Table 2.
Semi-detached double-lined eclipsing binaries observed in the Galaxy with at least one component exceeding 8 M⊙.
| Name | Period | Ma | Md | q | Ra | Rd | Ta | Td | References |
|---|---|---|---|---|---|---|---|---|---|
| (d) | (M⊙) | (M⊙) | (R⊙) | (R⊙) | (kK) | (kK) | (#) | ||
| TT Aur | 1.33 | 8.10 | 5.40 | 1.50 | 3.90 | 4.20 | 24.8 | 18.2 | [1] |
| μ1 Sco | 1.44 | 8.30 ± 1.00 | 4.60 ± 1.00 | 1.80 | 3.90 ± 0.30 | 4.60 ± 0.40 | 24.0 ± 1.0 | 17.0 ± 0.7 | [2] |
| SV Gem | 4.00 | 8.34 | 3.37 | 2.47 | 4.87 | 6.70 | [3] | ||
| V454 Cyg | 2.31 | 8.40 | 2.86 | 2.93 | 4.99 | 4.64 | [1] | ||
| BF Cen | 3.69 | 8.70 | 3.80 | 2.29 | 5.10 | 7.10 | 12.9 | 9.4 | [1] |
| BM Ori | 6.47 | 9.50 | 3.51 | 2.70 | 4.47 | 8.94 | [3] | ||
| IZ Per | 3.68 | 9.97 ± 0.55 | 3.20 ± 0.17 | 3.11 | 7.51 ± 0.13 | 6.90 ± 0.12 | 19.0 ± 0.5 | 9.5 ± 0.5 | [4] |
| AI Cru | 1.41 | 10.30 ± 0.20 | 6.30 ± 0.10 | 1.63 | 4.95 ± 0.06 | 4.43 ± 0.05 | 24.2 ± 0.5 | 17.7 ± 0.5 | [5] |
| SX Aur | 1.21 | 10.30 ± 0.40 | 5.60 ± 0.30 | 1.84 | 5.17 ± 0.09 | 3.90 ± 0.07 | [3] | ||
| MP Cen | 2.99 | 11.40 ± 0.40 | 4.40 ± 0.20 | 2.59 | 7.70 ± 0.10 | 6.60 ± 0.10 | 18.7 ± 0.4 | 12.4 ± 0.1 | [6] |
| IU Aur | 1.81 | 11.99 ± 0.08 | 6.07 ± 0.04 | 1.97 | 6.30 ± 0.20 | 5.20 ± 0.20 | 33.3 ± 0.1 | 28.8 ± 0.2 | [7] |
| V356 Sgr | 8.89 | 12.10 | 4.70 | 2.57 | 7.40 | 14.00 | 19.1 | 8.8 | [1] |
| V Pup (a) | 1.45 | 12.85 ± 0.50 | 6.33 ± 0.30 | 2.03 | 5.48 ± 0.18 | 4.59 ± 0.06 | 28.2 ± 1.0 | 26.6 ± 1.0 | [8] |
| V498 Cyg | 3.48 | 13.44 | 6.45 | 2.08 | 6.81 | 8.12 | [1] | ||
| GN Car | 4.34 | 13.49 | 4.59 | 2.94 | 7.14 | 8.29 | [1] | ||
| LZ Cep | 3.07 | 16.00 ± 9.80 | 6.50 ± 2.40 | 2.46 | 11.70 ± 3.30 | 9.40 ± 2.60 | 32.0 ± 1.0 | 28.0 ± 1.0 | [9] |
| δ Pic | 1.67 | 16.30 | 8.60 | 1.89 | 7.62 | 5.05 | 25.2 | 21.4 | [10] |
| XX Cas | 3.06 | 16.85 | 6.07 | 2.77 | 8.28 | 7.19 | [1] | ||
| HH Car | 3.23 | 17.00 | 14.00 | 1.21 | 6.10 | 10.70 | 35.5 | 29.9 | [1] |
| V337 Aql | 2.73 | 17.44 ± 0.31 | 7.83 ± 0.18 | 2.22 | 9.86 ± 0.06 | 7.48 ± 0.04 | 28.0 ± 0.5 | 23.6 ± 0.5 | [11] |
| AQ Cas | 11.70 | 17.63 ± 0.91 | 12.50 ± 0.81 | 1.41 | 13.40 ± 0.64 | 23.50 ± 0.73 | 27.0 ± 1.0 | 16.7 ± 0.4 | [12] |
| XZ Cep | 5.09 | 18.70 ± 1.30 | 9.30 ± 0.50 | 2.01 | 14.20 ± 0.10 | 14.20 ± 0.10 | 28.0 ± 1.0 | 24.0 ± 3.0 | [13] |
| 29 CMa (b) | 4.39 | 19.00 | 16.00 | 1.20 | 10.00 | 13.00 | 29.0 | 33.7 | [14] |
| AB Cru | 3.41 | 19.75 ± 1.04 | 6.95 ± 0.65 | 2.84 | 10.50 ± 0.32 | 8.85 ± 0.32 | 35.8 | 27.2 | [15] |
| V448 Cyg | 6.51 | 24.70 ± 0.70 | 13.70 ± 0.70 | 1.80 | 7.80 ± 0.20 | 16.30 ± 0.30 | 30.5 ± 0.1 | 20.3 ± 0.1 | [16] |
