Sign on

SAO/NASA ADS Astronomy Abstract Service


· Find Similar Abstracts (with default settings below)
· Full Refereed Journal Article (PDF/Postscript)
· Full Refereed Scanned Article (GIF)
· References in the article
· Citations to the Article (89) (Citation History)
· Refereed Citations to the Article
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Cooling of solar flares plasmas. 1: Theoretical considerations
Authors:
Cargill, Peter J.; Mariska, John T.; Antiochos, Spiro K.
Affiliation:
AA(Naval Research Laboratory, Washington, DC, US), AB(Naval Research Laboratory, Washington, DC, US), AC(Naval Research Laboratory, Washington, DC, US)
Publication:
The Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 439, no. 2, p. 1034-1043 (ApJ Homepage)
Publication Date:
02/1995
Category:
Solar Physics
Origin:
STI
NASA/STI Keywords:
COOLING, CORONAL LOOPS, MAGNETOHYDRODYNAMICS, NUMERICAL ANALYSIS, PLASMAS (PHYSICS), SOLAR FLARES, CONDUCTIVE HEAT TRANSFER, MATHEMATICAL MODELS, RADIATIVE HEAT TRANSFER, SCALING LAWS, TEMPERATURE DISTRIBUTION
DOI:
10.1086/175240
Bibliographic Code:
1995ApJ...439.1034C

Abstract

Theoretical models of the cooling of flare plasma are reexamined. By assuming that the cooling occurs in two separate phase where conduction and radiation, respectively, dominate, a simple analytic formula for the cooling time of a flare plasma is derived. Unlike earlier order-of-magnitude scalings, this result accounts for the effect of the evolution of the loop plasma parameters on the cooling time. When the conductive cooling leads to an 'evaporation' of chromospheric material, the cooling time scales L5/6/p1/6, where the coronal phase (defined as the time maximum temperature). When the conductive cooling is static, the cooling time scales as L3/4n1/4. In deriving these results, use was made of an important scaling law (T proportional to n2) during the radiative cooling phase that was forst noted in one-dimensional hydrodynamic numerical simulations (Serio et al. 1991; Jakimiec et al. 1992). Our own simulations show that this result is restricted to approximately the radiative loss function of Rosner, Tucker, & Vaiana (1978). for different radiative loss functions, other scaling result, with T and n scaling almost linearly when the radiative loss falls off as T-2. It is shown that these scaling laws are part of a class of analytic solutions developed by Antiocos (1980).

Printing Options

Print whole paper
Print Page(s) through

Return 600 dpi PDF to Acrobat/Browser. Different resolutions (200 or 600 dpi), formats (Postscript, PDF, etc), page sizes (US Letter, European A4, etc), and compression (gzip,compress,none) can be set through the Printing Preferences



More Article Retrieval Options

HELP for Article Retrieval


Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)

  New!

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints