Astronomy and Astrophysics – Astrophysics
Scientific paper
Mar 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984a%26as...55..361r&link_type=abstract
Astronomy and Astrophysics Supplement Series (ISSN 0365-0138), vol. 55, March 1984, p. 361-369.
Astronomy and Astrophysics
Astrophysics
3
Abundance, O Stars, Stellar Spectra, Subdwarf Stars, Ultraviolet Spectra, Interstellar Extinction, Ions, Iue, Metallic Stars, Radial Velocity, Stellar Evolution, Stellar Mass Ejection
Scientific paper
The high and low resolution IUE spectra of four O subdwarfs (BD +75°325, BD +48°1777, BD +37°1977, BD +37°442) are analyzed. Line identification is given for the most abundant ions in the far ultraviolet. Fe V is by far the ion with the largest number of lines. Broad P Cygni profiles of the N V and C IV resonance doublets are observed in BD +37°442 and BD +37°1977, with terminal velocities of 2200 and 2300 km s-1 respectively. The N IV 1718 Å line presents an extended blue wing also arising in the winds of these stars. A low interstellar extinction (E(B-V) ≤ 0.05) is derived from the weakness of the 2200 Å i.s. band, and from the Lyα profile. Mean radial velocities are given for the photospheric and interstellar atomic species, and a high stellar velocity is found for the four stars, in agreement with the Population II nature of these objects.
Altamore Aldo
Rossi Luca
Viotti Roberto
No associations
LandOfFree
A comparative study of the ultraviolet spectrum of hot subdwarfs does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with A comparative study of the ultraviolet spectrum of hot subdwarfs, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and A comparative study of the ultraviolet spectrum of hot subdwarfs will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1036749