Asteroseismology of hot pre-white dwarf stars: the case of the DOV stars PG 2131+066 and PG 1707+427, and the PNNV star NGC 1501

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Table 2:

Observed and theoretical ( $\ell =1$ ) periods of the best-fit model for PG 2131+066 ( $M_*= 0.589~M_{\odot}$ , $T_{\rm eff}= 102~179$ K, $\log(L_*/L_{\odot}) = 1.57$ ). Periods are in seconds and rates of period change (theoretical) are in units of 10^-12 s/s. The observed periods are taken from Kawaler et al. (1995).
$\Pi_i^{\rm O}$	$\Pi_k^{\rm T}$	k	$\dot{\Pi}^{\rm T}_k$	Unstable
341.45	341.88	14	2.04	yes
--	363.66	15	3.90	yes
384.27	383.94	16	2.60	yes
403.93	403.30	17	3.30	yes
426.36	426.48	18	4.14	yes
450.28	445.31	19	2.89	yes
462.39	465.91	20	4.53	yes
--	488.81	21	4.11	no
507.91	507.91	22	3.79	no

Source LaTeX | All tables | In the text

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