Carbon, nitrogen, and oxygen abundances in early B-type stars

Details Carbon, nitrogen, and oxygen abundances in early B-type stars Carbon, nitrogen, and oxygen abundances in early B-type stars

Mar 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...387..673g&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 387, March 10, 1992, p. 673-700. Research supported by Robert A. Welch Foun

Astronomy and Astrophysics

Astrophysics

379

Abundance, B Stars, Early Stars, Stellar Composition, Stellar Interiors, Stellar Rotation, Supergiant Stars, Carbon, Line Spectra, Nitrogen, Oxygen, Spectral Line Width, Stellar Spectra

Scientific paper

A survey of the C, N, and O abundances in a sample of early B-type stars which was undertaken to test the hypothesis of Liubimkov (1984) that CN-cycled material is mixed to the surfaces of these stars during their core hydrogen-burning phase. Equivalent widths of generally weak lines are obtained using high-signal-to-noise Reticon spectra of 39 stars in four spectral regions. Effective temperatures and gravities for these stars are derived. Projected rotational velocities are measured using a cross-correlation technique. Abundances are derived using LTE methods and non-LTE equivalent width calculations. He, C, N, and O abundances of the nonsupergiant stars in the sample are found to be very close to the values found for the Orion Nebula, with the notable exception of a few stars which show enhanced N, a signature of CN-cycled material. No compelling evidence for a systematic increase in N abundance with evolutonary age was found; thus Liubimkov's claim that mixing occurs generally in main-sequence B stars cannot be confirmed.

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