Gamma Rays and Energetic Neutral Atoms from Solar Flares

Details Gamma Rays and Energetic Neutral Atoms from Solar Flares Gamma Rays and Energetic Neutral Atoms from Solar Flares

May 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009spd....40.3604h&link_type=abstract

American Astronomical Society, SPD meeting #40, #36.04; Bulletin of the American Astronomical Society, Vol. 41, p.868

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The recent discovery of energetic (1.6-5.0 MeV) neutral hydrogen atoms (ENAs) from an X9 solar flare on 2006 Dec. 5 (Mewaldt et al. 2009) raises the exciting possibility that they could represent a lower-energy range of the same population of accelerated ions responsible for flare gamma-ray emission. If so the neutralization would take place at low altitudes in the flaring loop, and the neutral atoms might need to escape through multiple epochs of re-ionization and neutralization. The probability for eventual escape is high because of the large mirror ratios of the coronal fields and because of small energy losses of the ENAs and the ions they become. Using a standard density model, we have shown that the collisional lifetime of re-ionized particles exceeds the observed injection time. We use Monte Carlo simulations of particle trajectories, including both neutral and ionized states, to estimate escape probabilities and directivity more generally within the context of a standard PFSS (potential-field source surface) model for the field above the Mewaldt et al. flare, and compare the results with RHESSI gamma-ray observations of this flare.

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