Abstract
The search for planets in multiple systems allows to improve our knowledge of planet formation and evolution. On one hand, the frequency of planets in binary systems has a strong effect on the global frequency of planets, as more than half of solar-type stars are in binary or multiple systems (Duquennoy and Mayor 1991). On the other hand, the properties of planets in binaries, and their differences with the properties of the planets orbiting single stars, would shed light on the effects caused by the presence of the companion stars. Indeed, the first analysis of the properties of planets in binaries showed the occurrence of some differences with respect to those orbiting single stars (Zucker and Mazeh 2002; Eggenberger et al. 2004).
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Notes
- 1.
The mass-ratio is defined here as M companion ∕ M planethost. In nearly all cases, the companion is less massive than the planet host.
- 2.
- 3.
The critical semimajor axis for dynamical stability of a planet in a binary as defined by Holman and Wiegert (2001) is given by
$$\begin{array}{rcl}{ a}_{\mathrm{crit}} = \left (0.464 - 0.380\mu - 0.631{e}_{\mathrm{bin}} + 0.586\mu {e}_{\mathrm{bin}}\right ){a}_{\mathrm{bin}} + \left (0.150{e}_{\mathrm{bin}}^{2} - 0.198\mu {e}_{\mathrm{ bin}}^{2}\right ){a}_{\mathrm{ bin}}.\quad & & \end{array}$$(5.1)In this equation, a bin and e bin are the binary semimajor axis and eccentricity, and μ is the mass-ratio defined as μ = M comp ∕ (M obj + M comp). The quantity M obj is the mass of the object for which the critical semimajor axis for dynamical stability is computed and M comp is the mass of its companion. The critical semimajor axis given by Eq. (5.1) refers to a planet in a circular orbit on the same plane as that of the binary.
- 4.
The very recent discovery of planets in highly eccentric orbits, orbiting stars in binary systems (Tamuz et al. 2007), adds further support to the link between binarity and extreme planet eccentricities.
- 5.
The planet candidates discussed in Section 5.7 have either long periods or low velocity amplitudes and therefore are not of concern in this discussion.
- 6.
Defined by Pfhal and Mutherspaugh (2006) as those binaries with semimajor axis less than 50 AU.
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Desidera, S. et al. (2010). The SARG Planet Search. In: Haghighipour, N. (eds) Planets in Binary Star Systems. Astrophysics and Space Science Library, vol 366. Springer, Dordrecht. https://doi.org/10.1007/978-90-481-8687-7_5
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