Pulsating low-mass white dwarfs in the frame of new evolutionary sequences - VI. Thin H-envelope sequences and asteroseismology of ELMV stars revisited

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Volume 620 (December 2018)

A&A, 620 (2018) A196

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Table 1.

Stellar masses of our set of low-mass He-core WD models (Col. 1) and the H content associated with different thicknesses of the envelope adopted for each stellar mass (T_eff ∼ 8000 K).

M_⋆/M_⊙	log(M_H/M_⋆)	log(M_H/M_⋆)	log(M_H/M_⋆)	log(M_H/M_⋆)	log(M_H/M_⋆)	log(M_H/M_⋆)	log(M_H/M_⋆)
0.1554	−1.69	−2.50	−3.00	−3.72	−4.37	−5.02	−5.20
0.1612	−1.76	−2.49	−3.00	−3.70	−4.35	−5.04	−5.23
0.1650	−1.82	−2.50	−3.01	−3.69	−4.35	−5.06	−5.28
0.1706	−1.89	−2.50	−3.01	−3.69	−4.39	−5.13	−5.32
0.1762	−1.95	−2.50	−3.00	−3.66	−4.34	−5.14	−5.43
0.1805	−2.44	−	−3.00	−3.65	−4.33	−5.17	−5.51
0.1869	−2.37	−	−2.99	−3.64	−4.32	−5.19	−5.61
0.1921	−2.35	−	−3.02	−3.62	−4.30	−5.17	−5.58
0.2025	−2.43	−	−3.00	−3.61	−4.30	−5.20	−5.62
0.2390	−2.45	−	−3.04	−3.67	−4.28	−5.15	−5.58
0.2707	−2.96	−	−	−3.67	−4.32	−5.19	−5.54
0.3205	−2.81	−	−	−3.60	−4.30	−5.08	−5.54
0.3624	−3.10	−	−	−3.62	−4.32	−5.15	−5.64
0.4352	−3.21	−	−	−3.71	−4.32	−5.14	−5.79

Notes. Column 2 indicates the upper limit of the H-envelope thickness (“canonical envelope”) for each stellar mass as given by our fully evolutionary computations that assume that mass loss proceeds via stable Roche lobe overflow.

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