 Å bandpass shows an oscillatory motion with the period of about 1000 s. Title: KREAM: Korean Radiation Exposure Assessment Model for Aviation Route Dose Authors: Hwang, J.; Dokgo, K.; Choi, E. J.; Kim, K. C.; Kim, H. P.; Cho, K. S. F. Bibcode: 2014AGUFMSM31A4176H Altcode: Since Korean Air has begun to use the polar route from Seoul/ICN airport to New York/JFK airport on August 2006, there are explosive needs for the estimation and prediction against cosmic radiation exposure for Korean aircrew and passengers in South Korea from public. To keep pace with those needs of public, Korean government made the law on safety standards and managements of cosmic radiation for the flight attendants and the pilots in 2013. And we have begun to develop our own Korean Radiation Exposure Assessment Model (KREAM) for aviation route dose since last year funded by Korea Meteorological Administration (KMA). GEANT4 model and NRLMSIS 00 model are used for calculation of the energetic particles' transport in the atmosphere and for obtaining the background atmospheric neutral densities depending on altitude. For prediction the radiation exposure in many routes depending on the various space weather effects, we constructed a database from pre-arranged simulations using all possible combinations of R, S, and G, which are the space weather effect scales provided by the National Oceanic and Atmospheric Administration (NOAA). To get the solar energetic particles' spectrum at the 100 km altitude which we set as a top of the atmospheric layers in the KREAM, we use ACE and GOES satellites' proton flux observations. We compare the results between KREAM and the other cosmic radiation estimation programs such as CARI-6M which is provided by the Federal Aviation Agency (FAA). We also validate KREAM's results by comparison with the measurement from Liulin-6K LET spectrometer onboard Korean commercial flights and Korean Air Force reconnaissance flights. Title: Multiwavelength observation of a large-scale flux rope eruption above a kinked small filament Authors: Kumar, Pankaj; Cho, Kyung-Suk Bibcode: 2014A&A...572A..83K Altcode: 2014arXiv1409.7213K We analyzed multiwavelength observations of a western limb flare (C3.9) that occurred in AR NOAA 111465 on 30 April 2012. The high-resolution images recorded by SDO/AIA 304, 1600 Å and Hinode/SOT Hα show the activation of a small filament (rising speed ~40 km s-1) associated with a kink instability and the onset of a C-class flare near the southern leg of the filament. The first magnetic reconnection occurred at one of the footpoints of the filament and caused the breaking of its southern leg. The filament shows unwinding motion of the northern leg and apex in counterclockwise direction and failed to erupt. A flux-rope structure (visible only in hot channels, i.e., AIA 131 and 94 Å and Hinode/SXT) appeared along the neutral line during the second magnetic reconnection that occurred above the kinked filament. The formation of the RHESSI hard X-ray source (12-25 keV) above the kinked filament and the simultaneous appearance of the hot 131 Å loops associated with photospheric brightenings (AIA 1700 Å) indicates the particle acceleration along these loops from the top of the filament. In addition, extreme ultraviolet disturbances or waves observed above the filament in 171 Å also show a close association with magnetic reconnection. The flux rope rises slowly (~100 km s-1), which produces a very large twisted structure possibly through reconnection with the surrounding sheared magnetic fields within ~15-20 min, and showed an impulsive acceleration reaching a height of about 80-100 Mm. AIA 171 and SWAP 174 Å images reveal a cool compression front (or coronal mass ejection frontal loop) surrounding the hot flux rope structure. Movies associated with Figs. 2 and 7 are available in electronic form at http://www.aanda.org Title: Magnetic Structure and Nonthermal Electrons in the X6.9 Flare on 2011 August 09 Authors: Hwangbo, J. E.; Lee, J.; Park, S. H.; Bong, S. C.; Lee, D. Y.; Kim, Y. H.; Cho, K. S. F.; Park, Y. D. Bibcode: 2014AGUFMSH23A4155H Altcode: The 2011 August 09 Flare is one of the largest X-ray flares of Sunspot Cycle 24, but the spatial information is rather limited due to its position close to the western limb. This paper presents the information on the location of high energy electrons derived from the hard X-ray and microwave spectra obtained with the Reuven Ramaty High-Energy Solar Spectroscopic Imager(RHESSI) and the Korean Solar Radio Burst Locator (KSRBL), respectively. The KSRBL microwave spectrum shows significant fluxes at low frequencies, implying that the high energy electrons reside in a coronal volume highly concentrated at strong magnetic fields, and rapidly expanding with decreasing magnetic fields. After a simple modeling of the microwave spectrum, we found that the microwave source should be located above the inner pair of magnetic poles in a large quadrupolar configuration. The time-dependent evolution of magnetic field distribution and total nonthermal energy derived from the microwave spectra is also consistent with the standard picture of multiple magnetic reconnections recurring at a magnetic null point that forms above the magnetic quadrupoles and moves up with time. Title: Kinematics of Solar Chromospheric Surges of AR 10930 Authors: Bong, Su-Chan; Cho, Kyung-Suk; Yurchyshyn, Vasyl Bibcode: 2014JKAS...47..311B Altcode: No abstract at ADS Title: Multi-wavelength Observation of Initiation Phase of Filament Eruption Authors: Kim, S.; Cho, K. S. F.; Park, S. H. Bibcode: 2014AGUFMSH13B4102K Altcode: We have examined a nonthermal emission of a preflare activity associated with M-class flare. This activity resulted in a filament eruption that was developed into a halo CME. It was observed by microwave from Nobeyama Radioheliograph (NoRH) at 17 GHz and 34 GHz, Hard X-ray from Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) at 6-80 keV, and EUV from Atmospheric Imaging Assembly (AIA) onboard Solar Dynamics Observatory (SDO). We found that a microwave nonthermal source appeared near a southern footpoint of the filament system during the preflare phase. Then it moved systematically away from there in the direction parallel to two-ribbons together with the rapid eruption of the filament system. It implies that the particle acceleration of the flare started near the southern footpoint of the filament system and, thus, it provided a decisive factor for the eruption of it. During the preflare phase, Hard X-ray source also appeared in the position close to microwave source and their source positions lined up depending on their energy-bands. Unfortunately, there is no RHESSI data during the main flare because it passed night-part of the earth. Here, we present the detail investigation of physical parameters and emission mechanism of the preflare nonthermal emission based on the imaging spectroscopy of microwave and Hard X-ray. Title: Magnetic Structure and Nonthermal Electrons in the X6.9 Flare on 2011 August 9 Authors: Hwangbo, Jung-Eun; Lee, Jeongwoo; Park, Sung-Hong; Kim, Sujin; Lee, Dae-Young; Bong, Su-Chan; Kim, Yeon-Han; Cho, Kyung-Suk; Park, Young-Deuk Bibcode: 2014ApJ...796...80H Altcode: The 2011 August 9 flare is one of the largest X-ray flares of sunspot cycle 24, but spatial information is rather limited due to its position close to the western limb. This paper presents information about the location of high-energy electrons derived from hard X-ray and microwave spectra obtained with the Reuven Ramaty High-Energy Solar Spectroscopic Imager (RHESSI) and the Korean Solar Radio Burst Locator (KSRBL), respectively. The KSRBL microwave spectrum shows significant fluxes at low frequencies, implying that the high-energy electrons reside in a coronal volume highly concentrated at strong magnetic fields, and rapidly expanding with decreasing magnetic fields. After a simple modeling of the microwave spectrum, we found that the microwave source should be located above the inner pair of magnetic poles in a large quadrupolar configuration. The time-dependent evolution of the magnetic field distribution and total nonthermal energy derived from the microwave spectra is also consistent with the standard picture of multiple magnetic reconnections recurring at a magnetic null point that forms above the magnetic quadrupoles and moves up with time. Title: Active Region Coronal Rain Event Observed by the Fast Imaging Solar Spectrograph on the NST Authors: Ahn, Kwangsu; Chae, Jongchul; Cho, Kyung-Suk; Song, Donguk; Yang, Heesu; Goode, Philip R.; Cao, Wenda; Park, Hyungmin; Nah, Jakyung; Jang, Bi-Ho; Park, Young-Deuk Bibcode: 2014SoPh..289.4117A Altcode: 2014SoPh..tmp...98A The Fast Imaging Solar Spectrograph (FISS) is being operated on the New Solar Telescope of the Big Bear Solar Observatory. It simultaneously records spectra of Hα and Ca II 8542 Å lines, and this dual-spectra measurement provides an estimate of the temperature and nonthermal speed components. We observed a loop structure in AR 11305 using the FISS, SDO/AIA, and STEREO/EUVI in 304 Å, and found plasma material falling along the loop from a coronal height into the umbra of a sunspot, which accelerated up to 80 km s−1. We also observed C2 and C7 flare events near the loop. The temperature of the downflows was in the range of 10 000 - 33 000 K, increasing toward the umbra. The temperature of the flow varied with time, and the temperature near the footpoint rose immediately after the C7 flare, but the temperature toward the umbra remained the same. There seemed to be a temporal correlation between the amount of downflow material and the observed C-class flares. The downflows decreased gradually soon after the flares and then increased after a few hours. These high-speed red-shift events occurred continuously during the observations. The flows observed on-disk in Hα and Ca II 8542 Å appeared as fragmented, fuzzy condensed material falling from the coronal heights when seen off-limb with STEREO/EUVI at 304 Å. Based on these observations, we propose that these flows were an on-disk signature of coronal rain. Title: Impulsive Energy Release and Non-thermal Emission in a Confined M4.0 Flare Triggered by Rapidly Evolving Magnetic Structures Authors: Kushwaha, Upendra; Joshi, Bhuwan; Cho, Kyung-Suk; Veronig, Astrid; Tiwari, Sanjiv Kumar; Mathew, S. K. Bibcode: 2014ApJ...791...23K Altcode: 2014arXiv1407.8115K We present observations of a confined M4.0 flare from NOAA 11302 on 2011 September 26. Observations at high temporal, spatial, and spectral resolution from the Solar Dynamics Observatory, Reuven Ramaty High Energy Solar Spectroscopic Imager, and Nobeyama Radioheliograph observations enabled us to explore the possible triggering and energy release processes of this flare despite its very impulsive behavior and compact morphology. The flare light curves exhibit an abrupt rise of non-thermal emission with co-temporal hard X-ray (HXR) and microwave (MW) bursts that peaked instantly without any precursor emission. This stage was associated with HXR emission up to 200 keV that followed a power law with photon spectral index (γ) ~ 