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MHD Numerical Simulations of Magnetic Reconnection Associated with Emerging Flux

Published online by Cambridge University Press:  12 April 2016

K. Shibata ,
S. Nozawa  and
R. Matsumoto
K. Shibata
Affiliation:
National Astronomical Observatory, Mitaka, Tokyo 181, Japan
S. Nozawa
Affiliation:
STE Laboratory, Nagoya University, Toyokawa442
R. Matsumoto
Affiliation:
College of Arts and Sciences, Chiba University, Chiba260

Abstract

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Two-dimensional (2D) magnetohydrodynamic (MHD) numerical simulations have been performed to study magnetic reconnection between emerging flux and the overlying coronal magnetic field, taking into account of gravity. It is found that (1) reconnection starts when most of chromospheric mass in the current sheet between the emerging flux and the coronal field has drained down along the loop because of gravity, (2) multiple magnetic islands, which confine cool, dense chromospheric plasma, are created in the sheet; the islands coalesce dynamically and are ejected along the sheet, together with the ambient hot plasma, at Alfven speed. The coexistence of hot and cool plasmas in the mass ejection (jet) associated with the reconnection seems to explain those X-ray jets observed by Yohkoh, which are identified with Hα surges.

Type
Session 8. Structure and Role of Emerging Flux Regions
Information
International Astronomical Union Colloquium , Volume 141: The Magnetic and Velocity Fields of Solar Active Regions , 1993 , pp. 500 - 503
Copyright
Copyright © Astronomical Society of the Pacific 1993

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