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Record Details

Record 16 of 51486
Shock Formation and Energy Dissipation of Slow Magnetosonic Waves in Coronal Plumes
Author and Affiliation:
Cuntz, M.(Texas Univ., Arlington, TX, United States)
Suess, S. T.(National Space Science and Technology Center, Huntsville, AL, United States)
Abstract: We study the shock formation and energy dissipation of slow magnetosonic waves in coronal plumes. The wave parameters and the spreading function of the plumes as well as the base magnetic field strength are given by empirical constraints mostly from SOHO/UVCS. Our models show that shock formation occurs at low coronal heights, i.e., within 1.3 bun, depending on the model parameters. In addition, following analytical estimates, we show that scale height of energy dissipation by the shocks ranges between 0.15 and 0.45 Rsun. This implies that shock heating by slow magnetosonic waves is relevant at most heights, even though this type of waves is apparently not a solely operating energy supply mechanism.
Publication Date: Jan 01, 2003
Document ID:
20040005906
(Acquired Jan 21, 2004)
Subject Category: ENERGY PRODUCTION AND CONVERSION
Document Type: Preprint
Meeting Information: 12th Cambridge Workshop on Cool Stars, Stellar Systems and The Sun; 30 Jul. - 3 Aug. 2001; Boulder, CO; United States
Financial Sponsor: NASA Marshall Space Flight Center; Huntsville, AL, United States
Organization Source: Texas Univ.; Arlington, TX, United States
Description: 1p; In English
Distribution Limits: Unclassified; Publicly available; Unlimited
Rights: No Copyright
NASA Terms: SHOCK HEATING; MAGNETOACOUSTIC WAVES; CORONAS; ENERGY OF FORMATION; MAGNETIC FLUX; ENERGY DISSIPATION; SPREADING; PLUMES; ESTIMATES
Availability Source: Other Sources
Availability Notes: Abstract Only
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