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Title: SDO/AIA DETECTION OF SOLAR PROMINENCE FORMATION WITHIN A CORONAL CAVITY

Abstract

We report the first analyses of SDO/AIA observations of the formation of a quiescent polar crown prominence in a coronal cavity. The He II 304 A (log T{sub max} {approx} 4.8 K) data show both the gradual disappearance of the prominence due to vertical drainage and lateral transport of plasma followed by the formation of a new prominence 12 hr later. The formation is preceded by the appearance of a bright emission 'cloud' in the central region of the coronal cavity. The peak brightness of the cloud progressively shifts in time from the Fe XIV 211 A channel, through the Fe XII 193 A channel, to the Fe IX 171 A channel (log T{sub max} {approx} 6.2, 6.1, 5.8 K, respectively) while simultaneously decreasing in altitude. Filter ratio analysis estimates the initial temperature of the cloud to be approximately log T {approx} 6.25 K with evidence of cooling over time. The subsequent growth of the prominence is accompanied by darkening of the cavity in the 211 A channel. The observations imply prominence formation via in situ condensation of hot plasma from the coronal cavity, in support of our previously proposed process of magnetothermal convection in coronal magnetic flux ropes.

Authors:
 [1];  [2];  [3]
  1. National Solar Observatory, 950 North Cherry Avenue, Tucson, AZ 85719 (United States)
  2. Lockheed Martin Solar and Astrophysics Laboratory, B/252 3251 Hanover Street, Palo Alto, CA 94304 (United States)
  3. High Altitude Observatory, National Center for Atmospheric Research, P.O. Box 3000, Boulder, CO 80307 (United States)
Publication Date:
OSTI Identifier:
22078475
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal Letters
Additional Journal Information:
Journal Volume: 758; Journal Issue: 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 2041-8205
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; BRIGHTNESS; CAVITIES; CHROMOSPHERE; CONVECTION; COOLING; EMISSION; HOT PLASMA; MAGNETIC FLUX; SOLAR CORONA; SOLAR PROMINENCES

Citation Formats

Berger, Thomas E., Liu Wei, and Low, B. C. SDO/AIA DETECTION OF SOLAR PROMINENCE FORMATION WITHIN A CORONAL CAVITY. United States: N. p., 2012. Web. doi:10.1088/2041-8205/758/2/L37.
Berger, Thomas E., Liu Wei, & Low, B. C. SDO/AIA DETECTION OF SOLAR PROMINENCE FORMATION WITHIN A CORONAL CAVITY. United States. doi:10.1088/2041-8205/758/2/L37.
Berger, Thomas E., Liu Wei, and Low, B. C. Sat . "SDO/AIA DETECTION OF SOLAR PROMINENCE FORMATION WITHIN A CORONAL CAVITY". United States. doi:10.1088/2041-8205/758/2/L37.
@article{osti_22078475,
title = {SDO/AIA DETECTION OF SOLAR PROMINENCE FORMATION WITHIN A CORONAL CAVITY},
author = {Berger, Thomas E. and Liu Wei and Low, B. C.},
abstractNote = {We report the first analyses of SDO/AIA observations of the formation of a quiescent polar crown prominence in a coronal cavity. The He II 304 A (log T{sub max} {approx} 4.8 K) data show both the gradual disappearance of the prominence due to vertical drainage and lateral transport of plasma followed by the formation of a new prominence 12 hr later. The formation is preceded by the appearance of a bright emission 'cloud' in the central region of the coronal cavity. The peak brightness of the cloud progressively shifts in time from the Fe XIV 211 A channel, through the Fe XII 193 A channel, to the Fe IX 171 A channel (log T{sub max} {approx} 6.2, 6.1, 5.8 K, respectively) while simultaneously decreasing in altitude. Filter ratio analysis estimates the initial temperature of the cloud to be approximately log T {approx} 6.25 K with evidence of cooling over time. The subsequent growth of the prominence is accompanied by darkening of the cavity in the 211 A channel. The observations imply prominence formation via in situ condensation of hot plasma from the coronal cavity, in support of our previously proposed process of magnetothermal convection in coronal magnetic flux ropes.},
doi = {10.1088/2041-8205/758/2/L37},
journal = {Astrophysical Journal Letters},
issn = {2041-8205},
number = 2,
volume = 758,
place = {United States},
year = {2012},
month = {10}
}