RE-EVALUATION OF THE NEUTRON EMISSION FROM THE SOLAR FLARE OF 2005 SEPTEMBER 7, DETECTED BY THE SOLAR NEUTRON TELESCOPE AT SIERRA NEGRA

ABSTRACT The X17.0 solar flare of 2005 September 7 released high-energy neutrons that were detected by the Solar Neutron Telescope (SNT) at Sierra Negra, Mexico. In three separate and independent studies of this solar neutron event, several of its unique characteristics were studied; in particular,...

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Bibliographic Details
Published in:The Astrophysical journal 2015-12, Vol.814 (2), p.1-7
Main Authors: González, L. X., Valdés-Galicia, J. F., Sánchez, F., Muraki, Y., Sako, T., Watanabe, K., Matsubara, Y., Nagai, Y., Shibata, S., Sakai, T., Musalem, O., Hurtado, A.
Format: Article
Language:English
Subjects:
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
COMPUTERIZED SIMULATION
Deposition
ENERGY ABSORPTION
ENERGY LOSSES
ENERGY SPECTRA
Flares
GEV RANGE
Mathematical analysis
Mathematical models
methods: numerical
NEUTRON EMISSION
NEUTRON FLUX
SOLAR FLARES
SOLAR NEUTRONS
SOLAR PROTONS
Space telescopes
Spectra
SUN
Sun: flares
Sun: particle emission
TELESCOPES
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Summary:ABSTRACT The X17.0 solar flare of 2005 September 7 released high-energy neutrons that were detected by the Solar Neutron Telescope (SNT) at Sierra Negra, Mexico. In three separate and independent studies of this solar neutron event, several of its unique characteristics were studied; in particular, a power-law energy spectra was estimated. In this paper, we present an alternative analysis, based on improved numerical simulations of the detector using GEANT4, and a different technique for processing the SNT data. The results indicate that the spectral index that best fits the neutron flux is around 3, in agreement with previous works. Based on the numerically calculated neutron energy deposition on the SNT, we confirm that the detected neutrons might have reached an energy of 1 GeV, which implies that 10 GeV protons were probably produced; these could not be observed at Earth, as their parent flare was an east limb event.
ISSN:0004-637X
1538-4357
1538-4357
DOI:10.1088/0004-637X/814/2/136