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Title: MgII h and k lines in the cepheid Beta Doradus

Abstract

We have obtained spectral scans of the Cepheid ..beta.. Doradus in the region of the MgII k line using the Copernicus satellite. Identifications are given for absorption lines and the MgII emission line fluxes are estimated. The emission strength is similar to that in nonvariable stars except at two phases during declining light when it is enhanced significantly. The MgII emission thus occurs at a different part of the cycle than the CaII emission. We speculate on the possible reason for this phenomenon.

Authors:
;
Publication Date:
Research Org.:
Department of Physics and Astronomy, University of Nebraska--Lincoln, Lincoln, Nebraska 68588
OSTI Identifier:
6775207
Alternate Identifier(s):
OSTI ID: 6775207
Resource Type:
Journal Article
Journal Name:
Astron. J.; (United States)
Additional Journal Information:
Journal Volume: 84:2
Country of Publication:
United States
Language:
English
Subject:
71 CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS; CALCIUM IONS; COSMOCHEMISTRY; CEPHEIDS; MAGNESIUM IONS; ABSORPTION SPECTRA; CHROMOSPHERE; EMISSION SPECTRA; LUMINOSITY; MAIN SEQUENCE STARS; SHOCK WAVES; STELLAR ATMOSPHERES; ATMOSPHERES; ATOMIC IONS; CHARGED PARTICLES; CHEMISTRY; IONS; OPTICAL PROPERTIES; PHYSICAL PROPERTIES; PULSATING VARIABLE STARS; SOLAR ATMOSPHERE; SPECTRA; STARS; VARIABLE STARS 640102* -- Astrophysics & Cosmology-- Stars & Quasi-Stellar, Radio & X-Ray Sources

Citation Formats

Schmidt, E.G., and Weiler, E.J. MgII h and k lines in the cepheid Beta Doradus. United States: N. p., 1979. Web.
Schmidt, E.G., & Weiler, E.J. MgII h and k lines in the cepheid Beta Doradus. United States.
Schmidt, E.G., and Weiler, E.J. Thu . "MgII h and k lines in the cepheid Beta Doradus". United States.
@article{osti_6775207,
title = {MgII h and k lines in the cepheid Beta Doradus},
author = {Schmidt, E.G. and Weiler, E.J.},
abstractNote = {We have obtained spectral scans of the Cepheid ..beta.. Doradus in the region of the MgII k line using the Copernicus satellite. Identifications are given for absorption lines and the MgII emission line fluxes are estimated. The emission strength is similar to that in nonvariable stars except at two phases during declining light when it is enhanced significantly. The MgII emission thus occurs at a different part of the cycle than the CaII emission. We speculate on the possible reason for this phenomenon.},
doi = {},
journal = {Astron. J.; (United States)},
number = ,
volume = 84:2,
place = {United States},
year = {1979},
month = {2}
}