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Relationships Between Sequential Chromospheric Brightening and the Corona

Published online by Cambridge University Press:  12 September 2017

M. S. Kirk Open the ORCID record for M. S. Kirk [Opens in a new window] ,
K. S. Balasubramaniam ,
J. Jackiewicz  and
H. R. Gilbert
M. S. Kirk
Affiliation:
NASA Goddard Space Flight Center, Catholic University of America 8800 Greenbelt Rd., Code 670, Greenbelt, MD 20771, USA email: michael.s.kirk@nasa.gov
K. S. Balasubramaniam
Affiliation:
AFRL Battlespace Environment Division (AFRL/RVB)
J. Jackiewicz
Affiliation:
Department of Astronomy, New Mexico State University Las Cruces, NM 88003, USA
H. R. Gilbert
Affiliation:
NASA Goddard Space Flight Center8800 Greenbelt Rd., Code 670, Greenbelt, MD 20771, USA
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Abstract

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The chromosphere is a complex region that acts as an intermediary between the magnetic flux emergence in the photosphere and the magnetic features seen in the corona. Large eruptions in the chromosphere of flares and filaments are often accompanied by ejections of coronal mass off the sun. Several studies have observed fast-moving progressive trains of compact bright points (called Sequential Chromospheric Brightenings or SCBs) streaming away from chromospheric flares that also produce a coronal mass ejection (CME). In this work, we review studies of SCBs and search for commonalties between them. We place these findings into a larger context with contemporary chromospheric and coronal observations. SCBs are fleeting indicators of the solar atmospheric environment as it existed before their associated eruption. Since they appear at the very outset of a flare eruption, SCBs are good early indication of a CME measured in the chromosphere.

Keywords

Sun: chromosphereSun: flaresSun: corona
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S327: Fine Structure and Dynamics of the Solar Atmosphere , October 2016 , pp. 117 - 127
Copyright
Copyright © International Astronomical Union 2017 

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