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Title: Magnetic reconnection in the low solar chromosphere with a more realistic radiative cooling model

Abstract

Magnetic reconnection is the most likely mechanism responsible for the high temperature events that are observed in strongly magnetized locations around the temperature minimum in the low solar chromosphere. This work improves upon our previous work [Ni et al., Astrophys. J. 852, 95 (2018)] by using a more realistic radiative cooling model computed from the OPACITY project and the CHIANTI database. We find that the rate of ionization of the neutral component of the plasma is still faster than recombination within the current sheet region. For low β plasmas, the ionized and neutral fluid flows are well-coupled throughout the reconnection region resembling the single-fluid Sweet-Parker model dynamics. Decoupling of the ion and neutral inflows appears in the higher β case with β 0=1.46, which leads to a reconnection rate about three times faster than the rate predicted by the Sweet-Parker model. In all cases, the plasma temperature increases with time inside the current sheet, and the maximum value is above 2×10 4 K when the reconnection magnetic field strength is greater than 500 G. While the more realistic radiative cooling model does not result in qualitative changes of the characteristics of magnetic reconnection, it is necessary for studying the variationsmore » of the plasma temperature and ionization fraction inside current sheets in strongly magnetized regions of the low solar atmosphere. It is also important for studying energy conversion during the magnetic reconnection process when the hydrogen-dominated plasma approaches full ionization.« less

Authors:
ORCiD logo [1];  [2]; ORCiD logo [3];  [1]
  1. Chinese Academy of Sciences (CAS), Kunming, Yunnan (China). Yunnan Observatories; Chinese Academy of Sciences (CAS), Beijing (China). Center for Astronomical Mega-Science
  2. National Science Foundation (NSF), Alexandria, VA (United States)
  3. Harvard-Smithsonian Center for Astrophysics, Cambridge, MA (United States)
Publication Date:
Research Org.:
Smithsonian Inst. Cambridge, MA (United States)
Sponsoring Org.:
USDOE Office of Science (SC); National Science Foundation (NSF)
OSTI Identifier:
1514857
Grant/Contract Number:  
SC0016363; AGS-1358342
Resource Type:
Accepted Manuscript
Journal Name:
Physics of Plasmas
Additional Journal Information:
Journal Volume: 25; Journal Issue: 4; Journal ID: ISSN 1070-664X
Publisher:
American Institute of Physics (AIP)
Country of Publication:
United States
Language:
English
Subject:
70 PLASMA PHYSICS AND FUSION TECHNOLOGY

Citation Formats

Ni, Lei, Lukin, Vyacheslav S., Murphy, Nicholas A., and Lin, Jun. Magnetic reconnection in the low solar chromosphere with a more realistic radiative cooling model. United States: N. p., 2018. Web. doi:10.1063/1.5018351.
Ni, Lei, Lukin, Vyacheslav S., Murphy, Nicholas A., & Lin, Jun. Magnetic reconnection in the low solar chromosphere with a more realistic radiative cooling model. United States. doi:10.1063/1.5018351.
Ni, Lei, Lukin, Vyacheslav S., Murphy, Nicholas A., and Lin, Jun. Tue . "Magnetic reconnection in the low solar chromosphere with a more realistic radiative cooling model". United States. doi:10.1063/1.5018351. https://www.osti.gov/servlets/purl/1514857.
@article{osti_1514857,
title = {Magnetic reconnection in the low solar chromosphere with a more realistic radiative cooling model},
author = {Ni, Lei and Lukin, Vyacheslav S. and Murphy, Nicholas A. and Lin, Jun},
abstractNote = {Magnetic reconnection is the most likely mechanism responsible for the high temperature events that are observed in strongly magnetized locations around the temperature minimum in the low solar chromosphere. This work improves upon our previous work [Ni et al., Astrophys. J. 852, 95 (2018)] by using a more realistic radiative cooling model computed from the OPACITY project and the CHIANTI database. We find that the rate of ionization of the neutral component of the plasma is still faster than recombination within the current sheet region. For low β plasmas, the ionized and neutral fluid flows are well-coupled throughout the reconnection region resembling the single-fluid Sweet-Parker model dynamics. Decoupling of the ion and neutral inflows appears in the higher β case with β0=1.46, which leads to a reconnection rate about three times faster than the rate predicted by the Sweet-Parker model. In all cases, the plasma temperature increases with time inside the current sheet, and the maximum value is above 2×104 K when the reconnection magnetic field strength is greater than 500 G. While the more realistic radiative cooling model does not result in qualitative changes of the characteristics of magnetic reconnection, it is necessary for studying the variations of the plasma temperature and ionization fraction inside current sheets in strongly magnetized regions of the low solar atmosphere. It is also important for studying energy conversion during the magnetic reconnection process when the hydrogen-dominated plasma approaches full ionization.},
doi = {10.1063/1.5018351},
journal = {Physics of Plasmas},
number = 4,
volume = 25,
place = {United States},
year = {2018},
month = {4}
}

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Cited by: 4 works
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Figures / Tables:

Table I Table I: The important variables in case ALr, CLr, and ELr in this work and in case A, C, and E in our previous work. The maximum values of the ionization fraction fi, the plasma temperature Ti, the current density Jz, the difference between the ion and neutral inflows |Viymore » - Vny|, the outflow ion velocity Vix, the magnetic reconnection rate Msim, the minimum value of the current sheet width δsim, and the ion density ni during the later reconnection stage are presented.« less

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    Figures/Tables have been extracted from DOE-funded journal article accepted manuscripts.