3. Another non-thermal peak, observed 32 s later, was more pronounced in the MW flux than the HXR profiles. Dual peaked structures in the MW and HXR light curves suggest a two-step magnetic reconnection process. Extreme ultraviolet (EUV) images exhibit a sequential evolution of the inner and outer core regions of magnetic loop systems while the overlying loop configuration remained unaltered. Combined observations in HXR, (E)UV, and Hα provide support for flare models involving the interaction of coronal loops. The magnetograms obtained by the Helioseismic and Magnetic Imager reveal emergence of magnetic flux that began ~five hr before the flare. However, the more crucial changes in the photospheric magnetic flux occurred about one minute prior to the flare onset with opposite polarity magnetic transients appearing at the early flare location within the inner core region. The spectral, temporal, and spatial properties of magnetic transients suggest that the sudden changes in the small-scale magnetic field have likely triggered the flare by destabilizing the highly sheared pre-flare magnetic configuration. Title: Superpenumbral Fibrils Powered by Sunspot Oscillations Authors: Chae, Jongchul; Yang, Heesu; Park, Hyungmin; Ajor Maurya, Ram; Cho, Kyung-Suk; Yurchysyn, Vasyl Bibcode: 2014ApJ...789..108C Altcode: It is still a mystery how the solar chromosphere can stand high above the photosphere. The dominant portion of this layer must be dynamically supported, as is evident by the common occurrence of jets such as spicules and mottles in quiet regions, and fibrils and surges in active regions. Hence, revealing the driving mechanism of these chromospheric jets is crucial for our understanding of how the chromosphere itself exists. Here, we report our observational finding that fibrils in the superpenumbra of a sunspot are powered by sunspot oscillations. We find patterns of outward propagation that apparently originate from inside the sunspot, propagate like running penumbral waves, and develop into the fibrils. Redshift ridges seen in the time-distance plots of velocity often merge, forming a fork-like pattern. The predominant period of these shock waves increases, often jumping with distance, from 3 minutes to 10 minutes. This short-to-long period transition seems to result from the selective suppression of shocks by the falling material of their preceding shocks. Based on our results, we propose that the fibrils are driven by slow shock waves with long periods that are produced by the merging of shock waves with shorter periods propagating along the magnetic canopy. Title: Introduction to the Space Weather Monitoring System at KASI Authors: Baek, J.; Choi, S.; Kim, Y.; Cho, K.; Bong, S.; Lee, J.; Kwak, Y.; Hwang, J.; Park, Y.; Hwang, E. Bibcode: 2014ASPC..485..103B Altcode: 2014adass..23..103B We have developed the Space Weather Monitoring System (SWMS) at the Korea Astronomy and Space Science Institute (KASI). Since 2007, the system has continuously evolved into a better system. The SWMS consists of several subsystems: applications which acquire and process observational data, servers which run the applications, data storage, and display facilities which show the space weather information. The applications collect solar and space weather data from domestic and oversea sites. The collected data are converted to other format and/or visualized in real time as graphs and illustrations. We manage 3 data acquisition and processing servers, a file service server, a web server, and 3 sets of storage systems. We have developed 30 applications for a variety of data, and the volume of data is about 5.5 GB per day. We provide our customers with space weather contents displayed at the Space Weather Monitoring Lab (SWML) using web services. Title: Plasma Upflows and Microwave Emission in Hot Supra-arcade Structure Associated with an M1.6 Limb Flare Authors: Kim, S.; Shibasaki, K.; Bain, H. -M.; Cho, K. -S. Bibcode: 2014ApJ...785..106K Altcode: We have investigated a supra-arcade structure associated with an M1.6 flare, which occurred on the south-east limb on 2010 November 4. It is observed in EUV with the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory, microwaves at 17 and 34 GHz with the Nobeyama Radioheliograph (NoRH), and soft X-rays of 8-20 keV with RHESSI. Interestingly, we found exceptional properties of the supra-arcade thermal plasma from the AIA 131 Å and the NoRH: (1) plasma upflows along large coronal loops and (2) enhancing microwave emission. RHESSI detected two soft X-ray sources, a broad one in the middle of the supra-arcade structure and a bright one just above the flare-arcade. We estimated the number density and thermal energy for these two source regions during the decay phase of the flare. In the supra-arcade source, we found that there were increases of the thermal energy and the density at the early and last stages, respectively. On the contrary, the density and thermal energy of the source on the top of the flare-arcade decreases throughout. The observed upflows imply that there is continuous energy supply into the supra-arcade structure from below during the decay phase of the flare. It is hard to explain by the standard flare model in which the energy release site is located high in the corona. Thus, we suggest that a potential candidate of the energy source for the hot supra-arcade structure is the flare-arcade, which has exhibited a predominant emission throughout. Title: 우주환경 지상관측기 자료통합시스템 개발 Title: 우주환경 지상관측기 자료통합시스템 개발 Title: Development of Data Integration System for Ground-Based Space Weather Observational Facilities Authors: Baek, Ji-Hye; Choi, Seonghwan; Lee, Jae-Jin; Kim, Yeon-Han; Bong, Su-Chan; Park, Young-Deuk; Kwak, Young-Sil; Cho, Kyung-Suk; Hwang, Junga; Jang, Bi-Ho; Yang, Tae-Yong; Hwang, Eunmi; Park, Sung-Hong; Park, Jongyeob Bibcode: 2013PKAS...28...65B Altcode: No abstract at ADS Title: Temperature of Solar Prominences Obtained with the Fast Imaging Solar Spectrograph on the 1.6 m New Solar Telescope at the Big Bear Solar Observatory Authors: Park, Hyungmin; Chae, Jongchul; Song, Donguk; Maurya, Ram Ajor; Yang, Heesu; Park, Young-Deuk; Jang, Bi-Ho; Nah, Jakyoung; Cho, Kyung-Suk; Kim, Yeon-Han; Ahn, Kwangsu; Cao, Wenda; Goode, Philip R. Bibcode: 2013SoPh..288..105P Altcode: We observed solar prominences with the Fast Imaging Solar Spectrograph (FISS) at the Big Bear Solar Observatory on 30 June 2010 and 15 August 2011. To determine the temperature of the prominence material, we applied a nonlinear least-squares fitting of the radiative transfer model. From the Doppler broadening of the Hα and Ca II lines, we determined the temperature and nonthermal velocity separately. The ranges of temperature and nonthermal velocity were 4000 - 20 000 K and 4 - 11 km s−1. We also found that the temperature varied much from point to point within one prominence. Title: Fast Imaging Solar Spectrograph of the 1.6 Meter New Solar Telescope at Big Bear Solar Observatory Authors: Chae, Jongchul; Park, Hyung-Min; Ahn, Kwangsu; Yang, Heesu; Park, Young-Deuk; Nah, Jakyoung; Jang, Bi Ho; Cho, Kyung-Suk; Cao, Wenda; Goode, Philip R. Bibcode: 2013SoPh..288....1C Altcode: 2012SoPh..tmp..248C For high resolution spectral observations of the Sun - particularly its chromosphere, we have developed a dual-band echelle spectrograph named Fast Imaging Solar Spectrograph (FISS), and installed it in a vertical optical table in the Coudé Lab of the 1.6 meter New Solar Telescope at Big Bear Solar Observatory. This instrument can cover any part of the visible and near-infrared spectrum, but it usually records the Hα band and the Ca II 8542 Å band simultaneously using two CCD cameras, producing data well suited for the study of the structure and dynamics of the chromosphere and filaments/prominences. The instrument does imaging of high quality using a fast scan of the slit across the field of view with the aid of adaptive optics. We describe its design, specifics, and performance as well as data processing Title: Doppler Shifts of the Hα Line and the Ca II 854.2 nm Line in a Quiet Region of the Sun Observed with the FISS/NST Authors: Chae, Jongchul; Park, Hyung-Min; Ahn, Kwangsu; Yang, Heesu; Park, Young-Deuk; Cho, Kyung-Suk; Cao, Wenda Bibcode: 2013SoPh..288...89C Altcode: The characteristics of Doppler shifts in a quiet region of the Sun are compared between the Hα line and the Ca II infrared line at 854.2 nm. A small area of 16″×40″ was observed for about half an hour with the Fast Imaging Solar Spectrograph (FISS) of the 1.6 meter New Solar Telescope (NST) at Big Bear Solar Observatory. The observed area contains a network region and an internetwork region, and identified in the network region are fibrils and bright points. We infer Doppler velocity vm from each line profile at each individual point with the lambdameter method as a function of half wavelength separation Δλ. It is confirmed that the bisector of the spatially averaged Ca II line profile has an inverse C-shape with a significant peak redshift of + 1.8 km s−1. In contrast, the bisector of the spatially averaged Hα line profile has a C-shape with a small peak blueshift of − 0.5 km s−1. In both lines, the bisectors of bright network points are significantly redshifted not only at the line centers, but also at the wings. The Ca II Doppler shifts are found to be correlated with the Hα ones with the strongest correlation occurring in the internetwork region. Moreover, we find that here the Doppler shifts in the two lines are essentially in phase. We discuss the physical implications of our results in view of the formation of the Hα line and Ca II 854.2 nm line in the quiet region chromosphere. Title: Study of Magnetic Helicity Injection in the Active Region NOAA 9236 Producing Multiple Flare-associated Coronal Mass Ejection Events Authors: Park, Sung-Hong; Kusano, Kanya; Cho, Kyung-Suk; Chae, Jongchul; Bong, Su-Chan; Kumar, Pankaj; Park, So-Young; Kim, Yeon-Han; Park, Young-Deuk Bibcode: 2013ApJ...778...13P Altcode: 2013arXiv1308.5774P To better understand a preferred magnetic field configuration and its evolution during coronal mass ejection (CME) events, we investigated the spatial and temporal evolution of photospheric magnetic fields in the active region NOAA 9236 that produced eight flare-associated CMEs during the time period of 2000 November 23-26. The time variations of the total magnetic helicity injection rate and the total unsigned magnetic flux are determined and examined not only in the entire active region but also in some local regions such as the main sunspots and the CME-associated flaring regions using SOHO/MDI magnetogram data. As a result, we found that (1) in the sunspots, a large amount of positive (right-handed) magnetic helicity was injected during most of the examined time period, (2) in the flare region, there was a continuous injection of negative (left-handed) magnetic helicity during the entire period, accompanied by a large increase of the unsigned magnetic flux, and (3) the flaring regions were mainly composed of emerging bipoles of magnetic fragments in which magnetic field lines have substantially