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Response of chromospheric lines to different periodic non-thermal electron beams

Published online by Cambridge University Press:  09 September 2016

Jianxia Cheng  and
Mingde Ding
Jianxia Cheng
Affiliation:
Key Laboratory of Planetary Sciences, Shanghai Astronomical Observatory, Shanghai 200030, China email: chengjx@shao.ac.cn Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China
Mingde Ding
Affiliation:
School of Astronomy & Space Science, Nanjing University, Nanjing 210093, China email: dmd@nju.edu.cn
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Abstract

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Solar flares produce radiations in very broad wavelengths. Spectra can supply us abundant information about the local plasma, such as temperature, density, mass motion and so on. Strong chromospheric lines, like the most studied Hα and Ca II 8542 Å lines are formed under conditions of departures from local thermodynamic equilibrium in the lower atmosphere subject to flare heating. Understanding how these lines are formed is very useful for us to correctly interpret the observations. In this paper, we try to figure out the response of chromospheric lines heated by different periodic non-thermal electron beams. Our results are based on radiative hydrodynamic simulations. We vary the periods of electron beam injection from 1.25 s to 20 s. We compare the response times to different heating parameters. Possible explanations are discussed.

Keywords

solar flareradiative transfernumerical simulation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Symposium S320: Solar and Stellar Flares and their Effects on Planets , August 2015 , pp. 239 - 242
Copyright
Copyright © International Astronomical Union 2016 

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