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Title: Reconnection–Condensation Model for Solar Prominence Formation

Abstract

We propose a reconnection–condensation model in which topological change in a coronal magnetic field via reconnection triggers radiative condensation, thereby resulting in prominence formation. Previous observational studies have suggested that reconnection at a polarity inversion line of a coronal arcade field creates a flux rope that can sustain a prominence; however, they did not explain the origin of cool dense plasmas of prominences. Using three-dimensional magnetohydrodynamic simulations, including anisotropic nonlinear thermal conduction and optically thin radiative cooling, we demonstrate that reconnection can lead not only to flux rope formation but also to radiative condensation under a certain condition. In our model, this condition is described by the Field length, which is defined as the scale length for thermal balance between radiative cooling and thermal conduction. This critical condition depends weakly on the artificial background heating. The extreme ultraviolet emissions synthesized with our simulation results have good agreement with observational signatures reported in previous studies.

Authors:
 [1];  [2]
  1. Institute for Space-Earth Environmental Research, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Aichi 464-8601 (Japan)
  2. Department of Earth and Planetary Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033 (Japan)
Publication Date:
OSTI Identifier:
22663300
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 845; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 0004-637X
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ANISOTROPY; EMISSION; EXTREME ULTRAVIOLET RADIATION; MAGNETIC FIELDS; MAGNETOHYDRODYNAMICS; NONLINEAR PROBLEMS; PLASMA; RADIATIVE COOLING; SIMULATION; SOLAR PROMINENCES; SUN; THERMAL CONDUCTION; THREE-DIMENSIONAL CALCULATIONS

Citation Formats

Kaneko, Takafumi, and Yokoyama, Takaaki, E-mail: kaneko@isee.nagoya-u.ac.jp. Reconnection–Condensation Model for Solar Prominence Formation. United States: N. p., 2017. Web. doi:10.3847/1538-4357/AA7D59.
Kaneko, Takafumi, & Yokoyama, Takaaki, E-mail: kaneko@isee.nagoya-u.ac.jp. Reconnection–Condensation Model for Solar Prominence Formation. United States. doi:10.3847/1538-4357/AA7D59.
Kaneko, Takafumi, and Yokoyama, Takaaki, E-mail: kaneko@isee.nagoya-u.ac.jp. Thu . "Reconnection–Condensation Model for Solar Prominence Formation". United States. doi:10.3847/1538-4357/AA7D59.
@article{osti_22663300,
title = {Reconnection–Condensation Model for Solar Prominence Formation},
author = {Kaneko, Takafumi and Yokoyama, Takaaki, E-mail: kaneko@isee.nagoya-u.ac.jp},
abstractNote = {We propose a reconnection–condensation model in which topological change in a coronal magnetic field via reconnection triggers radiative condensation, thereby resulting in prominence formation. Previous observational studies have suggested that reconnection at a polarity inversion line of a coronal arcade field creates a flux rope that can sustain a prominence; however, they did not explain the origin of cool dense plasmas of prominences. Using three-dimensional magnetohydrodynamic simulations, including anisotropic nonlinear thermal conduction and optically thin radiative cooling, we demonstrate that reconnection can lead not only to flux rope formation but also to radiative condensation under a certain condition. In our model, this condition is described by the Field length, which is defined as the scale length for thermal balance between radiative cooling and thermal conduction. This critical condition depends weakly on the artificial background heating. The extreme ultraviolet emissions synthesized with our simulation results have good agreement with observational signatures reported in previous studies.},
doi = {10.3847/1538-4357/AA7D59},
journal = {Astrophysical Journal},
issn = {0004-637X},
number = 1,
volume = 845,
place = {United States},
year = {2017},
month = {8}
}