Evolution of long-lived globular cluster stars - IV. Initial helium content and white-dwarf properties

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Volume 602 (June 2017)

A&A, 602 (2017) A13

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Table 1

Age at the end of the core He-burning phase (Gyr), except for the cases at [Fe/H] = –0.5 and 0.0, where the age at the highest luminosity of the RGB phase is shown, for the 0.8 M_⊙ as a function of the initial helium content Y_ini at different metallicities [Fe/H].


[Fe/H]	Y_ini	τ_endHeb	First TP		# TP	Post-AGB
Z			M_tot	M_core		M_core


–2.2	0.248	13.84	0.60	0.48	7	0.57
0.0002	0.400	5.27	0.68	0.52	22	0.67


–1.75	0.248	14.29	0.57	0.47	8	0.54
0.0005	0.260	13.18	0.58	0.47	8	0.55
	0.270	12.34	0.59	0.47	8	0.57
	0.300	10.35	0.61	0.48	11	0.59
	0.330	8.55	0.63	0.49	13	0.61
	0.370	6.59	0.65	0.51	16	0.63
	0.400	5.40	0.66	0.53	18	0.64
	0.425	4.56	0.67	0.55	20	0.66
	0.450	3.84	0.68	0.57	21	0.67
	0.475	3.23	0.69	0.60	21	0.68
	0.525	2.26	0.71	0.64	20	0.70
	0.600	1.31	0.73	0.71	12	0.72
	0.800	0.26	–	–	0	0.74


–1.15	0.249	16.44	–	–	HF	0.50
0.002	0.270	14.39	0.51	0.46	2	0.51


–0.5	0.255	23.27	–	–	He-WD	0.47
0.008


0.0	0.276	25.58	–	–	He-WD	0.46
0.017

Notes. The M_tot and M_core (M_⊙) at the first TP, number of TPs and M_core on the post-AGB phase at the maximum T_eff. For each metallicity, the first Y_ini corresponds to the canonical value of helium; HF stands for hot flasher and when the star does not end its life as a CO-WD (when no indication is given) then He-WD is specified.

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