favorable conditions for making reconnection with large-scale, overlying, and oppositely directed magnetic field lines connecting the main sunspots. These observational findings can also be well explained by some MHD numerical simulations for CME initiation (e.g., reconnection-favored emerging flux models). We therefore conclude that reconnection-favored magnetic fields in the flaring emerging flux regions play a crucial role in producing the multiple flare-associated CMEs in NOAA 9236. Title: FISS Observations of Vertical Motion of Plasma in Tiny Pores Authors: Cho, K. -S.; Bong, S. -C.; Chae, J.; Kim, Y. -H.; Park, Y. -D.; Katsukawa, Y. Bibcode: 2013SoPh..288...23C Altcode: Pores can be exploited for the understanding of the interaction between small-scale vertical magnetic field and the surrounding convective motions as well as the transport of mechanical energy into the chromosphere along the magnetic field. For better understanding of the physics of pores, we investigate tiny pores in a new emerging active region (AR11117) that were observed on 26 October 2010 by the Solar Optical Telescope (SOT) on board Hinode and the Fast Imaging Solar Spectrograph (FISS) of the 1.6 meter New Solar Telescope (NST). The pores are compared with nearby small magnetic concentrations (SMCs), which have similar magnetic flux as the pores but do not appear dark. Magnetic flux density and Doppler velocities in the photosphere are estimated by applying the center-of-gravity method to the Hinode/Spectro-Polarimeter data. The line-of-sight motions in the lower chromosphere are determined by applying the bisector method to the wings of the Hα and the Ca II 8542 Å line simultaneously taken by the FISS. The coordinated observation reveals that the pores are filled with plasma which moves down slowly and are surrounded by stronger downflow in the photosphere. In the lower chromosphere, we found that the plasma flows upwards inside the pores while the plasma in the SMCs is always moving down. Our inspection of the Ca II 8542 Å line from the wing to the core shows that the upflow in the pores slows down with height and turns into downflow in the upper chromosphere while the downflow in the SMCs gains its speed. Our results are in agreement with the numerical studies which suggest that rapid cooling of the interior of the pores drives a strong downflow, which collides with the dense lower layer below and rebounds into an upflow. Title: Simultaneous EUV and radio observations of bidirectional plasmoids ejection during magnetic reconnection Authors: Kumar, Pankaj; Cho, Kyung-Suk Bibcode: 2013A&A...557A.115K Altcode: 2013arXiv1307.3910K We present a multiwavelength study of the X-class flare, which occurred in active region (AR) NOAA 11339 on 3 November 2011. The extreme ultraviolet (EUV) images recorded by SDO/AIA show the activation of a remote filament (located north of the AR) with footpoint brightenings about 50 min prior to the flare's occurrence. The kinked filament rises up slowly, and after reaching a projected height of ~49 Mm, it bends and falls freely near the AR, where the X-class flare was triggered. Dynamic radio spectrum from the Green Bank Solar Radio Burst Spectrometer (GBSRBS) shows simultaneous detection of both positive and negative drifting pulsating structures (DPSs) in the decimetric radio frequencies (500-1200 MHz) during the impulsive phase of the flare. The global negative DPSs in solar flares are generally interpreted as a signature of electron acceleration related to the upward-moving plasmoids in the solar corona. The EUV images from AIA 94 Å reveal the ejection of multiple plasmoids, which move simultaneously upward and downward in the corona during the magnetic reconnection. The estimated speeds of the upward- and downward-moving plasmoids are ~152-362 and ~83-254 km s-1, respectively. These observations strongly support the recent numerical simulations of the formation and interaction of multiple plasmoids due to tearing of the current-sheet structure. On the basis of our analysis, we suggest that the simultaneous detection of both the negative and positive DPSs is most likely generated by the interaction or coalescence of the multiple plasmoids moving upward and downward along the current-sheet structure during the magnetic reconnection process. Moreover, the differential emission measure (DEM) analysis of the active region reveals a hot flux-rope structure (visible in AIA 131 and 94 Å) prior to the flare initiation and ejection of the multitemperature plasmoids during the flare impulsive phase. Movie is available in electronic form at http://www.aanda.org Title: RHESSI and TRACE Observations of Multiple Flare Activity in AR 10656 and Associated Filament Eruption Authors: Joshi, Bhuwan; Kushwaha, Upendra; Cho, K. -S.; Veronig, Astrid M. Bibcode: 2013ApJ...771....1J Altcode: 2013arXiv1305.1493J We present Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) and Transition Region and Coronal Explorer (TRACE) observations of multiple flare activity that occurred in the NOAA active region 10656 over a period of 2 hr on 2004 August 18. Out of four successive flares, three were class C events, and the final event was a major X1.8 solar eruptive flare. The activities during the pre-eruption phase, i.e., before the X1.8 flare, are characterized by three localized episodes of energy release occurring in the vicinity of a filament that produces intense heating along with non-thermal emission. A few minutes before the eruption, the filament undergoes an activation phase during which it slowly rises with a speed of ~12 km s-1. The filament eruption is accompanied by an X1.8 flare, during which multiple hard X-ray (HXR) bursts are observed up to 100-300 keV energies. We observe a bright and elongated coronal structure simultaneously in E(UV) and 50-100 keV HXR images underneath the expanding filament during the period of HXR bursts, which provides strong evidence for ongoing magnetic reconnection. This phase is accompanied by very high plasma temperatures of ~31 MK, followed by the detachment of the prominence from the solar source region. From the location, timing, strength, and spectrum of HXR emission, we conclude that the prominence eruption is driven by the distinct events of magnetic reconnection occurring in the current sheet below the erupting prominence. These multi-wavelength observations also suggest that the localized magnetic reconnections associated with different evolutionary stages of the filament in the pre-eruption phase play an important role in destabilizing the active-region filament through the tether-cutting process, leading to large-scale eruption and X-class flare. Title: Propagation Characteristics of CMEs Associated with Magnetic Clouds and Ejecta Authors: Kim, R. -S.; Gopalswamy, N.; Cho, K. -S.; Moon, Y. -J.; Yashiro, S. Bibcode: 2013SoPh..284...77K Altcode: We have investigated the characteristics of magnetic cloud (MC) and ejecta (EJ) associated coronal mass ejections (CMEs) based on the assumption that all CMEs have a flux rope structure. For this, we used 54 CMEs and their interplanetary counterparts (interplanetary CMEs: ICMEs) that constitute the list of events used by the NASA/LWS Coordinated Data Analysis Workshop (CDAW) on CME flux ropes. We considered the location, angular width, and speed as well as the direction parameter, D. The direction parameter quantifies the degree of asymmetry of the CME shape in coronagraph images, and shows how closely the CME propagation is directed to Earth. For the 54 CDAW events, we found the following properties of the CMEs: i) the average value of D for the 23 MCs (0.62) is larger than that for the 31 EJs (0.49), which indicates that the MC-associated CMEs propagate more directly toward the Earth than the EJ-associated CMEs; ii) comparison between the direction parameter and the source location shows that the majority of the MC-associated CMEs are ejected along the radial direction, while many of the EJ-associated CMEs are ejected non-radially; iii) the mean speed of MC-associated CMEs (946 km s−1) is faster than that of EJ-associated CMEs (771 km s−1). For seven very fast CMEs (≥ 1500 km s−1), all CMEs with large D (≥ 0.4) are associated with MCs and the CMEs with small D are associated with EJs. From the statistical analysis of CME parameters, we found the superiority of the direction parameter. Based on these results, we suggest that the CME trajectory essentially determines the observed ICME structure. Title: Observation of a Non-radial Penumbra in a Flux Emerging Region under Chromospheric Canopy Fields Authors: Lim, Eun-Kyung; Yurchyshyn, Vasyl; Goode, Philip; Cho, Kyung-Suk Bibcode: 2013ApJ...769L..18L Altcode: The presence of a penumbra is one of the main properties of a mature sunspot, but its formation mechanism has been elusive due to a lack of observations that fully cover the formation process. Utilizing the New Solar Telescope at the Big Bear Solar Observatory, we observed the formation of a partial penumbra for about 7 hr simultaneously at the photospheric (TiO; 7057 Å) and the chromospheric (Hα - 1 Å) spectral lines with high spatial and temporal resolution. From this uninterrupted, long observing sequence, we found that the formation of the observed penumbra was closely associated with flux emergence under the pre-existing chromospheric canopy fields. Based on this finding, we suggest a possible scenario for penumbra formation in which a penumbra forms when the emerging flux is constrained from continuing to emerge, but rather is trapped at the photospheric level by the overlying chromospheric canopy fields. Title: Comparison of Helicity Signs in Interplanetary CMEs and Their Solar Source Regions Authors: Cho, K. -S.; Park, S. -H.; Marubashi, K.; Gopalswamy, N.; Akiyama, S.; Yashiro, S.; Kim, R. -S.; Lim, E. -K. Bibcode: 2013SoPh..284..105C Altcode: If all coronal mass ejections (CMEs) have flux ropes, then the CMEs should keep their helicity signs from the Sun to the Earth according to the helicity conservation principle. This study presents an attempt to answer the question from the Coordinated Data Analysis Workshop (CDAW), "Do all CMEs have flux ropes?", by using a qualitative helicity sign comparison between interplanetary CMEs (ICMEs) and their CME source regions. For this, we select 34 CME-ICME pairs whose source active regions (ARs) have continuous SOHO/MDI magnetogram data covering more than 24 hr without data gap during the passage of the ARs near the solar disk center. The helicity signs in the ARs are determined by estimation of cumulative magnetic helicity injected through the photosphere in the entire source ARs. The helicity signs in the ICMEs are estimated by applying the cylinder model developed by Marubashi (Adv. Space. Res., 26, 55, 2000) to 16 second resolution magnetic field data from the MAG instrument onboard the ACE spacecraft. It is found that 30 out of 34 events (88 %) are helicity sign-consistent events, while four events (12 %) are sign-inconsistent. Through a detailed investigation of the source ARs of the four sign-inconsistent events, we find that those events can be explained by the local