Hot star wind models with new solar abundances

Free access article

Issue		A&A Volume 464, Number 2, March III 2007


Page(s)		L17 - L20
Section		Letters
DOI		http://dx.doi.org/10.1051/0004-6361:20066775

A&A 464, L17-L20 (2007)
DOI: 10.1051/0004-6361:20066775

Letter

Hot star wind models with new solar abundances

J. Krticka¹ and J. Kubát²

¹ Ústav Teoretické Fyziky a Astrofyziky PrF MU, 611 37 Brno, Czech Republic
e-mail: krticka@physics.muni.cz
² Astronomický Ústav, Akademie Ved Ceské Republiky, 251 65 Ondrejov, Czech Republic

(Received 20 November 2006 / Accepted 11 January 2007 )

Abstract
We compare the hot-star wind models calculated by assuming older solar-abundance determination with models calculated using the recently published values derived from 3D hydrodynamical model atmospheres. We show that the use of new abundances with lower metallicity improves the agreement between wind observation and theory in several aspects. (1) The predicted wind mass-loss rates are lower by a factor of 0.76. This leads to better agreement with mass-loss rates derived from observational analysis that takes the clumping into account. (2) As a result of the lowering of mass-loss rates, there is better agreement between the predicted modified wind momentum-luminosity relationship and that derived from observational analysis that takes the clumping into account. (3) Both the lower mass fraction of heavier elements and lower mass-loss rates lead to a decrease in opacity in the X-ray region. This influences the prediction of the X-ray line profile shapes. (4) There is better agreement between predicted $\ion{P}{v}$ ionization fractions and those derived from observations.

Key words: stars: winds, outflows -- stars: mass-loss -- stars: early-type -- hydrodynamics

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