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Title: Solar Flare Termination Shock and Synthetic Emission Line Profiles of the Fe xxi 1354.08 Å Line

Abstract

Solar flares are among the most energetic phenomena that occur in the solar system. In the standard solar flare model, a fast mode shock, often referred to as the flare termination shock (TS), can exist above the loop-top source of hard X-ray emissions. The existence of the TS has been recently related to spectral hardening of a flare’s hard X-ray spectra at energies >300 keV. Observations of the Fe xxi 1354.08 Å line during solar flares by the Interface Region Imaging Spectrograph ( IRIS ) spacecraft have found significant redshifts with >100 km s{sup −1}, which is consistent with a reconnection downflow. The ability to detect such a redshift with IRIS suggests that one may be able to use IRIS observations to identify flare TSs. Using a magnetohydrodynamic simulation to model magnetic reconnection of a solar flare and assuming the existence of a TS in the downflow of the reconnection plasma, we model the synthetic emission of the Fe xxi 1354.08 line in this work. We show that the existence of the TS in the solar flare may manifest itself in the Fe xxi 1354.08 Å line.

Authors:
 [1];  [2]; ;  [3]
  1. Lockheed Martin Solar and Astrophysics Laboratory, Palo Alto, CA (United States)
  2. Department of Space Science and CSPAR, University of Alabama in Huntsville, Huntsville, AL (United States)
  3. Harvard-Smithsonian Center for Astrophysics, Boston, MA (United States)
Publication Date:
OSTI Identifier:
22654395
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal Letters; Journal Volume: 846; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; EMISSION; HARD X RADIATION; INTERFACES; KEV RANGE; MAGNETIC RECONNECTION; MAGNETOHYDRODYNAMICS; MASS; PLASMA; RED SHIFT; SIMULATION; SOLAR FLARES; SOLAR SYSTEM; SPACE VEHICLES; SPECTRAL HARDENING; SUN; X-RAY SPECTRA

Citation Formats

Guo, Lijia, Li, Gang, Reeves, Kathy, and Raymond, John, E-mail: gang.li@uah.edu. Solar Flare Termination Shock and Synthetic Emission Line Profiles of the Fe xxi 1354.08 Å Line. United States: N. p., 2017. Web. doi:10.3847/2041-8213/AA866A.
Guo, Lijia, Li, Gang, Reeves, Kathy, & Raymond, John, E-mail: gang.li@uah.edu. Solar Flare Termination Shock and Synthetic Emission Line Profiles of the Fe xxi 1354.08 Å Line. United States. doi:10.3847/2041-8213/AA866A.
Guo, Lijia, Li, Gang, Reeves, Kathy, and Raymond, John, E-mail: gang.li@uah.edu. Fri . "Solar Flare Termination Shock and Synthetic Emission Line Profiles of the Fe xxi 1354.08 Å Line". United States. doi:10.3847/2041-8213/AA866A.
@article{osti_22654395,
title = {Solar Flare Termination Shock and Synthetic Emission Line Profiles of the Fe xxi 1354.08 Å Line},
author = {Guo, Lijia and Li, Gang and Reeves, Kathy and Raymond, John, E-mail: gang.li@uah.edu},
abstractNote = {Solar flares are among the most energetic phenomena that occur in the solar system. In the standard solar flare model, a fast mode shock, often referred to as the flare termination shock (TS), can exist above the loop-top source of hard X-ray emissions. The existence of the TS has been recently related to spectral hardening of a flare’s hard X-ray spectra at energies >300 keV. Observations of the Fe xxi 1354.08 Å line during solar flares by the Interface Region Imaging Spectrograph ( IRIS ) spacecraft have found significant redshifts with >100 km s{sup −1}, which is consistent with a reconnection downflow. The ability to detect such a redshift with IRIS suggests that one may be able to use IRIS observations to identify flare TSs. Using a magnetohydrodynamic simulation to model magnetic reconnection of a solar flare and assuming the existence of a TS in the downflow of the reconnection plasma, we model the synthetic emission of the Fe xxi 1354.08 line in this work. We show that the existence of the TS in the solar flare may manifest itself in the Fe xxi 1354.08 Å line.},
doi = {10.3847/2041-8213/AA866A},
journal = {Astrophysical Journal Letters},
number = 1,
volume = 846,
place = {United States},
year = {Fri Sep 01 00:00:00 EDT 2017},
month = {Fri Sep 01 00:00:00 EDT 2017}
}