helicity sign opposite to that of the entire AR helicity (28 July 2000 ICME), incorrectly reported solar source region in the CDAW list (20 May 2005 ICME), or the helicity sign of the pre-existing coronal magnetic field (13 October 2000 and 20 November 2003 ICMEs). We conclude that the helicity signs of the ICMEs are quite consistent with those of the injected helicities in the AR regions from where the CMEs erupted. Title: Progress Report of Korean Data Center for SDO Authors: Choi, S.; Hwang, E.; Baek, J. -H.; Kim, Y. -H.; Park, Y. -D.; Cho, K. -S. Bibcode: 2013enss.confE.136C Altcode: KASI has been constructing Korean Data Center for SDO based on the letter of agreement between KASI and NASA for space weather research. We have installed a data transfer server and a storage system about 1.5 PB. We have successfully installed NetDRMS to synchronize database and JMD to download FITS files with the help of Stanford University and NSO. We will increase its storage capacity more from year to year. In 2013, we will improve network performance and stability through GLORIAD between Stanford University and KASI, and it will be integrated with VSO (Virtual Solar Observatory). In addition, scientists and space weather institutes will be able to access Korean data center through the website (http://sdo.kasi.re.kr) and the visualization tool that is in development and be scheduled to be released in the middle of this year. The Korean Data Center for SDO will contribute space weather researches and applications not only in Korea but also over the world. Title: A High-frequency Type II Solar Radio Burst Associated with the 2011 February 13 Coronal Mass Ejection Authors: Cho, K. -S.; Gopalswamy, N.; Kwon, R. -Y.; Kim, R. -S.; Yashiro, S. Bibcode: 2013ApJ...765..148C Altcode: We examine the relationship between the high-frequency (425 MHz) type II radio burst and the associated white-light coronal mass ejection (CME) that occurred on 2011 February 13. The radio burst had a drift rate of 2.5 MHz s-1, indicating a relatively high shock speed. From SDO/AIA observations we find that a loop-like erupting front sweeps across high-density coronal loops near the start time of the burst (17:34:17 UT). The deduced distance of shock formation (0.06 Rs) from the flare center and speed of the shock (1100 km s-1) using the measured density from SDO/AIA observations are comparable to the height (0.05 Rs, from the solar surface) and speed (700 km s-1) of the CME leading edge observed by STEREO/EUVI. We conclude that the type II burst originates even in the low corona (<59 Mm or 0.08 Rs, above the solar surface) due to the fast CME shock passing through high-density loops. Title: STEREO Observations of Fast Magnetosonic Waves in the Extended Solar Corona Associated with EIT/EUV Waves Authors: Kwon, Ryun-Young; Ofman, Leon; Olmedo, Oscar; Kramar, Maxim; Davila, Joseph M.; Thompson, Barbara J.; Cho, Kyung-Suk Bibcode: 2013ApJ...766...55K Altcode: We report white-light observations of a fast magnetosonic wave associated with a coronal mass ejection observed by STEREO/SECCHI/COR1 inner coronagraphs on 2011 August 4. The wave front is observed in the form of density compression passing through various coronal regions such as quiet/active corona, coronal holes, and streamers. Together with measured electron densities determined with STEREO COR1 and Extreme UltraViolet Imager (EUVI) data, we use our kinematic measurements of the wave front to calculate coronal magnetic fields and find that the measured speeds are consistent with characteristic fast magnetosonic speeds in the corona. In addition, the wave front turns out to be the upper coronal counterpart of the EIT wave observed by STEREO EUVI traveling against the solar coronal disk; moreover, stationary fronts of the EIT wave are found to be located at the footpoints of deflected streamers and boundaries of coronal holes, after the wave front in the upper solar corona passes through open magnetic field lines in the streamers. Our findings suggest that the observed EIT wave should be in fact a fast magnetosonic shock/wave traveling in the inhomogeneous solar corona, as part of the fast magnetosonic wave propagating in the extended solar corona. Title: Multiwavelength Study of a Solar Eruption from AR NOAA 11112 I. Flux Emergence, Sunspot Rotation and Triggering of a Solar Flare Authors: Kumar, Pankaj; Park, Sung-Hong; Cho, K. -S.; Bong, S. -C. Bibcode: 2013SoPh..282..503K Altcode: 2012arXiv1210.3413K We analyze the multiwavelength observations of an M2.9/1N flare that occurred in the active region (AR) NOAA 11112 in the vicinity of a huge filament system on 16 October 2010. SDO/HMI magnetograms reveal the emergence of a bipole (within the existing AR) 50 hours prior to the flare event. During the emergence, both the positive and negative sunspots in the bipole show translational as well as rotational motion. The positive-polarity sunspot shows significant motion/rotation in the south-westward/clockwise direction, and we see continuously pushing/sliding of the surrounding opposite-polarity field region. On the other hand, the negative-polarity sunspot moves/rotates in the westward/anticlockwise direction. The positive-polarity sunspot rotates ≈ 70∘ within 30 hours, whereas the one with negative polarity rotates ≈ 20∘ within 10 hours. SDO/AIA 94 Å EUV images show the emergence of a flux tube in the corona, consistent with the emergence of the bipole in HMI. The footpoints of the flux tube were anchored in the emerging bipole. The initial brightening starts at one of the footpoints (western) of the emerging loop system, where the positive-polarity sunspot pushes/slides towards a nearby negative-polarity field region. A high speed plasmoid ejection (speed ≈ 1197 km s−1) was observed during the impulsive phase of the flare, which suggests magnetic reconnection of the emerging positive-polarity sunspot with the surrounding opposite-polarity field region. The entire AR shows positive-helicity injection before the flare event. Moreover, the newly emerging bipole reveals the signature of a negative (left-handed) helicity. These observations provide unique evidence of the emergence of twisted flux tubes from below the photosphere to coronal heights, triggering a flare mainly due to the interaction between the emerging positive-polarity sunspot and a nearby negative-polarity sunspot by the shearing motion of the emerging positive sunspot towards the negative one. Our observations also strongly support the idea that the rotation can most likely be attributed to the emergence of twisted magnetic fields, as proposed by recent models. Title: Multiwavelength Study of a Solar Eruption from AR NOAA 11112: II. Large-Scale Coronal Wave and Loop Oscillation Authors: Kumar, Pankaj; Cho, K. -S.; Chen, P. F.; Bong, S. -C.; Park, Sung-Hong Bibcode: 2013SoPh..282..523K Altcode: 2012arXiv1210.3417K We analyze multiwavelength observations of an M2.9/1N flare that occurred in AR NOAA 11112 on 16 October 2010. AIA 211 Å EUV images reveal the presence of a faster coronal wave (decelerating from ≈ 1390 to ≈ 830 km s−1) propagating ahead of a slower wave (decelerating from ≈ 416 to ≈ 166 km s−1) towards the western limb. The dynamic radio spectrum from Sagamore Hill radio telescope shows the presence of a metric type II radio burst, which reveals the presence of a coronal shock wave (speed ≈ 800 km s−1). The speed of the faster coronal wave, derived from AIA 211 Å images, is found to be comparable to the coronal shock speed. AIA 171 Å high-cadence observations showed that a coronal loop, which was located at a distance of ≈ 0.32R⊙ to the west of the flaring region, started to oscillate by the end of the impulsive phase of the flare. The results indicate that the faster coronal wave may be the first driver of the transversal oscillations of coronal loop. As the slower wave passed through the coronal loop, the oscillations became even stronger. There was a plasmoid eruption observed in EUV and a white-light CME was recorded, having velocity of ≈ 340 - 350 km s−1. STEREO 195 Å images show an EIT wave, propagating in the same direction as the lower-speed coronal wave observed in AIA, but decelerating from ≈ 320 to ≈ 254 km s−1. These observations reveal the co-existence of both waves (i.e. coronal Moreton and EIT waves), and the type II radio burst seems to be associated with the coronal Moreton wave. Title: Multi-wavelength investigation of pre-flare activity and magnetic reconnection during the evolutionary phases of a solar eruptive flare Authors: Joshi, Bhuwan; Veronig, Astrid; Cho, Kyung-Suk; Bong, Su-chan; Tiwari, Sanjiv Kumar; Lee, J. Bibcode: 2012cosp...39..845J Altcode: 2012cosp.meet..845J No abstract at ADS Title: Day-to-day variability of equatorial anomaly in GPS-TEC during low solar activity period Authors: Aggarwal, Malini; Joshi, H. P.; Iyer, K. N.; Kwak, Y. -S.; Lee, J. J.; Chandra, H.; Cho, K. S. Bibcode: 2012AdSpR..49.1709A Altcode: The ionospheric total electron content (TEC) in the northern hemispheric equatorial ionization anomaly (EIA) crest region is investigated by using dual-frequency signals of the Global Positioning System (GPS) acquired from Rajkot (Geog. Lat. 22.29°N, Geog. Long. 70.74°E; Geom. Lat. 14.21°N, Geom. Long. 144.90°E), India. The day-to-day variability of EIA characteristics is examined during low solar activity period (F10.7∼83 sfu). It is found that the daily maximum TEC at EIA crest exhibits a day-to-day and strong semi-annual variability. The seasonal anomaly and equinoctial asymmetry in TEC at EIA is found non-existent and weaker, respectively. We found a moderate and positive correlation of daily magnitude of crest, Ic with daily F10.7 and EUV fluxes with a correlation coefficient of 0.43 and 0.33, respectively indicating an existence of a short-term relation between TEC at EIA and the solar radiation even during low solar activity period. The correlation of daily Ic with Dst index is also moderate (r = -0.35), whereas no correlation is found with the daily Kp index (r = 0.14) respectively. We found that the magnitude of EIA crest is moderately correlated with solar flux in all seasons except winter where it is weakly related (0.27). The magnitude of EIA crest is also found highly related with EEJ strength in spring (r = 0.69) and summer (r = 0.65) than autumn (0.5) and winter (r = 0.47), though EEJ is stronger in autumn than spring. Title: The Occurrence and Speed of CMEs Related to Two Characteristic Evolution Patterns of Helicity Injection in Their Solar Source Regions Authors: Park, Sung-Hong; Cho, Kyung-Suk; Bong, Su-Chan; Kumar, Pankaj; Chae, Jongchul; Liu, Rui; Wang, Haimin Bibcode: 2012ApJ...750...48P Altcode: 2012arXiv1203.1690P Long-term (a few days) variation of magnetic helicity injection was calculated for 28 solar active regions that produced 47 coronal mass ejections (CMEs) to find its relationship to the CME occurrence and speed using SOHO/MDI line-of-sight magnetograms. As a result, we found that the 47 CMEs can be categorized into two different groups by two characteristic evolution patterns of helicity injection in their source active regions, which