Radial velocities for different spectral lines of B and A supergiants in our Galaxy and in the Large Magellanic Cloud

Details Radial velocities for different spectral lines of B and A supergiants in our Galaxy and in the Large Magellanic Cloud Radial velocities for different spectral lines of B and A supergiants in our Galaxy and in the Large Magellanic Cloud

Jul 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981a%26as...45..121k&link_type=abstract

Astronomy and Astrophysics Supplement Series, vol. 45, July 1981, p. 121-128. Research supported by the Comite Inter-Unions de

Astronomy and Astrophysics

Astrophysics

1

Early Stars, Magellanic Clouds, Milky Way Galaxy, Radial Velocity, Stellar Spectra, Supergiant Stars, A Stars, B Stars, Balmer Series, H Lines, Stellar Luminosity, Stellar Spectrophotometry, Stellar Structure

Scientific paper

Coudé spectra of 23 early-type supergiants (16 of them belong to our Galaxy and 7 to the Large Magellanic Cloud (LMC)) were measured to study the radial velocities of all metallic and non-metallic lines in relation to their EP + IP (high excitation + ionization potential).
The identified elements of the spectra do not show any systematic dependence (gradient) of the radial velocities on EP + IP in the range of 3 eV to 38 eV except the hydrogen lines, for the stars exhibiting Balmer radial velocity progression. The Balmer progression, always positive, is stronger and more frequent in the LMC supergiants, which happen to be the most luminous among the stars of our sample.
Stars with more than one spectrum available show mean radial velocity and Balmer progression variability with time.

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