Solar neutron emission and propagation mechanisms for 2003 October 28 event

Details Solar neutron emission and propagation mechanisms for 2003 October 28 event Solar neutron emission and propagation mechanisms for 2003 October 28 event

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufmsh43b1511w&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #SH43B-1511

Astronomy and Astrophysics

Astrophysics

7500 Solar Physics, Astrophysics, And Astronomy, 7514 Energetic Particles (2114), 7519 Flares, 7554 X-Rays, Gamma Rays, And Neutrinos

Scientific paper

Ions accelerated in solar flares interact with the solar atmosphere to produce gamma-ray lines and neutrons. Some of the neutrons that escape from the Sun into interplanetary space can survive to the Earth and be observed both by satellite detectors and by ground-based neutron monitors. Observations of such solar neutrons provide information about the ion acceleration mechanism in solar flares and propagation of the neutrons. Solar neutrons were observed by the Tsumeb neutron monitor on the ground from the solar flare on 2003 October 28. Gamma-ray lines at 2.2, 4.4, and 6.1 MeV were also observed by the INTEGRAL and RHESSI satellites. Using these gamma-ray line emissions, we calculate predicted time-dependent neutron spectra arriving at Earth using the solar flare magnetic loop transport and interaction model of Hua et al. (2002). These spectra are then convolved with the response functions of the Earth's atmosphere and the neutron monitor to provide predicted neutron monitor count rates. We compare these predicted rates with the observed rates and search for the best model to explain data.

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