appeared for ~0.5-4.5 days before their occurrence: (1) a monotonically increasing pattern with one sign of helicity (Group A 30 CMEs in 23 active regions) and (2) a pattern of significant helicity injection followed by its sign reversal (Group B 17 CMEs in 5 active regions). We also found that CME speed has a correlation with average helicity injection rate with linear correlation coefficients of 0.85 and 0.63 for Group A and Group B, respectively. In addition, these two CME groups show different characteristics as follows: (1) the average CME speed of Group B (1330 km s-1) is much faster than that of Group A (870 km s-1), (2) the CMEs in Group A tend to be single events whereas those in Group B mainly consist of successive events, and (3) flares related to the CMEs in Group B are relatively more energetic and impulsive than those in Group A. Our findings therefore suggest that the two CME groups have different pre-CME conditions in their source active regions and different CME characteristics. Title: Search for a Dark Matter Candidate Produced in Association with a Single Top Quark in pp¯ Collisions at s=1.96TeV Authors: Aaltonen, T.; Álvarez González, B.; Amerio, S.; Amidei, D.; Anastassov, A.; Annovi, A.; Antos, J.; Anzá, F.; Apollinari, G.; Appel, J. A.; Arisawa, T.; Artikov, A.; Asaadi, J.; Ashmanskas, W.; Auerbach, B.; Aurisano, A.; Azfar, F.; Badgett, W.; Bae, T.; Barbaro-Galtieri, A.; Barnes, V. E.; Barnett, B. A.; Barria, P.; Bartos, P.; Bauce, M.; Bedeschi, F.; Behari, S.; Bellettini, G.; Bellinger, J.; Benjamin, D.; Beretvas, A.; Bhatti, A.; Bisello, D.; Bizjak, I.; Bland, K. R.; Blumenfeld, B.; Bocci, A.; Bodek, A.; Bortoletto, D.; Boudreau, J.; Boveia, A.; Brigliadori, L.; Bromberg, C.; Brucken, E.; Budagov, J.; Budd, H. S.; Burkett, K.; Busetto, G.; Bussey, P.; Buzatu, A.; Calamba, A.; Calancha, C.; Camarda, S.; Campanelli, M.; Campbell, M.; Canelli, F.; Carls, B.; Carlsmith, D.; Carosi, R.; Carrillo, S.; Carron, S.; Casal, B.; Casarsa, M.; Castro, A.; Catastini, P.; Cauz, D.; Cavaliere, V.; Cavalli-Sforza, M.; Cerri, A.; Cerrito, L.; Chen, Y. C.; Chertok, M.; Chiarelli, G.; Chlachidze, G.; Chlebana, F.; Cho, K.; Chokheli, D.; Chung, W. H.; Chung, Y. S.; Ciocci, M. A.; Clark, A.; Clarke, C.; Compostella, G.; Convery, M. E.; Conway, J.; Corbo, M.; Cordelli, M.; Cox, C. A.; Cox, D. J.; Crescioli, F.; Cuevas, J.; Culbertson, R.; Dagenhart, D.; d'Ascenzo, N.; Datta, M.; de Barbaro, P.; Dell'Orso, M.; Demortier, L.; Deninno, M.; Devoto, F.; d'Errico, M.; Di Canto, A.; Di Ruzza, B.; Dittmann, J. R.; D'Onofrio, M.; Donati, S.; Dong, P.; Dorigo, M.; Dorigo, T.; Ebina, K.; Elagin, A.; Eppig, A.; Erbacher, R.; Errede, S.; Ershaidat, N.; Eusebi, R.; Farrington, S.; Feindt, M.; Fernandez, J. P.; Field, R.; Flanagan, G.; Forrest, R.; Frank, M. J.; Franklin, M.; Freeman, J. C.; Fuks, B.; Funakoshi, Y.; Furic, I.; Gallinaro, M.; Garcia, J. E.; Garfinkel, A. F.; Garosi, P.; Gerberich, H.; Gerchtein, E.; Giagu, S.; Giakoumopoulou, V.; Giannetti, P.; Gibson, K.; Ginsburg, C. M.; Giokaris, N.; Giromini, P.; Giurgiu, G.; Glagolev, V.; Glenzinski, D.; Gold, M.; Goldin, D.; Goldschmidt, N.; Golossanov, A.; Gomez, G.; Gomez-Ceballos, G.; Goncharov, M.; González, O.; Gorelov, I.; Goshaw, A. T.; Goulianos, K.; Grinstein, S.; Grosso-Pilcher, C.; Group, R. C.; Guimaraes da Costa, J.; Hahn, S. R.; Halkiadakis, E.; Hamaguchi, A.; Han, J. Y.; Happacher, F.; Hara, K.; Hare, D.; Hare, M.; Harr, R. F.; Hatakeyama, K.; Hays, C.; Heck, M.; Heinrich, J.; Herndon, M.; Hewamanage, S.; Hocker, A.; Hopkins, W.; Horn, D.; Hou, S.; Hughes, R. E.; Hurwitz, M.; Husemann, U.; Hussain, N.; Hussein, M.; Huston, J.; Introzzi, G.; Iori, M.; Ivanov, A.; James, E.; Jang, D.; Jayatilaka, B.; Jeon, E. J.; Jindariani, S.; Jones, M.; Joo, K. K.; Jun, S. Y.; Junk, T. R.; Kamon, T.; Karchin, P. E.; Kasmi, A.; Kato, Y.; Ketchum, W.; Keung, J.; Khotilovich, V.; Kilminster, B.; Kim, D. H.; Kim, H. S.; Kim, J. E.; Kim, M. J.; Kim, S. B.; Kim, S. H.; Kim, Y. K.; Kim, Y. J.; Kimura, N.; Kirby, M.; Klimenko, S.; Knoepfel, K.; Kondo, K.; Kong, D. J.; Konigsberg, J.; Kotwal, A. V.; Kreps, M.; Kroll, J.; Krop, D.; Kruse, M.; Krutelyov, V.; Kuhr, T.; Kurata, M.; Kwang, S.; Laasanen, A. T.; Lami, S.; Lammel, S.; Lancaster, M.; Lander, R. L.; Lannon, K.; Lath, A.; Latino, G.; LeCompte, T.; Lee, E.; Lee, H. S.; Lee, J. S.; Lee, S. W.; Leo, S.; Leone, S.; Lewis, J. D.; Limosani, A.; Lin, C. -J.; Lindgren, M.; Lipeles, E.; Lister, A.; Litvintsev, D. O.; Liu, C.; Liu, H.; Liu, Q.; Liu, T.; Lockwitz, S.; Loginov, A.; Lucchesi, D.; Lueck, J.; Lujan, P.; Lukens, P.; Lungu, G.; Lys, J.; Lysak, R.; Madrak, R.; Maeshima, K.; Maestro, P.; Malik, S.; Manca, G.; Manousakis-Katsikakis, A.; Margaroli, F.; Marino, C.; Martínez, M.; Mastrandrea, P.; Matera, K.; Mattson, M. E.; Mazzacane, A.; Mazzanti, P.; McFarland, K. S.; McIntyre, P.; McNulty, R.; Mehta, A.; Mehtala, P.; Mesropian, C.; Miao, T.; Mietlicki, D.; Mitra, A.; Miyake, H.; Moed, S.; Moggi, N.; Mondragon, M. N.; Moon, C. S.; Moore, R.; Morello, M. J.; Morlock, J.; Movilla Fernandez, P.; Mukherjee, A.; Muller, Th.; Murat, P.; Mussini, M.; Nachtman, J.; Nagai, Y.; Naganoma, J.; Nakano, I.; Napier, A.; Nett, J.; Neu, C.; Neubauer, M. S.; Nielsen, J.; Nodulman, L.; Noh, S. Y.; Norniella, O.; Oakes, L.; Oh, S. H.; Oh, Y. D.; Oksuzian, I.; Okusawa, T.; Orava, R.; Ortolan, L.; Pagan Griso, S.; Pagliarone, C.; Palencia, E.; Papadimitriou, V.; Paramonov, A. A.; Patrick, J.; Pauletta, G.; Paulini, M.; Paus, C.; Pellett, D. E.; Penzo, A.; Phillips, T. J.; Piacentino, G.; Pianori, E.; Pilot, J.; Pitts, K.; Plager, C.; Pondrom, L.; Poprocki, S.; Potamianos, K.; Prokoshin, F.; Pranko, A.; Ptohos, F.; Punzi, G.; Rahaman, A.; Ramakrishnan, V.; Ranjan, N.; Redondo, I.; Renton, P.; Rescigno, M.; Riddick, T.; Rimondi, F.; Ristori, L.; Robson, A.; Rodrigo, T.; Rodriguez, T.; Rogers, E.; Rolli, S.; Roser, R.; Ruffini, F.; Ruiz, A.; Russ, J.; Rusu, V.; Safonov, A.; Sakumoto, W. K.; Sakurai, Y.; Santi, L.; Sato, K.; Saveliev, V.; Savoy-Navarro, A.; Schlabach, P.; Schmidt, A.; Schmidt, E. E.; Schwarz, T.; Scodellaro, L.; Scribano, A.; Scuri, F.; Seidel, S.; Seiya, Y.; Semenov, A.; Sforza, F.; Shalhout, S. Z.; Shears, T.; Shepard, P. F.; Shimojima, M.; Shochet, M.; Shreyber-Tecker, I.; Simonenko, A.; Sinervo, P.; Sliwa, K.; Smith, J. R.; Snider, F. D.; Soha, A.; Sorin, V.; Song, H.; Squillacioti, P.; Stancari, M.; St. Denis, R.; Stelzer, B.; Stelzer-Chilton, O.; Stentz, D.; Strologas, J.; Strycker, G. L.; Sudo, Y.; Sukhanov, A.; Suslov, I.; Takemasa, K.; Takeuchi, Y.; Tang, J.; Tecchio, M.; Teng, P. K.; Thom, J.; Thome, J.; Thompson, G. A.; Thomson, E.; Toback, D.; Tokar, S.; Tollefson, K.; Tomura, T.; Tonelli, D.; Torre, S.; Torretta, D.; Totaro, P.; Trovato, M.; Ukegawa, F.; Uozumi, S.; Varganov, A.; Vázquez, F.; Velev, G.; Vellidis, C.; Vidal, M.; Vila, I.; Vilar, R.; Vizán, J.; Vogel, M.; Volpi, G.; Wagner, P.; Wagner, R. L.; Wakisaka, T.; Wallny, R.; Wang, S. M.; Warburton, A.; Waters, D.; Wester, W. C., III; Whiteson, D.; Wicklund, A. B.; Wicklund, E.; Wilbur, S.; Wick, F.; Williams, H. H.; Wilson, J. S.; Wilson, P.; Winer, B. L.; Wittich, P.; Wolbers, S.; Wolfe, H.; Wright, T.; Wu, X.; Wu, Z.; Yamamoto, K.; Yamato, D.; Yang, T.; Yang, U. K.; Yang, Y. C.; Yao, W. -M.; Yeh, G. P.; Yi, K.; Yoh, J.; Yorita, K.; Yoshida, T.; Yu, G. B.; Yu, I.; Yu, S. S.; Yun, J. C.; Zanetti, A.; Zeng, Y.; Zhou, C.; Zucchelli, S. Bibcode: 2012PhRvL.108t1802A Altcode: 2012arXiv1202.5653C We report a new search for dark matter in a data sample of an integrated luminosity of 7.7fb-1 of Tevatron pp¯ collisions at s=1.96TeV, collected by the CDF II detector. We search for production of a dark-matter candidate, D, in association with a single top quark. We consider the hadronic decay mode of the top quark exclusively, yielding a final state of three jets with missing transverse energy. The data are consistent with the standard model; we thus set 95% confidence level upper limits on the cross section of the process pp¯→t+D as a function of the mass of the dark-matter candidate. The limits are approximately 0.5 pb for a dark-matter particle with mass in the range of 0-150GeV/c2. Title: Search for Dark Matter in Events with One Jet and Missing Transverse Energy in pp¯ Collisions at s=1.96TeV Authors: Aaltonen, T.; Álvarez González, B.; Amerio, S.; Amidei, D.; Anastassov, A.; Annovi, A.; Antos, J.; Apollinari, G.; Appel, J. A.; Arisawa, T.; Artikov, A.; Asaadi, J.; Ashmanskas, W.; Auerbach, B.; Aurisano, A.; Azfar, F.; Badgett, W.; Bae, T.; Bai, Y.; Barbaro-Galtieri, A.; Barnes, V. E.; Barnett, B. A.; Barria, P.; Bartos, P.; Bauce, M.; Bedeschi, F.; Behari, S.; Bellettini, G.; Bellinger, J.; Benjamin, D.; Beretvas, A.; Bhatti, A.; Bisello, D.; Bizjak, I.; Bland, K. R.; Blumenfeld, B.; Bocci, A.; Bodek, A.; Bortoletto, D.; Boudreau, J.; Boveia, A.; Brigliadori, L.; Bromberg, C.; Brucken, E.; Budagov, J.; Budd, H. S.; Burkett, K.; Busetto, G.; Bussey, P.; Buzatu, A.; Calamba, A.; Calancha, C.; Camarda, S.; Campanelli, M.; Campbell, M.; Canelli, F.; Carls, B.; Carlsmith, D.; Carosi, R.; Carrillo, S.; Carron, S.; Casal, B.; Casarsa, M.; Castro, A.; Catastini, P.; Cauz, D.; Cavaliere, V.; Cavalli-Sforza, M.; Cerri, A.; Cerrito, L.; Chen, Y. C.; Chertok, M.; Chiarelli, G.; Chlachidze, G.; Chlebana, F.; Cho, K.; Chokheli, D.; Chung, W. H.; Chung, Y. S.; Ciocci, M. A.; Clark, A.; Clarke, C.; Compostella, G.; Convery, M. E.; Conway, J.; Corbo, M.; Cordelli, M.; Cox, C. A.; Cox, D. J.; Crescioli, F.; Cuevas, J.; Culbertson, R.; Dagenhart, D.; d'Ascenzo, N.; Datta, M.; de Barbaro, P.; Dell'Orso, M.; Demortier, L.; Deninno, M.; Devoto, F.; d'Errico, M.; Di Canto, A.; Di Ruzza, B.; Dittmann, J. R.; D'Onofrio, M.; Donati, S.; Dong, P.; Dorigo, M.; Dorigo, T.; Ebina, K.; Elagin, A.; Eppig, A.; Erbacher, R.; Errede, S.; Ershaidat, N.; Eusebi, R.; Farrington, S.; Feindt, M.; Fernandez, J. P.; Field, R.; Flanagan, G.; Forrest, R.; Fox, P. J.; Frank, M. J.; Franklin, M.; Freeman, J. C.; Funakoshi, Y.; Furic, I.; Gallinaro, M.; Garcia, J. E.; Garfinkel, A. F.; Garosi, P.; Gerberich, H.; Gerchtein, E.; Giagu, S.; Giakoumopoulou, V.; Giannetti, P.; Gibson, K.; Ginsburg, C. M.; Giokaris, N.; Giromini, P.; Giurgiu, G.; Glagolev, V.; Glenzinski, D.; Gold, M.; Goldin, D.; Goldschmidt, N.; Golossanov, A.; Gomez, G.; Gomez-Ceballos, G.; Goncharov, M.; González, O.; Gorelov, I.; Goshaw, A. T.; Goulianos, K.; Grinstein, S.; Grosso-Pilcher, C.; Group, R. C.; Guimaraes da