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SH1 and SH2.1 (Sun & Corona, IP Transport)

SH1 and SH2.1 (Sun & Corona, IP Transport). C. M. S. Cohen ( Caltech ). 93 papers total. Topics. (12 papers). First Results from RHESSI (really!) The devil is in the details - new puzzles Some topics never die Particle Acceleration Particle Transport

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SH1 and SH2.1 (Sun & Corona, IP Transport)

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  1. SH1 and SH2.1(Sun & Corona, IP Transport) C. M. S. Cohen (Caltech)

  2. 93 papers total Topics (12 papers) • First Results from RHESSI (really!) • The devil is in the details - new puzzles • Some topics never die • Particle Acceleration • Particle Transport • TGFM (Thank goodness for modellers) • Future prospects (38 papers) (8 papers) (21 papers) (14 papers)

  3. What do we want to know about solar energetic particles? • Where they are accelerated • What is being accelerated • How they are accelerated • How they reach us Tools • Particles • Onsets, Composition, Charge States • Photons • Images/Movies, Wavelengths, Spectra

  4. Particle Measurements • Spacecraft • IMP8, Wind, SOHO, ACE, Cassini, GOES, NOZOMI, SAMPEX, MITA • Neutron Monitors/SNT • Tibet, Mt. Chacaltaya, Mt. Haleakala, Mt. Norikura, Spaceship Earth, ... • Muon Telescopes • L3+C, GRAPES, GRAND, BUST, Andyrchy, Carpet

  5. NM MT Particle Measurements • Bastille (7/14/00) event • Easter/Resurrection (4/15/01) event

  6. Two Main Acceleration Processes Flare-related Fe/O ~ 1 3He/4He ~ 0.1 - 1 QFe ~ 20 CME-driven Shock Fe/O ~ 0.1 3He/4He <0.01 QFe ~ 10-14

  7. Tylka et al. Bieber et al. (Harley) Mewaldt et al. Where? Different methods agree rather well • Timing Studies • T vs c/v (Mewaldt et al., Tylka et al.) • injection/transport models with NM data (Bieber et al.) • NM & electron velocity (Kahler et al.)

  8. 2-10 RS Flare Mewaldt et al. Shock Where? • Most big events point to CME-shock accel. • After CME lift off • After type III radio • After HXR emission • Association with DH & metric type II radio (Cliver et al.) Tylka et al.

  9. Where? Mewaldt et al. Scattering / Pitch angle distributions • Injection/Release - all species/energies together? • Tylka et al., Posner & Kunow - yes • Kahler et al. - no (H+ before e-) • Mewaldt et al. - sometimes (heavies after e-)

  10. Where? • RHESSI protons and electron acceleration locations are different (Hurford et al.) • Size of HXR region and pre-eruption motion related to SEP characteristics (Nitta et al.) Hurford et al. Nitta et al.

  11. What? • Reames 1995 • CME-shocks accelerate Solar Wind • Desai et al. 2003 • composition at shocks (1 AU) is not solar wind-like • composition most like upstream material Upstream material = mix of flare and solar wind-like (on average 30% & 70%)

  12. Laivola et al. What? • Flare Material (remnant? concurrent?) • 3He/4He in SEPs larger than solar wind values (Laivola et al.)

  13. Labrador et al. Solar Wind Tylka et al. What? • Flare Material (remnant? concurrent?) • 3He/4He in SEPs larger than solar wind values (Laivola et al.) • QFe correlates with Fe/O in SEPs (Labrador et al., Tylka et al.)

  14. Möbius et al. Flare-related ? 00/159 Suprthermal material may have solar wind-like Qs 00/096 Popecki et al. What? • Flare Material (remnant? concurrent?) • 3He/4He in SEPs larger than solar wind values (Laivola et al.) • QFe correlates with Fe/O in SEPs (Labrador et al., Tylka et al.) • QFe distributions can have high-Q tail (Popecki et al.) • But... • Maybe not enough material (Mewaldt et al.) • Shock events have Qs like solar wind (Klecker et al.)

  15. Tanuma & Shibata Naito Kota et al. How? • Modelling flares • Shocks in reconnection jet (Tanuma & Shibata) • Shocks in flares and orientation (Naito) • Shocks in giant arcades (Shiota et al.) • Modelling CME shocks (Kota et al.)

  16. 4/15/01 Bieber et al. 7/14/00 Duldig et al. 7/14/00 Delayed - soft, broad Vashenyuk et al. How? • Extended Injection • NM (Bieber et al., Duldig et al.) • >100 MeV H+ (Struminsky et al.) • Transport or acceleration? • Delay is getting to connected field line • 2 acceleration mechanisms (Vashenyuk et al.) Prompt - hard, narrow

  17. Mazur et al. 2000 McKibben et al. 2001 Zhang et al. Chuychai et al. 40-90 MeV H+ Transport • Field line connection (Chuychai et al.) • Particle diffusion (Zhang et al.) Significant cross field diffusion

  18. Casolino et al. Sako et al. Energy (MeV) SELENE/PS Takashima et al. The Future • New SNT • Mt. Sierra Negra - 19N (Valdes-Galicia et al.) • Super SNT (Sako et al.) • Improvements • Mt. Aragats (Muraki et al.), ADAMO (Bonechi et al.) • Mobile NM (Moraal et al.), RECORD (Ksenotontov et al.) • Spacecraft Instruments • ResursDK1/PAMELA - 2005 (Casolino et al.) • SELENE/PS - 2004 (Takashima et al.) 3-400 MeV/n Heavies

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