Japan Geoscience Union Meeting 2019

Presentation information

[J] Oral

P (Space and Planetary Sciences ) » P-EM Solar-Terrestrial Sciences, Space Electromagnetism & Space Environment

[P-EM19] Frontiers in the solar physics

Sun. May 26, 2019 3:30 PM - 5:00 PM A03 (TOKYO BAY MAKUHARI HALL)

convener:Shinsuke Imada(Institute for Space-Earth Environmental Research, Nagoya University), Takaaki Yokoyama(School of Science, University of Tokyo), Toshifumi Shimizu(Institute of Space and Astronautical Science, JAXA), Yukio Katsukawa(National Astronomical Observatory of Japan, National Institute of Natural Sciences), Chairperson:Shinsuke Imada

4:45 PM - 5:00 PM

[PEM19-06] Detection and energy derivation of nano-flares based on deep learning

*Toshiki Kawai1, Shinsuke Imada1 (1.Institute for Space-Earth Environmental Research, Nagoya University)

Keywords:deep learning, nano-flare

Coronal heating is one of the long-standing problems in solar physics. So far, two primary mechanisms have been proposed to explain how the corona is heated, namely small-scale magnetic reconnection and wave dissipation. To estimate the contribution of small-scale magnetic reconnection, so called nano-flares, to heat the corona is crucial to solve the coronal heating problem. The purpose of this study is to develop a method which can accurately detect nano-flares and estimate their energies. Firstly, we carry out one-dimensional hydrodynamic simulations of coronal loops heated by nano-flares which have wide range of energy (1023 < E < 1027 erg). Secondly, we calculate the temporal variation of EUV and soft X-ray spectra of coronal loops from the simulation results by using CHIANTI atomic database. We perform these procedures more than 1,000 times with randomized flare energy and occurrence time to produce various datasets. Finally, we train a Deep Neural Network (DNN) by using these datasets to estimate the energy distribution and occurrence times of flares from soft X-ray observation. Moreover, we apply trained DNN to actual soft X-ray observations. As a result, we obtain reasonable occurrence times and energies of flares comparing another method which regards flare energy as change amount of thermal energy of the loop.