Costa, J.; Hahn, S. R.; Halkiadakis, E.; Hamaguchi, A.; Han, J. Y.; Happacher, F.; Hara, K.; Hare, D.; Hare, M.; Harnik, R.; Harr, R. F.; Hatakeyama, K.; Hays, C.; Heck, M.; Heinrich, J.; Herndon, M.; Hewamanage, S.; Hocker, A.; Hopkins, W.; Horn, D.; Hou, S.; Hughes, R. E.; Hurwitz, M.; Husemann, U.; Hussain, N.; Hussein, M.; Huston, J.; Introzzi, G.; Iori, M.; Ivanov, A.; James, E.; Jang, D.; Jayatilaka, B.; Jeon, E. J.; Jindariani, S.; Jones, M.; Joo, K. K.; Jun, S. Y.; Junk, T. R.; Kamon, T.; Karchin, P. E.; Kasmi, A.; Kato, Y.; Ketchum, W.; Keung, J.; Khotilovich, V.; Kilminster, B.; Kim, D. H.; Kim, H. S.; Kim, J. E.; Kim, M. J.; Kim, S. B.; Kim, S. H.; Kim, Y. K.; Kim, Y. J.; Kimura, N.; Kirby, M.; Klimenko, S.; Knoepfel, K.; Kondo, K.; Kong, D. J.; Konigsberg, J.; Kotwal, A. V.; Kreps, M.; Kroll, J.; Krop, D.; Kruse, M.; Krutelyov, V.; Kuhr, T.; Kurata, M.; Kwang, S.; Laasanen, A. T.; Lami, S.; Lammel, S.; Lancaster, M.; Lander, R. L.; Lannon, K.; Lath, A.; Latino, G.; LeCompte, T.; Lee, E.; Lee, H. S.; Lee, J. S.; Lee, S. W.; Leo, S.; Leone, S.; Lewis, J. D.; Limosani, A.; Lin, C. -J.; Lindgren, M.; Lipeles, E.; Lister, A.; Litvintsev, D. O.; Liu, C.; Liu, H.; Liu, Q.; Liu, T.; Lockwitz, S.; Loginov, A.; Lucchesi, D.; Lueck, J.; Lujan, P.; Lukens, P.; Lungu, G.; Lys, J.; Lysak, R.; Madrak, R.; Maeshima, K.; Maestro, P.; Malik, S.; Manca, G.; Manousakis-Katsikakis, A.; Margaroli, F.; Marino, C.; Martínez, M.; Mastrandrea, P.; Matera, K.; Mattson, M. E.; Mazzacane, A.; Mazzanti, P.; McFarland, K. S.; McIntyre, P.; McNulty, R.; Mehta, A.; Mehtala, P.; Mesropian, C.; Miao, T.; Mietlicki, D.; Mitra, A.; Miyake, H.; Moed, S.; Moggi, N.; Mondragon, M. N.; Moon, C. S.; Moore, R.; Morello, M. J.; Morlock, J.; Movilla Fernandez, P.; Mukherjee, A.; Muller, Th.; Murat, P.; Mussini, M.; Nachtman, J.; Nagai, Y.; Naganoma, J.; Nakano, I.; Napier, A.; Nett, J.; Neu, C.; Neubauer, M. S.; Nielsen, J.; Nodulman, L.; Noh, S. Y.; Norniella, O.; Oakes, L.; Oh, S. H.; Oh, Y. D.; Oksuzian, I.; Okusawa, T.; Orava, R.; Ortolan, L.; Pagan Griso, S.; Pagliarone, C.; Palencia, E.; Papadimitriou, V.; Paramonov, A. A.; Patrick, J.; Pauletta, G.; Paus, C.; Pellett, D. E.; Penzo, A.; Phillips, T. J.; Piacentino, G.; Pianori, E.; Pilot, J.; Pitts, K.; Plager, C.; Pondrom, L.; Poprocki, S.; Potamianos, K.; Prokoshin, F.; Pranko, A.; Ptohos, F.; Punzi, G.; Rahaman, A.; Ramakrishnan, V.; Ranjan, N.; Redondo, I.; Renton, P.; Rescigno, M.; Riddick, T.; Rimondi, F.; Ristori, L.; Robson, A.; Rodrigo, T.; Rodriguez, T.; Rogers, E.; Rolli, S.; Roser, R.; Ruffini, F.; Ruiz, A.; Russ, J.; Rusu, V.; Safonov, A.; Sakumoto, W. K.; Sakurai, Y.; Santi, L.; Sato, K.; Saveliev, V.; Savoy-Navarro, A.; Schlabach, P.; Schmidt, A.; Schmidt, E. E.; Schwarz, T.; Scodellaro, L.; Scribano, A.; Scuri, F.; Seidel, S.; Seiya, Y.; Semenov, A.; Sforza, F.; Shalhout, S. Z.; Shears, T.; Shepard, P. F.; Shimojima, M.; Shochet, M.; Shreyber-Tecker, I.; Simonenko, A.; Sinervo, P.; Sliwa, K.; Smith, J. R.; Snider, F. D.; Soha, A.; Sorin, V.; Song, H.; Squillacioti, P.; Stancari, M.; St. Denis, R.; Stelzer, B.; Stelzer-Chilton, O.; Stentz, D.; Strologas, J.; Strycker, G. L.; Sudo, Y.; Sukhanov, A.; Suslov, I.; Takemasa, K.; Takeuchi, Y.; Tang, J.; Tecchio, M.; Teng, P. K.; Thom, J.; Thome, J.; Thompson, G. A.; Thomson, E.; Toback, D.; Tokar, S.; Tollefson, K.; Tomura, T.; Tonelli, D.; Torre, S.; Torretta, D.; Totaro, P.; Trovato, M.; Ukegawa, F.; Uozumi, S.; Varganov, A.; Vázquez, F.; Velev, G.; Vellidis, C.; Vidal, M.; Vila, I.; Vilar, R.; Vizán, J.; Vogel, M.; Volpi, G.; Wagner, P.; Wagner, R. L.; Wakisaka, T.; Wallny, R.; Wang, S. M.; Warburton, A.; Waters, D.; Wester, W. C., III; Whiteson, D.; Wicklund, A. B.; Wicklund, E.; Wilbur, S.; Wick, F.; Williams, H. H.; Wilson, J. S.; Wilson, P.; Winer, B. L.; Wittich, P.; Wolbers, S.; Wolfe, H.; Wright, T.; Wu, X.; Wu, Z.; Yamamoto, K.; Yamato, D.; Yang, T.; Yang, U. K.; Yang, Y. C.; Yao, W. -M.; Yeh, G. P.; Yi, K.; Yoh, J.; Yorita, K.; Yoshida, T.; Yu, G. B.; Yu, I.; Yu, S. S.; Yun, J. C.; Zanetti, A.; Zeng, Y.; Zhou, C.; Zucchelli, S. Bibcode: 2012PhRvL.108u1804A Altcode: 2012arXiv1203.0742T We present the results of a search for dark matter production in the monojet signature. We analyze a sample of Tevatron pp¯ collisions at s=1.96TeV corresponding to an integrated luminosity of 6.7fb-1 recorded by the CDF II detector. In events with large missing transverse energy and one energetic jet, we find good agreement between the standard model prediction and the observed data. We set 90% confidence level upper limits on the dark matter production rate. The limits are translated into bounds on nucleon-dark matter scattering rates which are competitive with current direct detection bounds on spin-independent interaction below a dark matter candidate mass of 5GeV/c2, and on spin-dependent interactions up to masses of 200GeV/c2. Title: Search for anomalous production of multiple leptons in association with W and Z bosons at CDF Authors: Aaltonen, T.; Álvarez González, B.; Amerio, S.; Amidei, D.; Anastassov, A.; Annovi, A.; Antos, J.; Apollinari, G.; Appel, J. A.; Arisawa, T.; Artikov, A.; Asaadi, J.; Ashmanskas, W.; Auerbach, B.; Aurisano, A.; Azfar, F.; Badgett, W.; Bae, T.; Barbaro-Galtieri, A.; Barnes, V. E.; Barnett, B. A.; Barria, P.; Bartos, P.; Bauce, M.; Bedeschi, F.; Behari, S.; Bellettini, G.; Bellinger, J.; Benjamin, D.; Beretvas, A.; Bhatti, A.; Bisello, D.; Bizjak, I.; Bland, K. R.; Blumenfeld, B.; Bocci, A.; Bodek, A.; Bortoletto, D.; Boudreau, J.; Boveia, A.; Brigliadori, L.; Bromberg, C.; Brucken, E.; Budagov, J.; Budd, H. S.; Burkett, K.; Busetto, G.; Bussey, P.; Buzatu, A.; Calamba, A.; Calancha, C.; Camarda, S.; Campanelli, M.; Campbell, M.; Canelli, F.; Carls, B.; Carlsmith, D.; Carosi, R.; Carrillo, S.; Carron, S.; Casal, B.; Casarsa, M.; Castro, A.; Catastini, P.; Cauz, D.; Cavaliere, V.; Cavalli-Sforza, M.; Cerri, A.; Cerrito, L.; Chen, Y. C.; Chertok, M.; Chiarelli, G.; Chlachidze, G.; Chlebana, F.; Cho, K.; Chokheli, D.; Chung, W. H.; Chung, Y. S.; Ciocci, M. A.; Clark, A.; Clarke, C.; Compostella, G.; Convery, M. E.; Conway, J.; Corbo, M.; Cordelli, M.; Cox, C. A.; Cox, D. J.; Crescioli, F.; Cuevas, J.; Culbertson, R.; Dagenhart, D.; d'Ascenzo, N.; Datta, M.; de Barbaro, P.; Dell'Orso, M.; Demortier, L.; Deninno, M.; Devoto, F.; d'Errico, M.; Di Canto, A.; Di Ruzza, B.; Dittmann, J. R.; D'Onofrio, M.; Donati, S.; Dong, P.; Dorigo, M.; Dorigo, T.; Ebina, K.; Elagin, A.; Eppig, A.; Erbacher, R.; Errede, S.; Ershaidat, N.; Eusebi, R.; Farrington, S.; Feindt, M.; Fernandez, J. P.; Field, R.; Flanagan, G.; Forrest, R.; Frank, M. J.; Franklin, M.; Freeman, J. C.; Frisch, H.; Funakoshi, Y.; Furic, I.; Gallinaro, M.; Garcia, J. E.; Garfinkel, A. F.; Garosi, P.; Gerberich, H.; Gerchtein, E.; Giagu, S.; Giakoumopoulou, V.; Giannetti, P.; Gibson, K.; Ginsburg, C. M.; Giokaris, N.; Giromini, P.; Giurgiu, G.; Glagolev, V.; Glenzinski, D.; Gold, M.; Goldin, D.; Goldschmidt, N.; Golossanov, A.; Gomez, G.; Gomez-Ceballos, G.; Goncharov, M.; González, O.; Gorelov, I.; Goshaw, A. T.; Goulianos, K.; Grinstein, S.; Grosso-Pilcher, C.; Group, R. C.; Guimaraes da Costa, J.; Hahn, S. R.; Halkiadakis, E.; Hamaguchi, A.; Han, J. Y.; Happacher, F.; Hara, K.; Hare, D.; Hare, M.; Harr, R. F.; Hatakeyama, K.; Hays, C.; Heck, M.; Heinrich, J.; Herndon, M.; Hewamanage, S.; Hocker, A.; Hopkins, W.; Horn, D.; Hou, S.; Hughes, R. E.; Hurwitz, M.; Husemann, U.; Hussain, N.; Hussein, M.; Huston, J.; Introzzi, G.; Iori, M.; Ivanov, A.; James, E.; Jang, D.; Jayatilaka, B.; Jeon, E. J.; Jindariani, S.; Jones, M.; Joo, K. K.; Jun, S. Y.; Junk, T. R.; Kamon, T.; Karchin, P. E.; Kasmi, A.; Kato, Y.; Ketchum, W.; Keung, J.; Khotilovich, V.; Kilminster, B.; Kim, D. H.; Kim, H. S.; Kim, J. E.; Kim, M. J.; Kim, S. B.; Kim, S. H.; Kim, Y. K.; Kim, Y. J.; Kimura, N.; Kirby, M.; Klimenko, S.; Knoepfel, K.; Kondo, K.; Kong, D. J.; Konigsberg, J.; Kotwal, A. V.; Kreps, M.; Kroll, J.; Krop, D.; Kruse, M.; Krutelyov, V.; Kuhr, T.; Kurata, M.; Kwang, S.; Laasanen, A. T.; Lami, S.; Lammel, S.; Lancaster, M.; Lander, R. L.; Lannon, K.; Lath, A.; Latino, G.; LeCompte, T.; Lee, E.; Lee, H. S.; Lee, J. S.; Lee, S. W.; Leo, S.; Leone, S.; Lewis, J. D.; Limosani, A.; Lin, C. -J.; Lindgren, M.; Lipeles, E.; Lister, A.; Litvintsev, D. O.; Liu, C.; Liu, H.; Liu, Q.; Liu, T.; Lockwitz, S.; Loginov, A.; Lucchesi, D.; Lueck, J.; Lujan, P.; Lukens, P.; Lungu, G.; Lys, J.; Lysak, R.; Madrak, R.; Maeshima, K.; Maestro, P.; Malik, S.; Manca, G.; Manousakis-Katsikakis, A.; Margaroli, F.; Marino, C.; Martínez, M.; Mastrandrea, P.; Matera, K.; Mattson, M. E.; Mazzacane, A.; Mazzanti, P.; McFarland, K. S.; McIntyre, P.; McNulty, R.; Mehta, A.; Mehtala, P.; Mesropian, C.; Miao, T.; Mietlicki, D.; Mitra, A.; Miyake, H.; Moed, S.; Moggi, N.; Mondragon, M. N.; Moon, C. S.; Moore, R.; Morello, M. J.; Morlock, J.; Movilla Fernandez, P.; Mukherjee, A.; Muller, Th.; Murat, P.; Mussini, M.; Nachtman, J.; Nagai, Y.; Naganoma, J.; Nakano, I.; Napier, A.; Nett, J.; Neu, C.; Neubauer, M. S.; Nielsen, J.; Nodulman, L.; Noh, S. Y.; Norniella, O.; Oakes, L.; Oh, S. H.; Oh, Y. D.; Oksuzian, I.; Okusawa, T.; Orava, R.; Ortolan, L.; Pagan Griso, S.; Pagliarone, C.; Palencia, E.; Papadimitriou, V.; Paramonov, A. A.; Patrick, J.; Pauletta, G.; Paulini, M.; Paus, C.; Pellett, D. E.; Penzo, A.; Phillips, T. J.; Piacentino, G.; Pianori, E.; Pilot, J.; Pitts, K.; Plager, C.; Pondrom, L.; Poprocki, S.; Potamianos, K.; Prokoshin, F.; Pranko, A.; Ptohos, F.; Punzi, G.; Rahaman, A.; Ramakrishnan, V.; Ranjan, N.; Redondo, I.; Renton, P.; Rescigno, M.; Riddick, T.; Rimondi, F.; Ristori, L.; Robson, A.; Rodrigo, T.; Rodriguez, T.; Rogers, E.; Rolli, S.; Roser, R.; Ruffini, F.; Ruiz, A.; Russ, J.; Rusu, V.; Safonov, A.; Sakumoto, W. K.; Sakurai, Y.; Santi, L.; Sato, K.; Saveliev, V.; Savoy-Navarro, A.; Schlabach, P.; Schmidt, A.; Schmidt, E. E.; Schwarz, T.; Scodellaro, L.; Scribano, A.; Scuri, F.; Seidel, S.; Seiya, Y.; Semenov, A.; Sforza, F.; Shalhout, S. Z.; Shears, T.; Shepard, P. F.; Shimojima, M.; Shochet, M.; Shreyber-Tecker, I.; Simonenko, A.; Sinervo, P.; Sliwa, K.; Smith, J. R.; Snider, F. D.; Soha, A.; Sorin, V.; Song, H.; Squillacioti, P.; Stancari, M.; St. Denis, R.; Stelzer, B.; Stelzer-Chilton, O.; Stentz, D.; Strologas, J.; Strycker, G. L.; Sudo, Y.; Sukhanov, A.; Suslov, I.; Takemasa, K.; Takeuchi, Y.; Tang, J.; Tecchio, M.; Teng, P. K.; Thom, J.; Thome, J.; Thompson, G. A.; Thomson, E.; Toback, D.; Tokar, S.; Tollefson, K.; Tomura, T.; Tonelli, D.; Torre, S.; Torretta, D.; Totaro, P.; Trovato, M.; Ukegawa, F.; Uozumi, S.; Varganov, A.; Vázquez, F.; Velev, G.; Vellidis, C.; Vidal, M.; Vila, I.; Vilar, R.; Vizán, J.; Vogel, M.; Volpi, G.; Wagner, P.; Wagner, R. L.; Wakisaka, T.; Wallny, R.; Wang, S. M.; Warburton, A.; Waters, D.; Wester, W. C., III; Whiteson, D.; Wicklund, A. B.; Wicklund, E.; Wilbur, S.; Wick, F.; Williams, H. H.; Wilson, J. S.; Wilson, P.; Winer, B. L.; Wittich, P.; Wolbers, S.; Wolfe, H.; Wright, T.; Wu, X.; Wu, Z.; Yamamoto, K.; Yamato, D.; Yang, T.; Yang, U. K.; Yang, Y. C.; Yao, W. -M.; Yeh, G. P.; Yi, K.; Yoh, J.; Yorita, K.; Yoshida, T.; Yu, G. B.; Yu, I.; Yu, S. S.; Yun, J. C.; Zanetti, A.; Zeng, Y.; Zucchelli, S. Bibcode: 2012PhRvD..85i2001A Altcode: 2012arXiv1202.1260T This paper presents a search for anomalous production of multiple low-energy leptons in association with a W or Z boson using events collected at the CDF experiment corresponding to 5.1fb-1 of integrated luminosity. This search is sensitive to a wide range of topologies with low-momentum leptons, including those with the leptons near one another. The observed rates of production of additional electrons and muons are compared with the standard model predictions. No indications of phenomena beyond the standard model are found. A 95% confidence level limit is presented on the production cross section for a