| QZ Car (c) | 5.99 | 30.00 ± 3.00 | 20.00 ± 3.00 | 1.50 | 10.00 ± 0.50 | 20.00 ± 1.00 | 36.0 | 30.0 | [17] |
| *GT Cep (d) | 4.90 | 10.70 ± 0.50 | 2.58 ± 0.14 | 4.14 | 6.34 ± 0.19 | 6.98 ± 0.11 | 22.4 ± 1.0 | 10.9 ± 0.3 | [18] |
| RZ Sct (e) | 15.20 | 11.70 | 2.49 | 4.68 | 15.00 | 15.90 | 19.0 | 6.5 | [1] |
| TU Mon (f) | 5.04 | 12.00 | 2.50 | 4.80 | 5.50 | 7.20 | 19.0 | 8.1 | [1] |
| V453 Cyg (g) | 3.89 | 14.36 ± 0.20 | 11.10 ± 0.13 | 1.29 | 8.55 ± 0.06 | 5.49 ± 0.06 | 26.6 ± 0.5 | 25.5 ± 0.8 | [1] |
| V729 Cyg (h) | 6.60 | 36.00 ± 3.00 | 10.00 ± 1.00 | 3.60 | 27.00 ± 1.00 | 15.00 ± 0.60 | [19] | ||
| BY Cru (i) | 106.40 | 9−11 | 1.80 | 5.30 | [20] |
Notes. Subscripts ‘a’ and ‘d’ refer to the mass accretor and mass donor, respectively. The list is adopted from the work of Malkov (2020) and Surkova & Svechnikov (2004). Systems without effective temperature estimates have only photometric orbit solutions and mass estimates. Comments on individual systems marked with superscripts:
Masses and radii taken from Budding et al. (2021).
Is a part of SB2+SB2 system, see Morrison & Conti (1979), Blackford et al. (2020).
The more massive star is rapidly rotating and has an accretion disc. See Wilson et al. (1985).
Debate about the mass ratio of this system exists in the literature. See the discussion in Cester et al. (1977).
Recent studies now consider this as a detached system. See Southworth et al. (2004).
A potential contact system (Ysarsoy & Yakut, 2014) and a part of a hierarchical triple system (Rauw et al. 2019).
A highly interacting binary with an F type supergiant donor, with the accretor invisible due to an accretion disc around it. The long orbital period suggests it may be undergoing thermal timescale Case AB or Case B mass transfer. As such, we do not compare our model predictions with six (d,e,f,g,h,i) observed systems marked with an asterisk.
References. (1) Surkova & Svechnikov (2004), (2) Budding et al. (2015), (3) Budding et al. (2004), (4) Hilditch et al. (2007), (5) Bell et al. (1987), (6) Terrell et al. (2005), (7) Surina & Kang (2009), (8) Stickland et al. (1998), (9) Mahy et al. (2011), (10) Evans (1974), (11) Tüysüz et al. (2014), (12) Ibanoglu et al. (2013), (13) Martins et al. (2017), (14) Bagnuolo et al. (1994), (15) Lorenz et al. (1994), (16) Djurašević et al. (2009), (17) Walker et al. (2017), (18) Çakırlı (2015), (19) Rauw et al. (1999), (20) Daems & Waelkens (1997).
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