SpringerLink
Forum Springer Astron. Astrophys.
Forum Whats New Search Orders


Astron. Astrophys. 329, 613-623 (1998)


Table of Contents
Available formats: HTML | PDF | (gzipped) PostScript

Helium enhancements in luminous OB-type stars:
the effect of microturbulence*

N.D. McErlean 1, D.J. Lennon 2 and P.L. Dufton 1

1 The Department of Pure and Applied Physics, The Queen's University of Belfast, Belfast BT7 1NN, Northern Ireland
2 Institut für Astronomie und Astrophysik der Universität München, Scheinerstrasse 1, D-81679 München, Germany

Received 14 July 1997 / Accepted 28 August 1997

Abstract

We present non-LTE analyses of high quality spectra for two B-type supergiants, [FORMULA]  Orionis & [FORMULA]  Orionis (spectral types B0.5 Ia & B0 Ia respectively). We investigate the effect of including a microturbulent velocity in the H I, He II and He I line broadening on the derived stellar atmospheric parameters ([FORMULA], [FORMULA] and y). Its inclusion has a significant effect on the profiles of the lines of neutral helium and leads to approximately normal estimates for the helium fractional abundances for both supergiants. By contrast, adopting zero microturbulence implies significant helium overabundances, if we adopt the mean abundance of all the lines considered here. The He I lines at 4437, 4387 and 5047Å are found to be rather insensitive to microturbulence and hence are more reliable indicators of helium abundance. There are some remaining unresolved discrepancies, such as a systematic difference between singlet and triplet transitions which we attribute to the neglect of line blocking, while the 5015Å 21 S - 31 P transition remains much stronger than predicted. This latter problem we tentatively attribute to the neglect of sphericity; the generalized dilution effect discussed by Voels et al. (1989). We suggest that a judicious choice of He I lines, and the use of an appropriate microturbulent velocity, may contribute to resolving the `helium discrepancy' in O-type stars. The question of the origin of a perceived microturbulence in supergiants is also briefly discussed in the context of stellar winds.

That two normal supergiants have close to solar helium abundances clearly implies that they have not undergone dredge-up in a previous red supergiant phase of evolution, supporting the contention that massive stars do not perform blue loops in the HR diagram at solar metallicity. Marginal evidence for a mild helium overabundance in [FORMULA] Ori however could be interpreted as being due to mixing processes, perhaps during its main sequence lifetime.

Key words: stars: atmospheres – stars: early-type – stars: evolution – stars: supergiants

* Based on Observations collected at the European Southern Observatory, La Silla, Chile

Send offprint requests to: N.McErlean@qub.ac.uk

© European Southern Observatory (ESO) 1998

Online publication: December 8, 1997
helpdesk.link@springer.de