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)
· On-line Data
· References in the article
· Citations to the Article (145) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (16)
· Associated Articles
· Reads History
· Translate This Page
Outer atmospheres of cool stars. XII - A survey of IUE ultraviolet emission line spectra of cool dwarf stars
Linsky, J. L.; Bornmann, P. L.; Carpenter, K. G.; Wing, R. F.; Giampapa, M. S.; Worden, S. P.; Hege, E. K.
AA(Joint Institute for Laboratory Astrophysics, Boulder, CO), AB(Joint Institute for Laboratory Astrophysics, Boulder, CO), AC(Ohio State University, Columbus, OH), AD(Steward Observatory, Tucson, AZ)
Astrophysical Journal, Part 1, vol. 260, Sept. 15, 1982, p. 670-694. (ApJ Homepage)
Publication Date:
NASA/STI Keywords:
Cool Stars, Dwarf Stars, Late Stars, Line Spectra, Stellar Atmospheres, Stellar Luminosity, Ultraviolet Spectra, Chromosphere, Iue, M Stars, Photometry, Spectrum Analysis, Stellar Flares, Stellar Magnetic Fields
Bibliographic Code:


Quantitative information is obtained on the chromospheres and transition regions of M dwarf stars, in order to determine how the outer atmospheres of dMe stars differ from dM stars and how they compare with the outer atmospheres of quiet and active G and K type dwarfs. IUE spectra of six dMe and four dM stars, together with ground-based photometry and spectroscopy of the Balmer and Ca II H and K lines, show no evidence of flares. It is concluded, regarding the quiescent behavior of these stars, that emission-line spectra resemble that of the sun and contain emission lines formed in regions with 4000-20,000 K temperatures that are presumably analogous to the solar chromosphere, as well as regions with temperatures of 20,000-200,000 K that are presumably analogous to the solar transition region. Emission-line surface fluxes are proportional to the emission measure over the range of temperatures at which the lines are formed.

Associated Articles

Part  1     Part  2     Part  3     Part  4     Part  6     Part  5     Part  7     Part  9     Part  8     Part 10     Part 11     Part 12     Part 13     Part 14     Part 15    

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)

Find Similar Abstracts:

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