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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Volume 499 / No 1 (May III 2009)

A&A, 499 1 (2009) 257-266

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Table 3:

Same as Table 2, but for the best-fit model for PG 1707+427 ( $M_*= 0.542~M_{\odot}$ , $T_{\rm eff}= 89~504$ K, $\log(L_*/L_{\odot}) = 1.40$ ). The observed periods are taken from Kawaler et al. (2004).
$\Pi_i^{\rm O}$	$\Pi_k^{\rm T}$	k	$\dot{\Pi}^{\rm T}_k$	Unstable
334.62	333.26	12	2.13	yes
--	355.73	13	1.19	yes
--	378.53	14	2.17	yes
--	401.64	15	1.51	yes
--	423.68	16	1.84	yes
448.07	447.31	17	2.46	yes
--	469.26	18	1.49	yes
494.39	492.56	19	2.76	yes
--	516.50	20	2.61	yes
536.41	537.67	21	1.66	yes
--	562.32	22	3.30	yes
--	584.78	23	2.37	yes
--	606.62	24	2.73	yes
--	632.11	25	3.25	yes
--	653.15	26	2.99	yes
677.89	677.38	27	3.43	yes
--	701.20	28	3.03	yes
726.02	722.82	29	3.95	no
745.78	747.58	30	3.42	no
--	770.93	31	3.71	no
--	793.13	32	4.45	no
--	817.86	33	3.61	no
--	841.70	34	4.64	no
--	863.34	35	3.91	no
--	888.59	36	5.03	no
909.05	912.34	37	4.21	no

Source LaTeX | All tables | In the text

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