Hot star wind models with new solar abundances
Jiri Krticka (1), Jiri Kubat (2)
(1) Ustav teoreticke fyziky a astrofyziky PrF MU, CZ-611 37 Brno, Czech Republic
(2) Astronomicky ustav, Akademie ved Ceske republiky, CZ-251 65 Ondrejov, Czech Republic
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 PV ionization fractions and those derived
from observations.
Reference: A&A Letters
Status: Manuscript has been accepted
Weblink: http://xxx.lanl.gov/abs/astro-ph/0701411
Comments:
Email: krticka@physics.muni.cz