All Tables
- Table 1:
The values of the stellar mass (in
)
from spectroscopic
and asteroseismic studies, and the values obtained in this work from three
different methods.
- Table 2:
Comparison between the observed periods of
PG 1159-035 (taken from KB94) and the theoretical (
)
periods of the
best-fit model (
s,
s).
- Table 3:
Comparison between the observed periods
of PG 2131+066 (taken from Kawaler et al. 1995)
and the theoretical (
)
periods of the
best-fit model (
s,
s).
- Table 4:
Comparison between the observed periods
of PG 1707+427 (taken from Kawaler et al. 2004) and
the theoretical (
)
periods of the best-fit model
(
s,
s).
- Table 5:
Comparison between the observed periods
of PG 0122+200 (taken from Vauclair et al. 2001) and the
theoretical (
)
periods of the best-fit model
(
s,
s).
- Table 6:
Summary of the seismic inferences for PG 1159-035,
PG 2131+066, PG 1707+427 and PG 0122+200 from
period fits.
The values of the observed mean period spacing were extracted from Table 6 of Kawaler et al. (2004).