Issue |
A&A
Volume 454, Number 3, August II 2006
|
|
---|---|---|
Page(s) | 883 - 888 | |
Section | Stellar structure and evolution | |
DOI | https://doi.org/10.1051/0004-6361:20065109 | |
Published online | 17 July 2006 |
2-dimensional models of rapidly rotating stars
II. Hydrostatic and acoustic models with
1
Astronomy Unit, Queen Mary, University of London, Mile End Road, London E1 4NS, UK e-mail: I.W.Roxburgh@qmul.ac.uk
2
LESIA, Observatoire de Paris, Place Jules Janssen, 92195 Meudon Cedex, France
Received:
28
February
2006
Accepted:
23
April
2006
Aims.We show how to construct 2-dimensional models of rapidly rotating stars in hydrostatic equilibrium
for any , given the density
along any one angle
.
If the hydrogen abundance
is given on
then the adiabatic exponent
can
by determined, yielding a self consistent acoustic model that can be used to investigate the
oscillation properties of rapidly rotating stars.
Methods.The system of equations governing the hydrostatic structure is solved by iteration
using the method of characteristics and spectral expansion, subject to the condition that
on
.
is calculated from
the equation of state under the assumption that
and is constant
on surfaces of constant entropy. Alternatively
can be approximated by taking
X constant in the equation of state and equal to the surface value.
Results.Results are presented for an evolved main sequence star of with the angular
velocity a function only of radius
, evolved to a central hydrogen abundance
of
. The model is first calculated using a spherically averaged stellar evolution code,
where the averaged centrifugal force
is added to gravity. The resulting
are then used as input to determine the 2-dimensional model.
Conclusions.The procedure described here gives self consistent hydrostatic and acoustic models of rapidly
rotating stars for any .
Key words: stars: rotation / stars: evolution
© ESO, 2006
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