The theoretical near ultraviolet spectrum of B type stars

Details The theoretical near ultraviolet spectrum of B type stars The theoretical near ultraviolet spectrum of B type stars

Apr 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976a%26a....48..173b&link_type=abstract

Astronomy and Astrophysics, vol. 48, no. 2, Apr. 1976, p. 173-185. Research supported by the Fonds de la Recherche Fondamentale

Astronomy and Astrophysics

Astrophysics

15

B Stars, Near Ultraviolet Radiation, Stellar Atmospheres, Stellar Spectra, Ultraviolet Spectra, Brightness Temperature, Line Spectra, Main Sequence Stars, Stellar Models

Scientific paper

Theoretical spectra are computed for a grid of stellar model atmospheres with effective temperatures from 10,000 to 30,000 K and log g from 2.5 to 4 in three wavelength regions: 2060-2160 A, 2495-2595 A, 2770-2870 A. The results show good agreement with S 59 observations. Line identifications are given; most of the spectral features in the 2100-A region are due to lines of doubly ionized metals, the feature of 2140 A and those in the 2500-A and 2800-A regions are mainly due to lines of singly ionized metals. Line-blocking factors are determined in each 10-A-wide interval; the line blocking in the 2100-A regions shows a maximum at 20,000 to 25,000 K. The line blocking in the 2500-A and 2800-A regions decreases from 10,000 K to 30,000 K. Lines of singly ionized elements are insensitive to gravity around 16,000 K; lines of doubly ionized elements, around 25,000 K. The microturbulent velocity is certainly much lower than 4 km/s in main-sequence B stars cooler than 20,000 K.

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