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Prominence-corona interface compared with the chromosphere-corona transition region

Journal Article:

Abstract

The intensities of 52 EUV emission lines from each of 9 hedgerow prominences observed at the limb with the Harvard experiment on ATM-Skylab have been compared with intensities from the interior of network cells at the center of the disk, in order to compare the prominence-corona (P-C) interface with the chromosphere-corona (C-C) transition region. The intensity ratio Isub(cell)/Isub(prominence) for each line varies systematically (in all of the prominences observed), with the temperature of formation of the line as approximately Tsup(-0.6). The density sensitive C III (formed at T approximately 9x10/sup 4/ K) line ratio Isub(lambda1175)/Isub(lambda977) implies an average density 1.3x10/sup 9/ electrons cm/sup -3/ in the P-C interface and approximately 4 times this value in the C-C transition of the cells. The total optical thickness at the head of the Lyman continuum is < approximately 10 in most of the prominences studied; in two of the prominences, however, the possibility that tau/sub 0/ is large cannot be rejected. Methods of analysis of these EUV data are developed assuming both a resolved and an unresolved internal prominence structure. Although the systematic differences between the P-C interface and the C-C transition are stressed, the similarities are probably more remarkable and may be  More>>
Authors:
Orrall, F Q; Schmahl, E J [1] 
  1. Harvard Coll. Observatory, Cambridge, Mass. (USA)
Publication Date:
Nov 01, 1976
Product Type:
Journal Article
Reference Number:
AIX-08-316936; EDB-77-122498
Resource Relation:
Journal Name: Sol. Phys.; (Netherlands); Journal Volume: 50:2
Subject:
71 CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS; CHROMOSPHERE; INTERFACES; SOLAR CORONA; SOLAR PROMINENCES; ELECTRON DENSITY; EMISSION SPECTRA; EXTREME ULTRAVIOLET RADIATION; LYMAN LINES; SKYLAB; SUN; ULTRAHIGH TEMPERATURE; ATMOSPHERES; ELECTROMAGNETIC RADIATION; RADIATIONS; SATELLITES; SOLAR ACTIVITY; SOLAR ATMOSPHERE; SPECTRA; STARS; ULTRAVIOLET RADIATION; 640104* - Astrophysics & Cosmology- Solar Phenomena
OSTI ID:
7221605
Country of Origin:
Netherlands
Language:
English
Other Identifying Numbers:
Journal ID: CODEN: SLPHA
Submitting Site:
INIS
Size:
Pages: 365-381
Announcement Date:

Journal Article:

Citation Formats

Orrall, F Q, and Schmahl, E J. Prominence-corona interface compared with the chromosphere-corona transition region. Netherlands: N. p., 1976. Web.
Orrall, F Q, & Schmahl, E J. Prominence-corona interface compared with the chromosphere-corona transition region. Netherlands.
Orrall, F Q, and Schmahl, E J. 1976. "Prominence-corona interface compared with the chromosphere-corona transition region." Netherlands.
@misc{etde_7221605,
title = {Prominence-corona interface compared with the chromosphere-corona transition region}
author = {Orrall, F Q, and Schmahl, E J}
abstractNote = {The intensities of 52 EUV emission lines from each of 9 hedgerow prominences observed at the limb with the Harvard experiment on ATM-Skylab have been compared with intensities from the interior of network cells at the center of the disk, in order to compare the prominence-corona (P-C) interface with the chromosphere-corona (C-C) transition region. The intensity ratio Isub(cell)/Isub(prominence) for each line varies systematically (in all of the prominences observed), with the temperature of formation of the line as approximately Tsup(-0.6). The density sensitive C III (formed at T approximately 9x10/sup 4/ K) line ratio Isub(lambda1175)/Isub(lambda977) implies an average density 1.3x10/sup 9/ electrons cm/sup -3/ in the P-C interface and approximately 4 times this value in the C-C transition of the cells. The total optical thickness at the head of the Lyman continuum is < approximately 10 in most of the prominences studied; in two of the prominences, however, the possibility that tau/sub 0/ is large cannot be rejected. Methods of analysis of these EUV data are developed assuming both a resolved and an unresolved internal prominence structure. Although the systematic differences between the P-C interface and the C-C transition are stressed, the similarities are probably more remarkable and may be a result of fine structure in the C-C transition.}
journal = {Sol. Phys.; (Netherlands)}
volume = {50:2}
journal type = {AC}
place = {Netherlands}
year = {1976}
month = {Nov}
}