benchmark model of supersymmetric hidden-valley Higgs production. Particle identification efficiencies are also provided to enable the calculation of limits on additional models. Title: On the Relationship Between a High-frequency Type II Solar Radio Burst and Coronal Mass Ejection on February 13, 2011 Authors: Cho, Kyung-Suk; Gopalswamy, N.; Kwon, R.; Kim, R.; Yashiro, S. Bibcode: 2012AAS...22052502C Altcode: We examine the relationship between a metric type II radio burst that started from an unusually high frequency of 425 MHz (fundamental component) and the associated white-light coronal mass ejection on 2011 February 11. The radio burst had a drift rate of 3 MHz/sec, indicating a relatively high shock speed. The question we would like to answer is whether the high frequency type II burst is generated by the CME. To avoid the ambiguity normally caused by the use of density models in the analysis of type II bursts, we measure the coronal electron density by applying automated emission measure analysis code developed by Aschwanden et al. (2011) to AIA/SDO images in 6 coronal filters. From SDO AIA observations we find that a loop-like erupting front sweeps across high density coronal loops near the start time of the burst (17:34:15 UT). The deduced height of shock formation (1.2 Rs) from the measured density is comparable to the height (1.15 Rs) of the CME observed by STEREO/EUVI. Thus we conclude that the high frequency type II burst could be generated at locations where the CME passes through the high density loops in the low corona. Title: Propagation Characteristics of CMEs Associated Magnetic Clouds and Ejecta Authors: Kim, Roksoon; Gopalswamy, N.; Cho, K.; Moon, Y.; Yashiro, S. Bibcode: 2012AAS...22052108K Altcode: We have investigated the characteristics of magnetic cloud (MC) and ejecta (EJ) associated coronal mass ejections (CMEs) based on the assumption that all CMEs have a flux rope structure. For this, we used 54 CMEs and their interplanetary counter parts (interplanetary CMEs: ICMEs) that constitute the list of events used by the NASA/LWS Coordinated Data Analysis Workshop (CDAW) on CME flux ropes. We considered the location, angular width, speed, and direction parameter, D, that quantifies the propagation direction of a CME. For the 54 CDAW events, we found several properties of the CMEs as follows: (1) the average value of D for the 23 MCs (0.62) is larger than that for the 31 EJs (0.49), which indicates that the MC-associated CMEs propagate more directly to the Earth than the EJ-associated CMEs; (2) comparison between the direction parameter and the source location shows that the majority of the MC-associated CMEs are ejected along the radial direction, while many of the EJ-associated CMEs are ejected non-radially; (3) the mean speed of MC-associated CMEs (946 km/s) is faster than that of EJ-associated CMEs (771 km/s). For seven very fast CMEs (> 1500 km/s), all CMEs with large D (> 0.4) are associated with MCs and the CMEs with small D are associated with EJs. On the basis of these results, we suggest that the CME trajectory essentially decides the observed ICME structure. Title: Comparison of the bubble and blob distributions during the solar minimum Authors: Choi, H. -S.; Kil, H.; Kwak, Y. -S.; Park, Y. -D.; Cho, K. -S. Bibcode: 2012JGRA..117.4314C Altcode: 2012JGRA..11704314C Plasma blobs, local plasma density enhancements with respect to the background, in low to middle latitudes are understood as byproducts of equatorial plasma bubbles, but this hypothesis is challenged by observations of blobs in the absence of equatorial bubbles in the same magnetic meridian. This study investigates the causal linkage between bubbles and blobs using their occurrence statistics during the solar minimum. The bubble and blob distributions were obtained by analyzing the ion density data acquired during the period August 2008-April 2010 by the Coupled Ion-Neutral Dynamics Investigation instrument on board the Communication/Navigation Outage Forecasting System satellite. The seasonal, longitudinal, and latitudinal distributions of bubbles during the solar minimum are similar to those during other periods of the solar cycle. The distinctive bubble distribution during the solar minimum is the high occurrence rate of bubbles after midnight. The blob distribution shows the peak occurrence rate near midnight in the altitude range 400-450 km and around ±25° magnetic latitudes. The bubble occurrence rate is minimal during the June solstice, but the blob occurrence rate is maximal during that season. The blob occurrence rate has a peak value at about a 1700 km magnetic apex height, where the bubble occurrence rate is negligibly small. The difference in the bubble and blob distributions and the frequent occurrence of blobs beyond the bubble apex height suggest that bubbles are not a prerequisite for the creation of blobs. Title: Magnetic Field Strength in the Upper Solar Corona Using White-light Shock Structures Surrounding Coronal Mass Ejections Authors: Kim, R. -S.; Gopalswamy, N.; Moon, Y. -J.; Cho, K. -S.; Yashiro, S. Bibcode: 2012ApJ...746..118K Altcode: 2011arXiv1112.0288K To measure the magnetic field strength in the solar corona, we examined 10 fast (>=1000 km s-1) limb coronal mass ejections(CMEs) that show clear shock structures in Solar and Heliospheric Observatory/Large Angle and Spectrometric Coronagraph images. By applying the piston-shock relationship to the observed CME's standoff distance and electron density compression ratio, we estimated the Mach number, Alfvén speed, and magnetic field strength in the height range 3-15 solar radii (Rs ). The main results from this study are as follows: (1) the standoff distance observed in the solar corona is consistent with those from a magnetohydrodynamic model and near-Earth observations; (2) the Mach number as a shock strength is in the range 1.49-3.43 from the standoff distance ratio, but when we use the density compression ratio, the Mach number is in the range 1.47-1.90, implying that the measured density compression ratio is likely to be underestimated owing to observational limits; (3) the Alfvén speed ranges from 259 to 982 km s-1 and the magnetic field strength is in the range 6-105 mG when the standoff distance is used; (4) if we multiply the density compression ratio by a factor of two, the Alfvén speeds and the magnetic field strengths are consistent in both methods; and (5) the magnetic field strengths derived from the shock parameters are similar to those of empirical models and previous estimates. Title: Initiation of Coronal Mass Ejection and Associated Flare Caused by Helical Kink Instability Observed by SDO/AIA Authors: Kumar, Pankaj; Cho, K. -S.; Bong, S. -C.; Park, Sung-Hong; Kim, Y. H. Bibcode: 2012ApJ...746...67K Altcode: 2011arXiv1111.4360K In this paper, we present multiwavelength observations of helical kink instability as a trigger of a coronal mass ejection (CME) which occurred in active region NOAA 11163 on 2011 February 24. The CME was associated with an M3.5 limb flare. High-resolution observations from the Solar Dynamics Observatory/Atmospheric Imaging Assembly suggest the development of helical kink instability in the erupting prominence, which implies a flux rope structure of the magnetic field. A brightening starts below the apex of the prominence with its slow rising motion (~100 km s-1) during the activation phase. A bright structure, indicative of a helix with ~3-4 turns, was transiently formed at this position. The corresponding twist of ~6π-8π is sufficient to generate the helical kink instability in a flux rope according to recently developed models. A slowly rising blob structure was subsequently formed at the apex of the prominence, and a flaring loop was observed near the footpoints. Within 2 minutes, a second blob was formed in the northern prominence leg. The second blob erupts (like a plasmoid ejection) with the detachment of the northern prominence leg, and flare intensity maximizes. The first blob at the prominence apex shows rotational motion in the counterclockwise direction in the plane of sky, interpreted as the unwinding motion of a helix, and it also erupts to give the CME. RHESSI hard X-ray (HXR) sources show the two footpoint sources and a loop-top source during the flare. We found RHESSI HXR flux, soft X-ray flux derivative, and CME acceleration in the low corona correlate well, which is in agreement with the standard flare model (CSHKP). We also discuss the possible role of ballooning as well as torus instabilities in driving the CME. We conclude that the CME and flare were triggered by the helical kink instability in a flux rope and accelerated mainly by the torus instability. Title: Geometry of the 20 November 2003 magnetic cloud Authors: Marubashi, Katsuhide; Cho, Kyung-Suk; Kim, Yeon-Han; Park, Yong-Deuk; Park, Sung-Hong Bibcode: 2012JGRA..117.1101M Altcode: 2012JGRA..11701101M This study is an attempt to find a coherent interpretation of the link between the 20 November 2003 magnetic cloud (MC) and its solar source. Most previous studies agree on the orientation of the MC, but the orientation is nearly perpendicular to the axis of the post-eruption arcade (PEA) or the orientation of the neutral line in the solar source region. We first determine the geometry of this MC by fitting methods with both torus and cylinder models. Three possible geometries are obtained, which can reproduce the observed magnetic field variations associated with the MC, one from the cylinder fit and two from the torus fit. The cylinder fit gives the MC orientation with a tilt of a large angle (∼60°) from the ecliptic plane and nearly perpendicular to the PEA axis, being similar to those from previous studies. In contrast, two torus fit results give the MC axis with tilt angles less than 20° from the ecliptic plane. The two torus results correspond to the spacecraft encounter with the eastern flank of the flux rope loop (model A) and the western flank of the loop (model B), respectively. In either case, the orientation of the loop around the apex is nearly parallel to the PEA as observed by the SOHO/extreme ultraviolet imaging telescope instrument in the most plausible solar source region of a halo coronal mass ejection (CME), which appeared in the field of view of Large Angle and Spectrometric Coronagraph (LASCO) C2 at 08:50 UT, 18 November 2003. The magnetic helicity of the PEA region is positive in agreement with the helicity of the MC. The 3-D reconstruction from the Solar Mass Ejection Imager data shows that the main part of the ejected plasma expands mainly to the west of the Sun-Earth line. Thus, we reach the most straightforward interpretation of the link between the MC and its solar source as follows. The MC was created in association with the launch of the CME that was first observed by the LASCO C2 at 08:50 UT, 18 November 2003, and propagated through interplanetary space with its orientation almost unchanged. The spacecraft encountered the eastern flank of the loop as described by model A. Title: Comparison of helicity signs in magnetic clouds and their solar source regions Authors: