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Title: MHD Simulations of the Eruption of Coronal Flux Ropes under Coronal Streamers

Abstract

Using three-dimensional magnetohydrodynamic (MHD) simulations, we investigate the eruption of coronal flux ropes underlying coronal streamers and the development of a prominence eruption. We initialize a quasi-steady solution of a coronal helmet streamer, into which we impose at the lower boundary the slow emergence of a part of a twisted magnetic torus. As a result, a quasi-equilibrium flux rope is built up under the streamer. With varying streamer sizes and different lengths and total twists of the flux rope that emerges, we found different scenarios for the evolution from quasi-equilibrium to eruption. In the cases with a broad streamer, the flux rope remains well confined until there is sufficient twist such that it first develops the kink instability and evolves through a sequence of kinked, confined states with increasing height until it eventually develops a “hernia-like” ejective eruption. For significantly twisted flux ropes, prominence condensations form in the dips of the twisted field lines due to runaway radiative cooling. Once formed, the prominence-carrying field becomes significantly non-force-free due to the weight of the prominence, despite having low plasma β . As the flux rope erupts, the prominence erupts, showing substantial draining along the legs of the erupting flux rope. Themore » prominence may not show a kinked morphology even though the flux rope becomes kinked. On the other hand, in the case with a narrow streamer, the flux rope with less than one wind of twist can erupt via the onset of the torus instability.« less

Authors:
 [1]
  1. High Altitude Observatory, National Center for Atmospheric Research, 3080 Center Green Drive, Boulder, CO 80301 (United States)
Publication Date:
OSTI Identifier:
22663371
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 844; 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; EQUILIBRIUM; KINK INSTABILITY; MAGNETOHYDRODYNAMICS; MASS; PLASMA; RADIATIVE COOLING; SIMULATION; STAR EVOLUTION; STELLAR CORONAE; STELLAR WINDS; SUN; THREE-DIMENSIONAL CALCULATIONS

Citation Formats

Fan, Yuhong, E-mail: yfan@ucar.edu. MHD Simulations of the Eruption of Coronal Flux Ropes under Coronal Streamers. United States: N. p., 2017. Web. doi:10.3847/1538-4357/AA7A56.
Fan, Yuhong, E-mail: yfan@ucar.edu. MHD Simulations of the Eruption of Coronal Flux Ropes under Coronal Streamers. United States. doi:10.3847/1538-4357/AA7A56.
Fan, Yuhong, E-mail: yfan@ucar.edu. Thu . "MHD Simulations of the Eruption of Coronal Flux Ropes under Coronal Streamers". United States. doi:10.3847/1538-4357/AA7A56.
@article{osti_22663371,
title = {MHD Simulations of the Eruption of Coronal Flux Ropes under Coronal Streamers},
author = {Fan, Yuhong, E-mail: yfan@ucar.edu},
abstractNote = {Using three-dimensional magnetohydrodynamic (MHD) simulations, we investigate the eruption of coronal flux ropes underlying coronal streamers and the development of a prominence eruption. We initialize a quasi-steady solution of a coronal helmet streamer, into which we impose at the lower boundary the slow emergence of a part of a twisted magnetic torus. As a result, a quasi-equilibrium flux rope is built up under the streamer. With varying streamer sizes and different lengths and total twists of the flux rope that emerges, we found different scenarios for the evolution from quasi-equilibrium to eruption. In the cases with a broad streamer, the flux rope remains well confined until there is sufficient twist such that it first develops the kink instability and evolves through a sequence of kinked, confined states with increasing height until it eventually develops a “hernia-like” ejective eruption. For significantly twisted flux ropes, prominence condensations form in the dips of the twisted field lines due to runaway radiative cooling. Once formed, the prominence-carrying field becomes significantly non-force-free due to the weight of the prominence, despite having low plasma β . As the flux rope erupts, the prominence erupts, showing substantial draining along the legs of the erupting flux rope. The prominence may not show a kinked morphology even though the flux rope becomes kinked. On the other hand, in the case with a narrow streamer, the flux rope with less than one wind of twist can erupt via the onset of the torus instability.},
doi = {10.3847/1538-4357/AA7A56},
journal = {Astrophysical Journal},
issn = {0004-637X},
number = 1,
volume = 844,
place = {United States},
year = {2017},
month = {7}
}