Table 5.
Overluminosity of observed Algol binaries in the Galaxy and the LMC, whenever available.
| Name | Period | Ma | Md | log La | log Ld | La/Lsingle | Ld/Lsingle | log (La/Ma) | log (Ld/Md) | Ref. |
|---|---|---|---|---|---|---|---|---|---|---|
| (d) | (M⊙) | (M⊙) | ||||||||
| TT Aur | 1.33 | 8.10 | 5.40 | 3.72 | 3.24 | 1.7 | 1.7 | 2.81 | 2.51 | [1] |
| μ1 Sco | 1.44 | 8.30 ± 1.00 | 4.60 ± 1.00 | 3.66 | 3.20 | 1.4 | 3.5 | 2.74 | 2.54 | [2] |
| BF Cen | 3.69 | 8.70 | 3.80 | 2.82 | 2.55 | 0.06 | 1.3 | 1.88 | 1.97 | [1] |
| IZ Per | 3.68 | 9.97 ± 0.55 | 3.20 ± 0.17 | 3.85 | 2.57 | 0.5 | 2.3 | 2.85 | 2.06 | [3] |
| AI Cru | 1.41 | 10.30 ± 0.20 | 6.30 ± 0.10 | 3.88 | 3.24 | 0.6 | 0.9 | 2.87 | 2.44 | [4] |
| MP Cen | 2.99 | 11.40 ± 0.40 | 4.40 ± 0.20 | 3.80 | 3.00 | 0.25 | 2.63 | 2.74 | 2.35 | [5] |
| IU Aur | 1.81 | 11.99 ± 0.08 | 6.07 ± 0.04 | 4.64 | 4.22 | 3.4 | 9.9 | 3.56 | 3.43 | [6] |
| V356 Sgr | 8.89 | 12.10 | 4.70 | 3.81 | 3.02 | 0.3 | 2.3 | 2.73 | 2.35 | [1] |
| V Pup | 1.45 | 14.00 ± 0.50 | 7.30 ± 0.30 | 4.28 | 3.97 | 1.7 | 8.1 | 3.13 | 3.10 | [7] |
| δ Pic | 1.67 | 16.30 | 8.60 | 4.32 | 3.68 | 0.4 | 0.8 | 3.10 | 2.74 | [8] |
| HH Car | 3.23 | 17.00 | 14.00 | 4.73 | 4.91 | 1.8 | 4.8 | 3.50 | 3.76 | [1] |
| V337 Aql | 2.73 | 17.44 ± 0.31 | 7.83 ± 0.18 | 4.73 | 4.20 | 1.1 | 4.7 | 3.49 | 3.30 | [9] |
| AQ Cas | 11.70 | 17.63 ± 0.91 | 12.50 ± 0.81 | 4.94 | 4.59 | 1.48 | 1.1 | 3.69 | 3.49 | [10] |
| XZ Cep | 5.09 | 18.70 ± 1.30 | 9.30 ± 0.50 | 5.05 | 4.79 | 1.3 | 11 | 3.78 | 3.82 | [11] |
| AB Cru | 3.41 | 19.75 ± 1.04 | 6.95 ± 0.65 | 5.21 | 4.58 | 2.5 | 20.6 | 3.91 | 3.74 | [12] |
| V448 Cyg | 6.51 | 24.70 ± 0.70 | 13.70 ± 0.70 | 4.63 | 4.57 | 0.3 | 1.1 | 3.23 | 3.43 | [13] |
| QZ Car | 5.99 | 30.00 ± 3.00 | 20.00 ± 3.00 | 5.18 | 5.46 | 0.9 | 5.2 | 3.70 | 4.16 | [14] |
| VFTS 061 | 2.33 | 16.30 ± 1.40 | 8.70 ± 0.60 | 4.77 | 4.75 | 1.9 | 14 | 3.55 | 3.81 | [15] |
| VFTS 652 | 8.59 | 18.10 ± 3.90 | 6.50 ± 1.10 | 5.35 | 4.92 | 5.8 | 31 | 4.09 | 4.10 | [15] |
| VFTS 538 | 4.15 | 18.30 ± 1.90 | 11.80 ± 1.40 | 4.96 | 5.31 | 2.4 | 20 | 3.70 | 4.24 | [15] |
| VFTS 450 | 6.89 | 29.00 ± 4.10 | 27.80 ± 3.90 | 5.30 | 5.46 | 1.3 | 1.5 | 3.84 | 4.01 | [15] |
Notes. We give here the luminosity of the accretors (La) and donors (Ld) of massive semi-detached double-lined eclipsing binaries in the Galaxy and the LMC, and derive the ratio of their respective luminosity to that of single star models (Lsingle) of the same mass and effective temperature. Masses and luminosities are in Solar units.
References. (1) Surkova & Svechnikov (2004), (2) Budding et al. (2015), (3) Hilditch et al. (2007), (4) Bell et al. (1987), (5) Terrell et al. (2005), (6) Surina & Kang (2009), (7) Stickland et al. (1998), (8) Evans (1974), (9) Tüysüz et al. (2014), (10) Ibanoglu et al. (2013), (11) Martins et al. (2017), (12) Lorenz et al. (1994), (13) Djurašević et al. (2009), (14) Walker et al. (2017), (15) Mahy et al. (2020a,b).
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