Asteroseismology of the DOV star PG 1159-035. (arXiv:1907.01137v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Chen_Y/0/1/0/all/0/1">Yanhui Chen</a>
Grids of DOV star models are evolved by texttt{WDEC} with fixed atmospheric
constituent to the spectral values of $X_{C}/X_{He}/X_{O}$ = 50/33/17. The core
compositions are from white dwarf models at highest $T_{eff}$ evolved by
texttt{MESA}. The eigenfrequencies are calculated and used to fit the observed
modes. Based on 264.1 hours of photometric observations on PG 1159-035, Winget
et al. identified 125 individual frequencies. Costa et al. identified 198
pulsation modes for PG 1159-035 according to the WET photometric data from
1983, 1985, 1989, and 2002. Both of them derived frequency splitting values of
$deltasigma_{l=1}$ $sim$ 4.2,$mu$Hz and $deltasigma_{l=2}$ $sim$
6.9,$mu$Hz. According to the values of $deltasigma_{l=1}$ and
$deltasigma_{l=2}$, 20 triplets and 9 quintuplets are selected and used to
constrain the fitting models. Our optimal model has $T_{eff}$ = 129000,K,
$M_{*}$ = 0.63,$M_{odot}$, log$g$ = 7.59, log($M_{rm env}/M_{*}$) = -5.0,
and $sigma_{RMS}$ = 1.97,s. The values of $T_{eff}$ and log$g$ are consistent
with that values of C’orsico et al.. The calculated modes of minimum rate of
period change correspond to modes with maximum kinetic energy distributed in
the envelope. The observed rates of period change with positive and negative
values can also be partially reproduced. In particular, there are negative
rates of period change for the calculated modes from our optimal model, which
is not found in previous work.
Grids of DOV star models are evolved by texttt{WDEC} with fixed atmospheric
constituent to the spectral values of $X_{C}/X_{He}/X_{O}$ = 50/33/17. The core
compositions are from white dwarf models at highest $T_{eff}$ evolved by
texttt{MESA}. The eigenfrequencies are calculated and used to fit the observed
modes. Based on 264.1 hours of photometric observations on PG 1159-035, Winget
et al. identified 125 individual frequencies. Costa et al. identified 198
pulsation modes for PG 1159-035 according to the WET photometric data from
1983, 1985, 1989, and 2002. Both of them derived frequency splitting values of
$deltasigma_{l=1}$ $sim$ 4.2,$mu$Hz and $deltasigma_{l=2}$ $sim$
6.9,$mu$Hz. According to the values of $deltasigma_{l=1}$ and
$deltasigma_{l=2}$, 20 triplets and 9 quintuplets are selected and used to
constrain the fitting models. Our optimal model has $T_{eff}$ = 129000,K,
$M_{*}$ = 0.63,$M_{odot}$, log$g$ = 7.59, log($M_{rm env}/M_{*}$) = -5.0,
and $sigma_{RMS}$ = 1.97,s. The values of $T_{eff}$ and log$g$ are consistent
with that values of C’orsico et al.. The calculated modes of minimum rate of
period change correspond to modes with maximum kinetic energy distributed in
the envelope. The observed rates of period change with positive and negative
values can also be partially reproduced. In particular, there are negative
rates of period change for the calculated modes from our optimal model, which
is not found in previous work.
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