Reference : Instability strips of slowly pulsating B stars and beta Cephei stars: the effect of t...
Scientific journals : Article
Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics
http://hdl.handle.net/2268/75393
Instability strips of slowly pulsating B stars and beta Cephei stars: the effect of the updated OP opacities and of the metal mixture
English
Miglio, Andrea mailto [Université de Liège - ULiège > Département d'astrophys., géophysique et océanographie (AGO) > Evol. et stabilité des étoiles et des amas d'étoiles (ESEA) >]
Montalban Iglesias, Josefa [Institut d'Astrophysique et de Géophysique de l'Université de Liège, Allée du 6 Août, 17 B-4000 Liège, Belgium]
Dupret, Marc-Antoine [Université de Liège - ULiège > Département d'astrophys., géophysique et océanographie (AGO) > Astrophysique stellaire théorique >]
1-Feb-2007
Monthly Notices of the Royal Astronomical Society
Blackwell Publishing
375
L21-L25
Yes (verified by ORBi)
International
0035-8711
1365-2966
Oxford
United Kingdom
[en] radiative transfer ; stars: abundances ; stars: early-type ; stars: interiors ; stars: oscillations ; stars: variables: other
[en] The discovery of beta Cephei stars in low-metallicity environments, as well as the difficulty in theoretically explaining the excitation of the pulsation modes observed in some beta Cephei and hybrid slowly pulsating B-beta Cephei pulsators, suggest that the `iron opacity bump' provided by stellar models could be underestimated. We analyze the effect of uncertainties in the opacity computations and in the solar metal mixture on the excitation of pulsation modes in B-type stars. We carry out a pulsational stability analysis for four grids of main-sequence models with masses between 2.5 and 12M[SUB]solar[/SUB] computed with OPAL and OP opacity tables and two different metal mixtures. We find that in a typical beta Cephei model the OP opacity is 25 per cent larger than OPAL in the region where the driving of pulsation modes occurs. Furthermore, the difference in the Fe mass fraction between the two metal mixtures considered is of the order of 20 per cent. The implication on the excitation of pulsation modes is non-negligible: the blue border of the slowly pulsating B star (SPB) instability strip is displaced at higher effective temperatures, leading to a larger number of models being hybrid SPB-beta Cephei pulsators. Moreover, higher overtone p-modes are excited in beta Cephei models and unstable modes are found in a larger number of models for lower metallicities, in particular beta Cephei pulsations are also found in models with Z = 0.01.
http://hdl.handle.net/2268/75393
10.1111/j.1745-3933.2006.00267.x
http://adsabs.harvard.edu/abs/2007MNRAS.375L..21M
http://de.arxiv.org/abs/astro-ph/0610789

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