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Title: High-resolution Observations of Sympathetic Filament Eruptions by NVST

Abstract

We investigate two sympathetic filament eruptions observed by the New Vacuum Solar Telescope on 2015 October 15. The full picture of the eruptions is obtained from the corresponding Solar Dynamics Observatory ( SDO )/Atmospheric Imaging Assembly (AIA) observations. The two filaments start from active region NOAA 12434 in the north and end in one large quiescent filament channel in the south. The left filament erupts first, followed by the right filament eruption about 10 minutes later. Clear twist structure and rotating motion are observed in both filaments during the eruption. Both eruptions failed, since the filaments first rise up, then flow toward the south and merge into the southern large quiescent filament. We also observe repeated activations of mini filaments below the right filament after its eruption. Using magnetic field models constructed based on SDO /HMI magnetograms via the flux rope insertion method, we find that the left filament eruption is likely to be triggered by kink instability, while the weakening of overlying magnetic fields due to magnetic reconnection at an X-point between the two filament systems might play an important role in the onset of the right filament eruption.

Authors:
; ; ;  [1];  [2];  [3]
  1. Key Laboratory for Dark Matter and Space Science, Purple Mountain Observatory, CAS, Nanjing 210008 (China)
  2. 5001 Riverwood Avenue, Sarasota, FL 34231 (United States)
  3. W. W. Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305 (United States)
Publication Date:
OSTI Identifier:
22663352
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal; Journal Volume: 844; 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; CHROMOSPHERE; ERUPTION; KINK INSTABILITY; MAGNETIC FIELDS; MAGNETIC RECONNECTION; RESOLUTION; ROTATION; SOLAR FLARES; SUN; TELESCOPES; ULTRAVIOLET RADIATION

Citation Formats

Li, Shangwei, Su, Yingna, Zhou, Tuanhui, Ji, Haisheng, Van Ballegooijen, Adriaan, and Sun, Xudong, E-mail: ynsu@pmo.ac.cn. High-resolution Observations of Sympathetic Filament Eruptions by NVST. United States: N. p., 2017. Web. doi:10.3847/1538-4357/AA78F5.
Li, Shangwei, Su, Yingna, Zhou, Tuanhui, Ji, Haisheng, Van Ballegooijen, Adriaan, & Sun, Xudong, E-mail: ynsu@pmo.ac.cn. High-resolution Observations of Sympathetic Filament Eruptions by NVST. United States. doi:10.3847/1538-4357/AA78F5.
Li, Shangwei, Su, Yingna, Zhou, Tuanhui, Ji, Haisheng, Van Ballegooijen, Adriaan, and Sun, Xudong, E-mail: ynsu@pmo.ac.cn. Thu . "High-resolution Observations of Sympathetic Filament Eruptions by NVST". United States. doi:10.3847/1538-4357/AA78F5.
@article{osti_22663352,
title = {High-resolution Observations of Sympathetic Filament Eruptions by NVST},
author = {Li, Shangwei and Su, Yingna and Zhou, Tuanhui and Ji, Haisheng and Van Ballegooijen, Adriaan and Sun, Xudong, E-mail: ynsu@pmo.ac.cn},
abstractNote = {We investigate two sympathetic filament eruptions observed by the New Vacuum Solar Telescope on 2015 October 15. The full picture of the eruptions is obtained from the corresponding Solar Dynamics Observatory ( SDO )/Atmospheric Imaging Assembly (AIA) observations. The two filaments start from active region NOAA 12434 in the north and end in one large quiescent filament channel in the south. The left filament erupts first, followed by the right filament eruption about 10 minutes later. Clear twist structure and rotating motion are observed in both filaments during the eruption. Both eruptions failed, since the filaments first rise up, then flow toward the south and merge into the southern large quiescent filament. We also observe repeated activations of mini filaments below the right filament after its eruption. Using magnetic field models constructed based on SDO /HMI magnetograms via the flux rope insertion method, we find that the left filament eruption is likely to be triggered by kink instability, while the weakening of overlying magnetic fields due to magnetic reconnection at an X-point between the two filament systems might play an important role in the onset of the right filament eruption.},
doi = {10.3847/1538-4357/AA78F5},
journal = {Astrophysical Journal},
number = 1,
volume = 844,
place = {United States},
year = {Thu Jul 20 00:00:00 EDT 2017},
month = {Thu Jul 20 00:00:00 EDT 2017}
}