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Co-leaders: Nariaki Nitta & Sophie Masson

What do we learn from observations and modeling of the solar corona for understanding solar energetic particle events?. Co-leaders: Nariaki Nitta & Sophie Masson. Motivations:

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Co-leaders: Nariaki Nitta & Sophie Masson

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  1. What do we learn from observations and modeling of the solar corona for understanding solar energetic particle events? Co-leaders: Nariaki Nitta & Sophie Masson Motivations: Connect SEP observations (occurrences, properties, etc.) with solar eruptions as captured by new instruments and theories/simulations. New SEP data, especially from widely separate locations, solar data of unprecedented volume and quality/potential (cadence, stereoscopic view, etc.), and realistic simulations.

  2. Invited Speakers Glenn Mason: What are the solar source regions of energetic 3He-rich SEPs? ViacheslavTitov: Which magnetic topologies are favorable for an efficient acceleration and escape of SEPs? Some keywords: MHD simulation, Standard model of eruptive flares, SDO, STEREO, AIA, HMI, EVE, SECCHI, EUVI, COR-1/2, HI-1/2, CME, flare, eruption, jet, shock wave, blast wave, MHD wave, EIT (EUV) wave, Moreton(-Ramsey) wave, type II/III burst, polarity inversion line, separatrix, separator, null points, reconnection, arcade, cusp, open field region, streamer, pseudo-streamer, PFSS, magnetic field connection, Parker spiral, magnetic field meandering, cross field diffusion, GLE, proton event, gradual SEP event, 3He-rich SEP event, CIR, preconditioning, seed particle, etc.

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