Profile analysis of He I 6678 in beta Orionis: Rotation, macroturbulence, and He abundance

Details Profile analysis of He I 6678 in beta Orionis: Rotation, macroturbulence, and He abundance Profile analysis of He I 6678 in beta Orionis: Rotation, macroturbulence, and He abundance

Jun 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995pasj...47..307t&link_type=abstract

PASJ: Publications of the Astronomical Society of Japan (ISSN 0004-6264), vol. 47, no. 3, p. 307-316

Astronomy and Astrophysics

Astronomy

9

Abundance, B Stars, Helium, Line Spectra, Stellar Atmospheres, Stellar Rotation, Supergiant Stars, Turbulence, Velocity Distribution, Visible Spectrum, Angular Velocity, Fitting, Radial Velocity, Spectral Resolution, Spectrum Analysis

Scientific paper

We have analyzed the line profile of He I 6678 in a typical late-B supergiant, beta Ori, by using the multi-parameter fitting method, in order to investigate the macroscopic velocity fields and the abundance of helium in its atmosphere. It turned out that the projected rotational velocity could be successfully separated from the (radial-tangential) macroturbulence as nue sin i = 40 km/s and zetaRT = 43 km/s. The heliocentric radial velocity was determined to be Vr = +23 km/s. The resulting helium composition of log epsilonHe = 11.38 reconfirms the previously reported mild enrichment of this element, presumably due to the mixing of CNO-cycle products. From a consideration of angular-momentum conservation, the present rotational rate indicates that this star would have been rotating very rapidly (possibly at near the fastest rate) when it was on the main sequence, which may have played a significant role in the process of envelope mixing.

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