Evidence for the Magnetic Trapping of Solar-Flare Ions from 1-8-MeV Solar Neutrons Detected with the MESSENGER Neutron Spectrometer

Details Evidence for the Magnetic Trapping of Solar-Flare Ions from 1-8-MeV Solar Neutrons Detected with the MESSENGER Neutron Spectrometer Evidence for the Magnetic Trapping of Solar-Flare Ions from 1-8-MeV Solar Neutrons Detected with the MESSENGER Neutron Spectrometer

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufm.u12a..02f&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #U12A-02

Physics

7509 Corona, 7514 Energetic Particles (2114), 7519 Flares, 7534 Radio Emissions, 7900 Space Weather

Scientific paper

Neutrons produced on the Sun during the M2 flare on 31 December 2007 were observed throughout an approximately 10-hour period at 0.48 AU by the MESSENGER Neutron Spectrometer. This flare contained multiple acceleration episodes as seen in Type III radio bursts and fine structure in the energetic-particle environment at MESSENGER. After these bursts ended, both the energetic-particle and neutron fluxes decayed smoothly to background with an e-folding decay time of 2.84 hours. The fact that this time is considerably longer than the mean life of a neutron (886 s) indicates that neutrons at the Sun must have been continuously produced. A likely explanation is that a considerable fraction of the energetic ions accelerated during the flare remained trapped on closed magnetic arcades high in the corona and were slowly pitch-angle scattered by coronal turbulence into their chromospheric loss cones. Subsequent interactions with chromospheric ions generated neutrons that scatter to form a population of upward-going albedo neutrons.

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