Exploring the boundary between stable mass transfer and L2 overflow in close binary evolution

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Volume 691 (November 2024)

A&A, 691 (2024) A174

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Table 3.

Mass estimates and orbital parameters of the four WR+O systems in the SMC.

	AB 3	AB 6	AB 7	AB 8
P_orb/ d	10.053(5) ^(f)	6.5384(4) ^(g)	19.5600(5) ^(h)	16.633(9) ⁽ⁱ⁾
q^ΔRV	–^(f)	2.23(9) ^(g)	1.94(6) ^(h)	2.85(20) ⁽ⁱ⁾
M_WR^lum/ M_⊙^(a)	$29_{- 2}^{+ 2}$ $29^{+2}_{-2}$	$26_{- 5}^{+ 7}$ $26^{+7}_{-5}$	$37_{- 5}^{+ 6}$ $37^{+6}_{-5}$	$40_{- 6}^{+ 7}$ $40^{+7}_{-6}$
$M_{WR}^{d X / d Q} / M_{⊙}$ $M_{\mathrm{WR}}^{\mathrm{d}X/\mathrm{d}Q}/\,M_\odot$ ^(b)	28	20…30 ^(c)	34	–
X_H, WR^(d)	0.25(5)	0.25(5)	0.15(5)	0^+0.15
M_O^SpT/ M_⊙^(d)	$20_{- 5}^{+ 20}$ $20^{+20}_{-5}$	$41_{- 10}^{+ 10}$ $41^{+10}_{-10}$	$44_{- 9}^{+ 26}$ $44^{+26}_{-9}$	$61_{- 25}^{+ 14}$ $61^{+14}_{-25}$
M_O^gr/ M_⊙^(d)	$13_{- 10}^{+ 70}$ $13^{+70}_{-10}$	$61_{- 30}^{+ 60}$ $61^{+60}_{-30}$	$30_{- 19}^{+ 55}$ $30^{+55}_{-19}$	$70_{- 52}^{+ 210}$ $70^{+210}_{-52}$
M_1i^lum/ M_⊙^(e)	$50_{- 5}^{+ 5}$ $50^{+5}_{-5}$	$47_{- 7}^{+ 10}$ $47^{+10}_{-7}$	$65_{- 10}^{+ 10}$ $65^{+10}_{-10}$	$80_{- 15}^{+ 15}$ $80^{+15}_{-15}$
$M_{1 i}^{SpT \land Δ RV} / M_{⊙}$ $M_{\mathrm{1i}}^{\mathrm{SpT} \wedge \Delta \mathrm{RV}}/\,M_\odot$ ^(e)	–	$35_{- 5}^{+ 5}$ $35^{+5}_{-5}$	$45_{- 7}^{+ 20}$ $45^{+20}_{-7}$	$47_{- 15}^{+ 8}$ $47^{+8}_{-15}$
$M_{1 i}^{gr \land Δ RV} / M_{⊙}$ $M_{\mathrm{1i}}^{\mathrm{gr} \wedge \Delta \mathrm{RV}}/\,M_\odot$ ^(e)	–	$50_{- 20}^{+ 40}$ $50^{+40}_{-20}$	$32_{- 15}^{+ 43}$ $32^{+43}_{-15}$	$50_{- 30}^{+ ?}$ $50^{+?}_{-30}$

Notes. The superscript indicates the method on which the mass estimate is based (ΔRV = radial velocity variation, lum = luminosity, dX/dQ = hydrogen gradient, SpT = spectral type, gr = surface gravity).

^(a)

Shenar et al. (2016, 2018) using the mass-luminosity relation from Gräfener et al. (2011).

^(b)

Schootemeijer & Langer (2018), since their method requires X_H, WR > 0, no mass could be determined for AB 8.

^(c)

Schootemeijer (priv. comm.).

^(d)

Shenar et al. (2016, 2018).

^(e)

Based on M_WR^lum/ M_⊙, X_H, WR and the profiles of Schootemeijer et al. (2019). The mass for AB 8 is a lower limit.

^(f)

Foellmi et al. (2003), no mass ratio could be determined.

^(g)

Shenar et al. (2018).

^(h)

Niemela et al. (2002).

⁽ⁱ⁾

Bartzakos et al. (2001), St-Louis et al. (2005).

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