Table 2
Physical and orbital parameters of confirmed circumbinary systems, and tidal parameters estimated with our model.
α | e2 | M2 | Viscosity regime | αcrit,g | αcrit,s | Migration direction | ![]() |
![]() |
|
---|---|---|---|---|---|---|---|---|---|
Kepler-16 (1) | 0.318 | 0.0069 | 0.175 | Gaseous | 0.086 | 0.260 | Outward | 3 × 1013 | 6 × 1014 |
Kepler-34 (2) | 0.210 | 0.182 | 0.250 | Gaseous | 0.309 | 1.340 | Inward | 7 × 1013 | 3 × 1012 |
Kepler-35 (2) | 0.292 | 0.042 | 0.249 | Gaseous | 0.171 | 0.559 | Outward | 2 × 1012 | 1× 1012 |
Kepler-38 (3) | 0.316 | 0.023 | 0.165 | ? | 0.162 | 0.492 | ? | 5 × 1012 | 8 × 1012 |
Kepler-47b (4) | 0.283 | 0.021 | 0.194 | Gaseous | 0.135 | 0.455 | Outward | 3× 1012 | 6× 1012 |
Kepler-47d (5) | 0.116 | 0.024 | 0.194 | Gaseous | 0.100 | 0.701 | Outward | 2 × 1015 | 3 × 1013 |
Kepler-47c (4) | 0.085 | 0.044 | 0.194 | ? | 0.121 | 1.070 | Inward | 7 × 1015 | 7 × 1013 |
Kepler-64 (6) | 0.267 | 0.0702 | 0.166 | Gaseous | 0.261 | 0.921 | Outward | 1 × 1015 | 1 × 1013 |
Kepler-413 (7) | 0.286 | 0.1181 | 0.240 | Gaseous | 0.290 | 0.966 | Inward | 5 × 1013 | 3 × 1011 |
Kepler-453 (8) | 0.235 | 0.0359 | 0.142 | Gaseous | 0.191 | 0.753 | Outward | 3 × 1014 | 3 × 1013 |
Kepler-1647 (9) | 0.047 | 0.0581 | 0.247 | Gaseous | 0.098 | 1.367 | Inward | 3 × 1018 | 1 × 1016 |
Kepler-1661 (10) | 0.295 | 0.057 | 0.181 | Gaseous | 0.235 | 0.761 | Outward | 2 × 1014 | 3 × 1013 |
TOI-1338 (11) | 0.287 | 0.093 | 0.173 | Gaseous | 0.303 | 1.007 | Inward | 5 × 1012 | 1 × 1011 |
Notes. The viscosity regime of the CB planet is inferred from the mass and radius, compared with the γ2-values estimated for the Solar System planets in Ferraz-Mello (2013). The critical α-values and the migration direction are discussed in Sect. 4.2.1., while the tidal timescales for the semimajor axis evolution are explained in Sect. 4.2.2. For Kepler-38 we consider the mass estimated by means of a mass-radius fit in Zoppetti et al. (2019a), while the eccentricity adopted corresponds to the forced eccentricity.
References. (1)Doyle et al. (2011). (2)Welsh et al. (2012). (3)Orosz et al. (2012a). (4)Orosz et al. (2012b). (5)Orosz et al. (2019). (6)Schwamb et al. (2013). (7)Kostov et al. (2014). (8)Welsh et al. (2015). (9)Kostov et al. (2016). (10)Socia et al. (2020). (11)Kostov et al. (2020).
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