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The abundance anomalies in a rotationally evolved 20 M⊙ OBN star model

Published online by Cambridge University Press:  26 May 2016

D. Eryurt ,
H. Kirbiyik ,
N. Kizilouǧlu ,
R. Cİvėlek  and
A. Weiss
D. Eryurt
Affiliation:
Middle East Technical University, Physics Department 06531 Ankara, Turkey
H. Kirbiyik
Affiliation:
Middle East Technical University, Physics Department 06531 Ankara, Turkey
N. Kizilouǧlu
Affiliation:
Middle East Technical University, Physics Department 06531 Ankara, Turkey
R. Cİvėlek
Affiliation:
Middle East Technical University, Physics Department 06531 Ankara, Turkey
A. Weiss
Affiliation:
Max-Planck-Institut für Physik und Astrophysik, Garching, Germany

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Walborn (1970, 1971) observationally found that OB stars showed nitrogen and carbon abundance anomalies in their atmospheres. Schönberner et al. (1988) found that OBN stars had helium enriched atmospheres. Several different suggestions have been made so far to explain the abundance anomalies in these stars (Paczynski 1973; Walborn 1976; Bolton and Rogers 1978). Maeder (1987) and Weiss et al. (1988) call attention to some possible effects of rotation in mixing chemical elements in Wolf-Rayet stars and B-supergiant stars respectively. They suggested that rotational mixing could explain the high He/H ratios and the high N/C and N/O ratios in the progenitor of 1987A Supernova. Saio et al. (1988) in an attempt to explain the nitrogen and helium enhancement in the progenitor of SN 1987A invoked extensive mixing in their models. They pointed out that such an effective mixing may be produced by rapid rotation. Such observations and ideas were the motivation for the present study.

Type
1. Pulsation and Rotation
Information
Symposium - International Astronomical Union , Volume 162: Pulsation, Rotation and Mass Loss in Early-Type Stars , 1994 , pp. 149 - 150
Copyright
Copyright © Kluwer 1994 

References

Allen, D.A., Meikle, W.P.S., Spyromillio, J., 1989, Nature , 342, 403 Google Scholar
Bolton, C.T., Rogers, G.L., 1978, ApJ. , 222, 234 Google Scholar
Fransson, C., 1989, ApJ , 336, 429 Google Scholar
Maeder, A., 1987, A& A , 178, 159 Google Scholar
Paczynski, B., 1973, Acta Astr. , 23, 191 Google Scholar
Panagia, N., et al., 1987, IAU Circ. , 4514.Google Scholar
Saio, H., Nomoto, K., Kato, M., 1988, Nature , 334, 508 Google Scholar
Schönberner, D., Herrero, A., Becker, S., et al., 1988, A& A , 197, 209 Google Scholar
Walborn, N.R., 1970, ApJ , 161, L149 Google Scholar
Walborn, N.R., 1971, ApJ , 164, L67 Google Scholar
Walborn, N.R., 1976, ApJ , 205, L419 Google Scholar
Walborn, N.R., 1988, Atmospheric diagnostics of stellar evolution., In: Nomoto, K. (ed.), Proc. IAU Collowq. , 108. Springer, Berlin, pp. 70–78 Google Scholar
Weiss, A., Hillebrandt, W., Truran, J.W., 1988, A& A , 197, L11 Hauck, B., Maeder, A., (eds.) p. 253 Google Scholar