The Tarantula Massive Binary Monitoring - II. First SB2 orbital and spectroscopic analysis for the Wolf-Rayet binary R145

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Table 3

Comparison with best-fitting evolution tracks.

	BEC	BPASS
	QHE^a	Non-hom.	QHE^b	Binary^c

M_i,1 [M_⊙]	105 ± 20	100 ± 20	100 ± 20	120 ± 20
M_i,2 [M_⊙]	91 ± 15	90 ± 20	90 ± 20	80 ± 20
M_cur,1 [M_⊙]		48 ± 10	96	58
M_cur,2 [M_⊙]		52 ± 10	85	113
Age [Myr]	2.3 ± 0.4	3.1 ± 0.3	2.1 ± 0.4	2.8 ± 0.4
X_H,1 (mass fr.)	0.3 ± 0.1	0.1 ± 0.1	0.4 ± 0.1	0.1 ± 0.1
X_H,2 (mass fr.)		0.1 ± 0.1	0.5 ± 0.1	–
R_max,1 [R_⊙]	40	1500	20	–

Notes. Initial parameters and predictions of best-fitting evolution tracks calculated for single stars experiencing homogeneous/non-homogeneous evolution.

^(a)

QHE in the BEC tracks is reached via an initial rotation velocity of ≈ 350 km s^-1for both components, which best-reproduces the observables.

^(b)

These tracks are fully homogeneous a-priori; rotation is not accounted for in the BPASS tracks.

^(c)

The tracks are identical to the non-homogeneous tracks, but include mass-transfer. The initial period defining the best-fitting track is P_i = 100 d.

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