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Title: SDO/AIA OBSERVATION OF KELVIN-HELMHOLTZ INSTABILITY IN THE SOLAR CORONA

Abstract

We present observations of the formation, propagation, and decay of vortex-shaped features in coronal images from the Solar Dynamics Observatory associated with an eruption starting at about 2:30 UT on 2010 April 8. The series of vortices were formed along the interface between an erupting (dimming) region and the surrounding corona. They ranged in size from several to 10 arcsec and traveled along the interface at 6-14 km s{sup -1}. The features were clearly visible in six out of the seven different EUV wave bands of the Atmospheric Imaging Assembly. Based on the structure, formation, propagation, and decay of these features, we identified the event as the first observation of the Kelvin-Helmholtz instability (KHI) in the corona in EUV. The interpretation is supported by linear analysis and by a nonlinear 2.5-dimensional magnetohydrodynamic model of KHI. We conclude that the instability is driven by the velocity shear between the erupting and closed magnetic field of the coronal mass ejection. The shear-flow-driven instability can play an important role in energy transfer processes in coronal plasma.

Authors:
 [1];  [2]
  1. Department of Physics, Catholic University of America, Washington, DC 20064 (United States)
  2. NASA Goddard Space Flight Center, Code 671, Greenbelt, MD 20771 (United States)
Publication Date:
OSTI Identifier:
21562612
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal Letters
Additional Journal Information:
Journal Volume: 734; Journal Issue: 1; Other Information: DOI: 10.1088/2041-8205/734/1/L11; Journal ID: ISSN 2041-8205
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ENERGY TRANSFER; ERUPTION; EXTREME ULTRAVIOLET RADIATION; HELMHOLTZ INSTABILITY; MAGNETIC FIELDS; MASS; SHEAR; SOLAR CORONA; VORTICES; ATMOSPHERES; ELECTROMAGNETIC RADIATION; INSTABILITY; PLASMA INSTABILITY; PLASMA MACROINSTABILITIES; RADIATIONS; SOLAR ATMOSPHERE; STELLAR ATMOSPHERES; STELLAR CORONAE; ULTRAVIOLET RADIATION

Citation Formats

Ofman, L, and Thompson, B J. SDO/AIA OBSERVATION OF KELVIN-HELMHOLTZ INSTABILITY IN THE SOLAR CORONA. United States: N. p., 2011. Web. doi:10.1088/2041-8205/734/1/L11.
Ofman, L, & Thompson, B J. SDO/AIA OBSERVATION OF KELVIN-HELMHOLTZ INSTABILITY IN THE SOLAR CORONA. United States. https://doi.org/10.1088/2041-8205/734/1/L11
Ofman, L, and Thompson, B J. 2011. "SDO/AIA OBSERVATION OF KELVIN-HELMHOLTZ INSTABILITY IN THE SOLAR CORONA". United States. https://doi.org/10.1088/2041-8205/734/1/L11.
@article{osti_21562612,
title = {SDO/AIA OBSERVATION OF KELVIN-HELMHOLTZ INSTABILITY IN THE SOLAR CORONA},
author = {Ofman, L and Thompson, B J},
abstractNote = {We present observations of the formation, propagation, and decay of vortex-shaped features in coronal images from the Solar Dynamics Observatory associated with an eruption starting at about 2:30 UT on 2010 April 8. The series of vortices were formed along the interface between an erupting (dimming) region and the surrounding corona. They ranged in size from several to 10 arcsec and traveled along the interface at 6-14 km s{sup -1}. The features were clearly visible in six out of the seven different EUV wave bands of the Atmospheric Imaging Assembly. Based on the structure, formation, propagation, and decay of these features, we identified the event as the first observation of the Kelvin-Helmholtz instability (KHI) in the corona in EUV. The interpretation is supported by linear analysis and by a nonlinear 2.5-dimensional magnetohydrodynamic model of KHI. We conclude that the instability is driven by the velocity shear between the erupting and closed magnetic field of the coronal mass ejection. The shear-flow-driven instability can play an important role in energy transfer processes in coronal plasma.},
doi = {10.1088/2041-8205/734/1/L11},
url = {https://www.osti.gov/biblio/21562612}, journal = {Astrophysical Journal Letters},
issn = {2041-8205},
number = 1,
volume = 734,
place = {United States},
year = {Fri Jun 10 00:00:00 EDT 2011},
month = {Fri Jun 10 00:00:00 EDT 2011}
}