Statistical properties of exoplanets. III. Planet properties and stellar multiplicity

By A. Eggenberger, S. Udry, M. Mayor. 2004

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Among the hundred or so extrasolar planets discovered to date, 19 are orbiting a component of a double or multiple star system. In this paper, we discuss the properties of these planets and compare them to the characteristics of planets orbiting isolated stars. Although the sample of planets found in multiple star systems is not large, some differences between the orbital parameters and the masses of these planets and the ones of planets orbiting single stars are emerging in the mass-period and in the eccentricity-period diagrams. As pointed out by Zucker & Mazeh (2002), the most massive short-period planets are all found in multiple star systems. We show here that the planets orbiting in multiple star systems also tend to have a very low eccentricity when their period is shorter than about 40 days. These observations seem to indicate that some kind of migration has been at work in the history of these systems. The properties of the five short-period planets orbiting in multiple star systems seem, however, difficult to explain with the current models of planet formation and evolution, at least if we want to invoke a single mechanism to account for all the characteristics of these planets.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/4fbc061965d310bbb876d6090f9b84743fc5d758

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Planets around evolved intermediate-mass stars - I. Two substellar companions in the open clusters NGC 2423 and NGC 4349 (2007, background): “First, we removed the few close binary stellar systems since planets in such systems probably have quite different properties (Eggenberger et al. 2004).”
Structure and Evolution of Nearby Stars with Planets. II. Physical Properties of ~1000 Cool Stars from the SPOCS Catalog (2006, background): “The distributions of observed planetary properties are of great importance for testing theories of planet formation and dynamics (Eggenberger et al. 2004; Marcy et al. 2005a).”
Prospects for the Characterization and Confirmation of Transiting Exoplanets via the Rossiter-McLaughlin Effect (2006, background): “By the time tides circularize the orbit and halt ‘‘Kozai migration,’’ the orbital inclination can change substantially (Wu & Murray 2003; Eggenberger et al. 2004; D. Fabrycky&S. Tremaine 2006, private communication).”
Planet formation and migration (2005, background): “It also appears that planets orbiting a component of a multiple star system tend to have a very low eccentricity when their period is shorter than about 40 days, i.e. when a is smaller than about 0.2 AU (Eggenberger et al 2004).”
Tertiary Companions to Close Spectroscopic Binaries (2006, background): “A distant (stellar) companion enhances planet growth and migration (Zucker & Mazeh 2002; Udry et al. 2003; Eggenberger et al. 2004), possibly in an analogous way to multiple-star formation as envisioned by Larson (2002) and others.”
The HARPS survey for southern extra-solar planets. II. A 14 Earth-masses exoplanet around μ Arae (2004, background): “…giving the possibility to explore their properties from a statistical point of view (e.g. Santos et al. 2001; Zucker & Mazeh 2002; Udry et al. 2003; Eggenberger et al. 2004), and the observational and theoretical approaches are now starting to converge (e.g. Trilling et al. 2002; Alibert et al.…”
Spectroscopic metallicities for planet-host stars: Extending the samples (2005, background): “See Eggenberger et al. (2004) and Eggenberger et al. (in prep.) for references.”
The SOPHIE search for northern extrasolar planets . I. A companion around HD 16760 with mass close to the planet/brown-dwarf transition (2009, background): “…planet thus adds to the growing evidence that, in contrast to short-period planets, long-period (>∼100 days) planets residing in binaries possess the same statistical properties as their counterparts orbiting single stars (Eggenberger et al. 2004; Mugrauer et al. 2005; Desidera et al. 2007).”
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A Bayesian Analysis of Extrasolar Planet Data for HD 73526 (2005, background): “…orbiting 51 Peg (Mayor & Queloz 1995), high-precision radial velocity measurements of the reflex radial velocity of the host star have lead to the discovery of over 130 planetary candidate companions to solar-type stars in both single- and multiple-star systems (see, e.g., Eggenberger et al. 2004).”
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Two Suns in The Sky: Stellar Multiplicity in Exoplanet Systems (2006, background): “We also exclude a radial velocity detected system, HD 219542, identified by Eggenberger et al. (2004) as an exoplanet system with multiple stars, but since confirmed as a false planet detection by its discoverers (Desidera et al. 2004).”
Properties of planets in binary systems - The role of binary separation (2006, background): “A more complete statistical analysis by Eggenberger et al. (2004), hereafter E04, confirms that massive planets in close orbits are mostly found in binaries.”
REVEALING A UNIVERSAL PLANET–METALLICITY CORRELATION FOR PLANETS OF DIFFERENT SIZES AROUND SOLAR-TYPE STARS (2013, background): “Eggenberger et al. (2004, 2011) found that circumstellar gas-giant planets are less frequent in systems with close-in stellar binaries.”
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Debris Disks in Main-Sequence Binary Systems (2006, background): “Some older binary systems also offer evidence of planetary system formation, with both planets (Patience et al. 2002; Eggenberger et al. 2004; Konacki 2005; Bakos et al. 2007) and debris disks (Aumann 1985; Patten & Willson 1991; Koerner et al. 2000; Prato et al. 2001) known.”