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 (1181) (Citation History)
· Refereed Citations to the Article
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Dynamics of the quiescent solar corona
Authors:
Rosner, R.; Tucker, W. H.; Vaiana, G. S.
Affiliation:
AA(Harvard College Observatory and Smithsonian Astrophysical Observatory, Center for Astrophysics, Cambridge, Mass.), AB(Harvard College Observatory and Smithsonian Astrophysical Observatory, Center for Astrophysics, Cambridge, Mass.), AC(Harvard College Observatory and Smithsonian Astrophysical Observatory, Center for Astrophysics, Cambridge, Mass; Osservatorio Astronomico, Palermo, Italy)
Publication:
Astrophysical Journal, Part 1, vol. 220, Mar. 1, 1978, p. 643-645, 647, 649-653, 655-665. Research supported by the Smithsonian Institution; (ApJ Homepage)
Publication Date:
03/1978
Category:
Solar Physics
Origin:
STI
NASA/STI Keywords:
Solar Activity, Solar Corona, Solar X-Rays, X Ray Astronomy, Astronomical Models, Convective Flow, Hydrostatic Pressure, Parameterization, Plasma Control, Skylab Program, Stellar Magnetic Fields
DOI:
10.1086/155949
Bibliographic Code:
1978ApJ...220..643R

Abstract

An analytical model for the quiescent inhomogeneous solar corona is developed on the basis of the hypothesis that looplike structures are the basic coronal building blocks. By assuming that quiescent loop structures observed in X-rays are in hydrostatic equilibrium, it is demonstrated that such loops must have their temperature maximum located near their apex and that substantial nonradiative energy deposition must occur along most of their length. The calculations yield a unique relation among loop temperature, pressure, and size, which fits the X-ray observations of quiescent structures well and is consistent with the initial assumption of hydrostatic equilibrium. The results suggest that the coronal loops visible in X-rays represent a relatively steady-state equilibrium of the confined plasmas and that fluctuations in such quantities as the local heating rate can lead to dynamically unstable states in which the loop plasma does not attain a temperature sufficient for X-ray emission. A parameterization of various proposed coronal heating theories is also developed within the context of the analytical model.

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