Table 9
Hierarchical triple systems with planets.
| Planet Host | Close Pair | Wide Pair | Planet | ||||||
|
|
|||||||||
| Name | Mass | Comp. Mass | ρ close | ρ wide | a crit a | M pl | a pl | e pl | Ref. |
| M ⊙ | M ⊙ | AU | AU | AU | M J | AU | |||
|
|
|||||||||
| 30 Ari B | 1.16 | 1.31+0.13b | 0.02 | 1500 | 318 | 9.88 | 1.00 | 0.29 | 1, 2 |
| HD 40979 | 1.19 | 0.83+0.38 | 129 | 6400 | 1452 | 3.83 | 0.85 | 0.27 | 3 |
| HD 65216 | 0.92 | 0.09+0.08 | 6 | 253 | 82 | 1.21 | 1.47 | 0.41 | 4, 5 |
| HD 132563B | 1.01 | 1.08+0.56c | 10 | 400 | 78 | 1.49 | 2.62 | 0.22 | 6 |
| HD 178911B | 1.06 | 1.10+0.79 | 3 | 640 | 120 | 7.35 | 0.35 | 0.14 | 7 |
| 16 Cyg B | 0.99 | 1.02+0.17 | 70 | 850 | 183 | 1.68 | 1.68 | 0.68 | 8 |
| HD 196050 | 1.15 | 0.29+0.19 | 20 | 511 | 146 | 2.90 | 2.45 | 0.23 | 5 |
| 91 Aqrd | 1.23 | 0.87+0.84 | 18 | 2250 | 461 | 2.90 | 0.30 | – | 9, 10, 6 |
Notes.
The critical semimajor axis for dynamical stability was obtained from the projected separation as in Bonavita & Desidera (2007);
value of plausible mass, see Sect. 5;
planet announced in 2003 (Mitchell et al. 2003) but never published in refereed journals, confirmed at the Conference “Planetary Systems Beyond the Main Sequence”, as reported in the Extrasolar Planet Encyclopedia. Stellar mass of 91 Aqr obtained from param interface (Da Silva et al. 2006) using the input parameters from Hekker et al. (2007); stellar masses of the companions from magnitudes in WDS and mass-luminosity relation.
References. 1: Guenther et al. (2009); 2: Morbey & Brosterhus (1974); 3: Mugrauer et al. (2007a), 4: Mugrauer et al. (2007b), 5: Eggenberger et al. (2007); 6: This paper; 7: Tokovinin et al. (2000); 8: Patience et al. (2002); 9: Raghavan et al. (2006); 10: WDS (Mason et al. 2001).
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