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Solar transition region and coronal response to heating rate perturbationsObservations of Doppler shifts in UV emission lines formed in the solar transition region show continual plasma downflows and impulsive plasma upflows. Using numerical simulations, the authors examine the conjecture that areas of downflowing plasma are the base regions of coronal loops in which the heating is gradually decreasing and that areas of upflowing plasma are the base regions of coronal loops in which the heating rate is gradually increasing. Beginning with a coronal loop in equilibrium, the heating rate is reduced on time scales of 100, 1000, and 2000 s to 10 percent and 1 percent of the initial value, and the loop is allowed to evolve to a new equilibrium. The heating rate for the cooled models is then increased back to the initial value on the same time scales. While significant mass motions do develop in the simulations, both the emission measure and the velocity at 100,000 K do not show the characteristics present in UV observations.
Document ID
19870062596
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Mariska, John T.
(U.S. Navy, E. O. Hulburt Center for Space Research, Washington DC, United States)
Date Acquired
August 13, 2013
Publication Date
August 1, 1987
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 319
ISSN: 0004-637X
Subject Category
Solar Physics
Accession Number
87A49870
Distribution Limits
Public
Copyright
Other

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