Table 1
Possible scenarios of the nature of Kepler-1625 b and its proposed companion.
| Scenario | R⋆ [R⊙] | Rp [RJup] | Rs [RJup] | Mp [MJup] | M⊕ | Ms∕Mp |
|---|---|---|---|---|---|---|
| (1aa) Saturn-mass gas planet, Earth-mass gas moon | 1.305a | 0.86b | 0.26b | 0.43 | 11 | 7.9 × 10−3 |
| (1ab) Saturn-mass gas planet, Neptune-mass water–rock moon | 172 | 1.3 × 10−1 | ||||
| (1ba) brown dwarf, Earth-mass gas moon | 753 | 11 | 4.2 × 10−5 | |||
| (1bb) brown dwarf, Neptune-mass water–rock moon | 172 | 7.1 × 10−4 | ||||
| (2aa) very-low-mass star, mini-Neptune planet | 1.793a | 1.18b | 0.35b | 913 | 104 | 3.5 × 10−4 |
| (2ab) very-low-mass star, super-Earth water–rock planet | 702 | 2.4 × 10−3 | ||||
| (3aa) very-low-mass star, Neptune-like planet | 2.056a | 1.36b | 0.40b | 1124 | 204 | 5.6 × 10−4 |
| (3ab) very-low-mass star, super-Saturn water–rock planet | 1802 | 5.1 × 10−3 | ||||
| (TKS) super-Jovian planet, Neptune-like moon | – | 15 | 0.355 | 105 | 175 | 5.4 × 10−3 |
Notes. (a) The stellar radius estimates are based on Mathur et al. (2017). (b) The radii of the transiting primary and proposed secondary were estimated from the lightcurves of Teachey et al. (2018). The corresponding masses of the objects were estimated using structure models and evolution tracks from the following references.
References. (1) Masuda (2014); (2) Fortney et al. (2007); (3) Baraffe et al. (2003); (4) Baraffe et al. (2008); (5) Teachey et al. (2018).
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