Working group 3 rays and ions
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Working Group 3:  -rays and ions PowerPoint PPT Presentation


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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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Working group 3 rays and ions

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


Discussion topics

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


Ena observation mewaldt et al 2009

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


Predicted enas from a shock

Predicted ENAs from a shock


Versus 300 kev electrons

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)


Working group 3 rays and ions

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).


Working group 3 rays and ions

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


Working group 3 rays and ions

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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