Properties of planets in binary systems - The role of binary separation

By S. Desidera, M. Barbieri. 2006

177 citations recorded by the source corpus.

Aims. The statistical properties of planets in binaries were investigated. Any difference to planets orbiting single stars can shed light on the formation and evolution of planetary systems. As planets were found around components of binaries with very different separation and mass ratio, it is particularly important to study the characteristics of planets as a function of the effective gravitational influence of the companion. Methods. A compilation of planets in binary systems was made; a search for companions orbiting stars recently shown to host planets was performed, resulting in the addition of two further binary planet hosts (HD 20782 and HD 109749). The probable original properties of the three binary planet hosts with white dwarfs companions were also investigated. Using this updated sample of planets in binaries we performed a statistical analysis of the distributions of planet mass, period, and eccentricity, fraction of multiplanet systems, and stellar metallicity for planets orbiting components of tight and wide binaries and single stars. Results. The only highly significant difference revealed by our analysis concerns the mass distribution of short-period planets. Massive planets in short period orbits are found in most cases around the components of rather tight binaries. The properties of exoplanets orbiting the components of wide binaries are compatible with those of planets orbiting single stars, except for a possible greater abundance of high-eccentricity planets. The previously suggested lack of massive planets with P > 100 days in binaries is not confirmed. Conclusions. We conclude that the presence of a stellar companion with separation smaller than 100-300 AU is able to modify the formation and/or migration and/or the dynamical evolution history of giant planets while wide companions play a more limited role.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/0c662117950e8cb5e763ab57f475de78f2844dfd

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In Astronomy and Astrophysics

1. A. Kraus
2. Michael J. Ireland
3. C. Mordasini
4. A. Mann
5. Y. Alibert
6. T. Dupuy
7. L. Hillenbrand
8. S. Naoz

Citations in the corpus

• THE IMPACT OF STELLAR MULTIPLICITY ON PLANETARY SYSTEMS. I. THE RUINOUS INFLUENCE OF CLOSE BINARY COMPANIONS (2016, background): “…wide binary companions to planet hosts have been identified as well (Mugrauer et al. 2005; Daemgen et al. 2009; Muterspaugh et al. 2010; Bergfors et al. 2012), and it appears that wide binary systems are common exoplanet hosts (Desidera & Barbieri 2007; Eggenberger et al. 2007; Duchêne 2010).”
• Radial Velocity Search for Extrasolar Planets in Visual Binary Systems (2009, background): “Recent observational results suggest differences in orbital elements between the planets found around single stars and those in binary systems (Zucker & Mazeh 2000; Eggenberger et al. 2004; Desidera & Barbieri 2007).”
• ON THE FORMATION OF HOT JUPITERS IN STELLAR BINARIES (2012, background): “…analyses suggest that at least ∼ 20% of the known extrasolar planetary systems are associated with one or more stellar companions (Raghavan et al. 2006; Desidera & Barbieri 2007; Eggenberger et al. 2007), and thus stellar perturbers are likely to be at least as important as planetary perturbers.”
• THE ROLE OF MULTIPLICITY IN DISK EVOLUTION AND PLANET FORMATION (2011, result): “This prediction is consistent with tentative results for exoplanet host stars in the field that have been identified via either radial velocities (Desidera & Barbieri 2007; Eggenberger et al. 2007) or planet transits (Daemgen et al. 2009), who have found that some exoplanet hosts have binary…”
• Extrasolar planet population synthesis - II. Statistical comparison with observations (2009, background): “(6) It was found that planets in relatively tight binary systems have statistically different properties (e.g. Eggenberger et al. 2004; Desidera & Barbieri 2007).”
• The great escape: how exoplanets and smaller bodies desert dying stars (2011, background): “In the second category, examples are thought to include Gl 86 = HD 13445 (Queloz et al. 2000; Mugrauer & Neuhäuser 2005; Lagrange et al. 2006), HD 27442 (Butler et al. 2001; Chauvin et al. 2006), and HD 147513 (Mayor et al. 2004; Desidera & Barbieri 2007).”
• Mapping the Shores of the Brown Dwarf Desert. I. Upper Scorpius (2007, result): “This supports early results from radial velocity and transit surveys (Desidera & Barbieri 2007; Roell et al. 2012; Wang et al. 2014).”