Cho, K.; Park, S.; Marubashi, K.; Bong, S.; Kim, R. Bibcode: 2011AGUFMSH51A1993C Altcode: Magnetic helicity, which is known as one of the few quantities that are conserved, quantifies the signed amount of twists, kinks, and inter-linkages of the magnetic field lines in a given magnetic field system. CMEs are one of the means by which the Sun ejects magnetic helicity into interplanetary space, and magnetic clouds (MCs) detected near the Earth may carry a similar amount of helicity ejected from solar source regions. If the helicity ejected by solar eruptions is conserved from the Sun to the Earth, we can assume that flux ropes in MCs should have similar characteristics with those in their solar source regions, and it is also expected that the signs of their helicties on the Sun and near the Earth should be same. With this expectation, we selected 36 CMEs that occurred at solar disk center among well identified 59 CME-MC pairs in the CDAW list, and determined the helicity signs in magnetic clouds and their solar source regions, respectively. The helicity signs in the solar source regions are determined by the amount of helicity injection through their photospheric surfaces using SOHO/MDI magnetograms, and the helicity signs in the MCs are estimated by adopting cylinder and torus models to ACE solar wind data. As a results, we found that among the total of 36 events, there are 30 helicity sign-consistent events (83%) and 6 sign-inconsistent events (17%). This result shows that most flux ropes erupted from the surface maintain their helicity signs from the Sun to the Earth, and supports that flux ropes in the MCs have a similar characteristic with those in their solar source regions. For 6 exceptional events, we investigate them in detail if they do not follow the helicity conservation rule or if they are come from the followings: (1) the helicity sign difference between the entire source active region and the local CME-originated region, (2) the wrong estimation of MC helicity signs by the fitting models, or (3) the uncertainty of helicity sign determination in the source region due to pre-existing opposite-sign helicity in a coronal volume of the source region. In this talk, we will show that our results support the idea of the helicity conservation rule of CDAW CME-MC pairs. Title: Pre-flare Activity and Magnetic Reconnection during the Evolutionary Stages of Energy Release in a Solar Eruptive Flare Authors: Joshi, Bhuwan; Veronig, Astrid M.; Lee, Jeongwoo; Bong, Su-Chan; Tiwari, Sanjiv Kumar; Cho, Kyung-Suk Bibcode: 2011ApJ...743..195J Altcode: 2011arXiv1109.3415J In this paper, we present a multi-wavelength analysis of an eruptive white-light M3.2 flare that occurred in active region NOAA 10486 on 2003 November 1. The excellent set of high-resolution observations made by RHESSI and the TRACE provides clear evidence of significant pre-flare activities for ~9 minutes in the form of an initiation phase observed at EUV/UV wavelengths followed by an X-ray precursor phase. During the initiation phase, we observed localized brightenings in the highly sheared core region close to the filament and interactions among short EUV loops overlying the filament, which led to the opening of magnetic field lines. The X-ray precursor phase is manifested in RHESSI measurements below ~30 keV and coincided with the beginning of flux emergence at the flaring location along with early signatures of the eruption. The RHESSI observations reveal that both plasma heating and electron acceleration occurred during the precursor phase. The main flare is consistent with the standard flare model. However, after the impulsive phase, an intense hard X-ray (HXR) looptop source was observed without significant footpoint emission. More intriguingly, for a brief period, the looptop source exhibited strong HXR emission with energies up to ~50-100 keV and significant non-thermal characteristics. The present study indicates a causal relation between the activities in the pre-flare and the main flare. We also conclude that pre-flare activities, occurring in the form of subtle magnetic reorganization along with localized magnetic reconnection, played a crucial role in destabilizing the active region filament, leading to a solar eruptive flare and associated large-scale phenomena. Title: Magnetic field strength in the upper solar corona using white-light shock structures surrounding coronal mass ejections Authors: Kim, R.; Gopalswamy, N.; Moon, Y.; Cho, K.; Yashiro, S. Bibcode: 2011AGUFMSH43B1955K Altcode: To measure the magnetic field strength in the solar corona, we examined 12 fast (> 1000 km s-1) limb CMEs which show clear shock-like structures in SOHO/LASCO observations. By applying piston-shock relationship to the observed CME's standoff distance and electron density compression ratio, we estimated the Mach number, Alfven speed, and magnetic field strength in the height range 3 to 15 solar radii (Rs). We found: (1) the standoff distance observed in the solar corona is consistent with those from a magnetohydrodynamic (MHD) model and near-Earth observations; (2) the Mach number as a shock strength is in the range 1.49 to 3.52 from the standoff distance data, but when we use the compression ratio, the Mach number is in the range 1.47 to 1.90, implying that the measured density compression ratio is likely to be underestimated due to observational limit; (3) the Alfven speed ranges from 259 to 982 km s-1 and the magnetic field strength is in the range 6 to 120 mG when the standoff distance is used; (4) if we multiply the density compression ratio by a factor of 2, the Alfven speeds and the magnetic field strengths are consistent in both methods; (5) the magnetic field strengths derived from the shock parameters are similar to those of empirical models and previous estimates. This is a new attempt to measure magnetic field strength in the upper corona up to 15 Rs from coronagraph observations alone. Our observations support the idea that the diffuse structures surrounding the CME front can be interpreted as shock structures. Title: Dependence of GCRs influx on the solar North-South asymmetry Authors: Cho, Il-Hyun; Kwak, Young-Sil; Chang, Heon-Young; Cho, Kyung-Suk; Park, Young-Deuk; Choi, Ho-Sung Bibcode: 2011JASTP..73.1723C Altcode: 2011arXiv1103.4255C We investigate the dependence of the amount of the observed galactic cosmic ray (GCR) influx on the solar North-South asymmetry using the neutron count rates obtained from four stations and sunspot data in archives spanning five solar cycles from 1953 to 2008. We find that the observed GCR influxes at Moscow, Kiel, Climax and Huancayo stations are more suppressed when the solar activity in the southern hemisphere is dominant compared with when the solar activity in the northern hemisphere is dominant. Its reduction rates at four stations are all larger than those of the suppression due to other factors including the solar polarity effect on the GCR influx. We perform the student's t-test to see how significant these suppressions are. It is found that suppressions due to the solar North-South asymmetry as well as the solar polarity are significant and yet the suppressions associated with the former are larger and more significant. Title: Two Types of Extreme-ultraviolet Brightenings In AR 10926 Observed by Hinode/EIS Authors: Lee, K. -S.; Moon, Y. -J.; Kim, Sujin; Choe, G. S.; Cho, Kyung-Suk; Imada, S. Bibcode: 2011ApJ...736...15L Altcode: We have investigated seven extreme-ultraviolet (EUV) brightenings in the active region AR 10926 on 2006 December 2 observed by the EUV Imaging Spectrometer on board the Hinode spacecraft. We have determined their Doppler velocities and non-thermal velocities from 15 EUV spectral lines (log T = 4.7 - 6.4) by fitting each line profile to a Gaussian function. The Doppler velocity maps for different temperatures are presented to show the height dependence of the Doppler shifts. It is found that the active region brightenings show two distinct Doppler shift patterns. The type 1 brightening shows a systematic increase of Doppler velocity from -68 km s-1 (strong blueshift) at log T = 4.7 to -2 km s-1 (weak blueshift) at log T = 6.4, while the type 2 brightenings have Doppler velocities in the range from -20 km s-1 to 20 km s-1. The type 1 brightening point is considered to sit in an upward reconnection outflow whose speed decreases with height. In both types of brightenings, the non-thermal velocity is found to be significantly enhanced at log T = 5.8 compared to the background region. We have also determined electron densities from line ratios and derived temperatures from emission measure loci using the CHIANTI atomic database. The electron densities of all brightenings are comparable to typical values in active regions (log Ne = 9.9-10.4). The emission measure loci plots indicate that these brightenings should be multi-thermal whereas the background is isothermal. The differential emission measure as a function of temperature shows multiple peaks in the EUV brightening regions, while it has only a single peak (log T = 6.0) in the background region. Using Michelson Doppler Imager magnetograms, we have found that the type 1 brightening is associated with a canceling magnetic feature with a flux canceling rate of 2.4 × 1018 Mx hr-1. We also found the canceling magnetic feature and chromospheric brightenings in the type 1 brightening from the Hinode SOT and Transition Region and Coronal Explorer data. This observation corroborates our argument that brightening is caused by magnetic reconnection in a low atmosphere. Title: An Analytical Model for the Coronal Component of Major Solar Energetic Particle Events Authors: Kocharov, Leon; Cho, Kyung-Suk; Valtonen, Eino Bibcode: 2011ApJ...735....4K Altcode: We formulate an analytical model of the coronal-phase acceleration observed in the beginning of major solar energetic particle (SEP) events, before the main-phase acceleration associated with coronal mass ejections (CMEs) in solar wind. The model is driven and constrained by the broadband observations of SEPs and CMEs, in particular SEP data from the particle telescope of the Energetic and Relativistic Nuclei and Electron (ERNE) experiment on the Solar and Heliospheric Observatory (SOHO) spacecraft, solar radio spectrograms, and low-corona observations of CMEs. The model is also verified against observations of solar high-energy neutrons and neutron-decay protons. The model suggests SEP acceleration above ~ 50 MeV nucleon-1 by coronal shock and the shock-amplified turbulence in closed magnetic structures, and particle release at magnetic reconnection between the closed structure of expanding CME and pre-existing open magnetic flux tubes. The analytical model connects parameters of coronal shocks and structures and the SEP parameters in space, which facilitates analysis of multiwavelength data and will assist in further development of coronal acceleration models. Title: Relationship between multiple type II solar radio bursts and CME observed by STEREO/SECCHI Authors: Cho, K. -S.; Bong, S. -C.; Moon, Y. -J.; Shanmugaraju, A.; Kwon, R. -Y.; Park, Y. D. Bibcode: 2011A&A...530A..16C Altcode: