Estimates of the neutron emission during large solar flares in the rising and maximum period of solar cycle 24 |
| |
| Institution: | 1. Solar-Terrestrial Environment Laboratory, Nagoya University, 1 Furo-cho, Chikusa-ku, Nagoya 464-8601, Japan;2. Instituto de Geofísica, Universidad Nacional Autónoma de México, 04510 México, D.F., Mexico;1. KTH Royal Institute of Technology, Department of Physics, 106 91 Stockholm, Sweden;2. The Oskar Klein Centre for Cosmoparticle Physics, AlbaNova University Centre, 106 91 Stockholm, Sweden;3. Hiroshima University, Department of Physical Science, Hiroshima 739-8526, Japan;4. Max-Planck-Institut für Physik, D-80805 München, Germany;1. Institute of Nuclear Physics PAN, Kraków, Poland;2. Institute for Nuclear Physics (IKP), Karlsruhe Institute of Technology, Karlsruhe, Germany;3. Argelander Institute for Astronomy (AIfA), Bonn, Germany;1. Gran Sasso Science Institute, viale Francesco Crispi, 7 L’Aquila 67100 (AQ), Italy;2. Institute for Space Sciences (CSIC/IEEC), Barcelona E-08193, Spain;3. Dublin Institute of Advanced Studies, 10 Burlington Road, Dublin 4, Ireland;4. Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, Heidelberg D-69117, Germany;1. Instituto de Ciência e Tecnologia, Universidade Federal de Alfenas, Rodovia José Aurélio Vilela, 11999, Cidade Universitária, CEP 37715-400, Poços de Caldas, MG, Brazil;2. Escola de Ciência e Tecnologia, Universidade Federal do Rio Grande do Norte, Campus Universitário, s/n, CEP 59072-970, Natal, Brazil;1. Center for Underground Physics, Institute for Basic science (IBS), Daejeon 305-811, Republic of Korea;2. Department of Physics, Sejong University, Seoul 143-747, Republic of Korea |
| |
| Abstract: | We searched for solar neutrons using the data collected by six detectors from the International Network of Solar Neutron Telescopes and one Neutron Monitor between January 2010 and December 2014. We considered the peak time of the X-ray intensity of thirty five ≥ X1.0 class flares detected by GOES satellite as the most probable production time of solar neutrons. We prepared a light-curve of the solar neutron telescopes and the neutron monitor for each flare, spanning ± 3 h from the peak time of GOES. Based on these light curves, we performed a statistical analysis for each flare. Setting a significance level at greater than 3σ, we report that no statistically significant signals due to solar neutrons were found. Therefore, upper limits are determined by the background level and solar angle of these thirty five solar flares. Our calculation assumed a power-law neutron energy spectrum and an impulsive emission profile at the Sun. The estimated upper limits of the neutron emission are consistent within the order of magnitude of the successful detections of solar neutrons made in solar cycle 23. |
| |
| Keywords: | |
| 本文献已被 ScienceDirect 等数据库收录！ |
|
