A new view of the solar outer atmosphere by the transition region and Coronal Explorer

Schrijver, C. J. et al. (1999) A new view of the solar outer atmosphere by the transition region and Coronal Explorer. Solar Physics, 187(2), pp. 261-302. (doi:10.1023/A:1005194519642)

Schrijver, C. J. et al. (1999) A new view of the solar outer atmosphere by the transition region and Coronal Explorer. Solar Physics, 187(2), pp. 261-302. (doi:10.1023/A:1005194519642)

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Abstract

The Transition Region and Coronal Explorer (TRACE) described in the companion paper by Handy et al. (1999) provides an unprecedented view of the solar outer atmosphere. In this overview, we discuss the initial impressions gained from, and interpretations of, the first million images taken with TRACE. We address, among other topics, the fine structure of the corona, the larger-scale thermal trends, the evolution of the corona over quiet and active regions, the high incidence of chromospheric material dynamically embedded in the coronal environment, the dynamics and structure of the conductively dominated transition region between chromosphere and corona, loop oscillations and flows, and sunspot coronal loops. With TRACE we observe a corona that is extremely dynamic and full of flows and wave phenomena, in which loops evolve rapidly in temperature, with associated changes in density. This dynamic nature points to a high degree of spatio-temporal variability even under conditions that traditionally have been referred to as quiescent. This variability requires that coronal heating can turn on and off on a time scale of minutes or less along field-line bundles with cross sections at or below the instrumental resolution of 700 km. Loops seen at 171 Å (˜1 MK) appear to meander through the coronal volume, but it is unclear whether this is caused by the evolution of the field or by the weaving of the heating through the coronal volume, shifting around for periods of up to a few tens of minutes and lighting up subsequent field lines. We discuss evidence that the heating occurs predominantly within the first 10 to 20 Mm from the loop footpoints. This causes the inner parts of active-region coronae to have a higher average temperature than the outer domains.

Item Type:Articles
Status:Published
Refereed:Yes
Glasgow Author(s) Enlighten ID:Fletcher, Professor Lyndsay
Authors: Schrijver, C. J., Title, A.M., Berger, T.E., Fletcher, L., Hurlburt, N.E., Nightingale, R.A., Tarbell, T.D., Wolfson, J., Golub, L., Bookbinder, J.A., Deluca, E.E., Warren, H.P., Kankelborg, C.C., Handy, B.N., and DePontieu, B.
Subjects:Q Science > QB Astronomy
Q Science > QC Physics
College/School:College of Science and Engineering > School of Physics and Astronomy
Research Group:Astronomy and Astrophysics
Journal Name:Solar Physics
Journal Abbr.:Sol. Phys.
Publisher:Springer Verlag
ISSN:0038-0938
ISSN (Online):1573-093X

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