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Working Group 3:  -rays and ions

Working Group 3:  -rays and ions. Albert Shih Alec MacKinnon Neus Agueda Michael Briggs Wei Chen Hugh Hudson Bob Lin Procheta Mallik Ron Murphy Richard Schwartz Gerry Share David Smith Kim Tolbert Tom Vestrand Nicole Vilmer … plus WG 2 and WG 6. Discussion topics.

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Working Group 3:  -rays and ions

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  1. Working Group 3: -rays and ions Albert Shih Alec MacKinnon NeusAgueda Michael Briggs Wei Chen Hugh Hudson Bob Lin ProchetaMallik Ron Murphy Richard Schwartz Gerry Share David Smith Kim Tolbert Tom Vestrand Nicole Vilmer … plus WG 2 and WG 6

  2. Discussion topics • Improved gamma-ray code and improved responses for better fits • Accelerated and ambient abundances • Searching for low-energy neutrons • Energetic neutral atoms (ENAs), observed and predicted • Fermi/GBM observations Annihilation escape Compton scatter Annihilation capture

  3. ENA observation (Mewaldt et al. 2009) • The STEREO observations provide both spatial and temporal signatures that clearly identify the particles as hydrogen • The injection times closely match the GOES light curve of the flare

  4. Predicted ENAs from a shock

  5. Versus >300 keV electrons • Direct proportionality • Dotted lines are factors of 2 from the best-fit line • Some spread is due to incomplete coverage (triangles) • Almost all flares fall within 1 σ of spread • Magenta diamond is the 2010 Jun 12 flare (Shih et al. 2009, ApJL)

  6. 06:45:40 to 06:48:00 UT. Best fitting model (solid black curve); low-energy brems. (solid yellow), high-energy brems. (solid orange), nuclear line and cont. (solid blue), pion-decay (solid purple), 2223 MeV (dotted purple), solar 511 keV (dashed purple), solar-scattered N-capture (solid light green), He line (dashed light blue).

  7. 2005 January 20 Time Histories of Different Flare Components. Inferred ion and electron spectra show variability.

  8. First gamma-ray flare of Cycle 24. Fits to the Fermi/GBM/BGO (left) and RHESSI (right). RHESSI spectral response degraded due to radiation damage.

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