Clues about the scarcity of stripped-envelope stars from the evolutionary state of the sdO+Be binary system φ Persei

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Volume 615 (July 2018)

A&A, 615 (2018) A30

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Table 3

Observed parameters of HeGBs.





	M_SES	T_{eff SES}	logL_SES	logg_SES	M_acc	T_{eff acc}	logL_acc	P_orb	R_SES∕R_acc
	[M_⊙]	[kK]	[L_⊙]		[M_⊙]	[kK]	[L_⊙]	[d]




Be+sdO:
φ Persei	1.2 ± 0.2^a	53 ± 3^a		4.2 ± 0.1^a	9.3 ± 0.3^a	29.3 ± 4.0^a		126.7^a	0.20 ± 0.01^a




FY CMa	1.3 ± 0.2^b	45 ± 5^b		4.3 ± 0.6^b	11.5 ± 1.5^b	27.5 ± 3.0^b		37.3^b	0.12 ± 0.04^b




59 Cyg	0.77 ± 0.15^c	52 ± 5^c		5.0 ± 1.0^c	7.8 ± 1.5^c	21.8 ± 0.7^c		28.2^c	0.062 ± 0.003^c
60 Cyg	1.7^d	42 ± 4^d			11.8^d	27^d		146.6^d	0.093 ± 0.012^d
HR 2142	0.7^e	≥43 ± 5^e	>1.7^e		9^e			80.9^e	>0.026^e




HeGBs:
KS Per	1^f	9.5 ± 0.4^g	3.3^g	2.0 ± 0.5^g	5–6^f	30^h		362.2ⁱ
υ SGR^*	2.52 ± 0.10^j	12.3 ± 0.2^k	4.6^j, 3.7^k	2.5 ± 0.5^k	4.05 ± 0.05^j			138^l
LSS 4300	1^m	12 ± 1ⁿ	4^m	1.4^m				51.1^l
LSS 1922		12 ± 0.5ⁿ
BI Lyn	0.5^o	28.6 ± 1.0^o	3.32^o	3.6 ± 0.1^o		5.9 ± 1.0^o




qWR+B:
HD 45166	4.2 ± 0.7^p	50 ± 2^p			4.8 ± 0.5^p	13.5^p		1.6^p

Notes. The helium giant is labeled “HeG”; the companion star is labeled “c”. We display the most recently published values (to our knowledge). Values without errors are estimates. The letters in superscript refer to the studies where the values are adopted from (or references therein): ^(a)Mourard et al. (2015), ^(b)Peters et al. (2008), ^(c)Peters et al. (2013), ^(d)Wang et al. (2017), ^(e)Peters et al. (2016), ^(f)Drilling & Schoenberner (1982), ^(g)Kipper & Klochkova (2008), ^(h)Parthasarathy et al. (1990), ⁽ⁱ⁾Margoni et al. (1988), ^(j)Dudley & Jeffery (1990), ^(k)Kipper & Klochkova (2012), ^(l)Frame et al. (1995), ^(m)Schoenberner & Drilling (1984), ⁽ⁿ⁾Dudley & Jeffery (1993), ^(o)Jeffery & Aznar Cuadrado (2001), ^(p)Groh et al. (2008). Systems that are starred^⋆ should have their masses divided by sin³i. The typically tiny errors on the orbital period are omitted.

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