Stellar Companions to Stars with Planets

By J. Patience, R. White, A. Ghez, C. McCabe, I. McLean, J. Larkin, L. Prato, Sungsoo S. Kim, J. Lloyd, M. Liu and 11 more. 2002

313 citations recorded by the source corpus.

A combination of high-resolution and wide-field imaging reveals two binary stars and one triple star system among the sample of the first 11 stars with planets detected by radial velocity variations. High-resolution speckle or adaptive optics (AO) data probe subarcsecond scales down to the diffraction limit of the Keck 10 m or the Lick 3 m, and direct images or AO images are sensitive to a wider field, extending to 10'' or 38'', depending on the camera. One of the binary system—HD 114762—was not previously known to be a spatially resolved multiple system; additional data taken with the combination of Keck adaptive optics and NIRSPEC are used to characterize the new companion. The second binary system—τ Boo—was a known multiple with two conflicting orbital solutions; the current data will help constrain the discrepant estimates of periastron time and separation. Another target—16 Cyg B—was a known common proper motion binary, but the current data resolve a new third component, close to the wide companion 16 Cyg A. Both the HD 114762 and 16 Cyg B systems harbor planets in eccentric orbits, while the τ Boo binary contains an extremely close planet in a tidally circularized orbit. Although the sample is currently small, the proportion of binary systems is comparable to that measured in the field over a similar separation range. Incorporating the null result from another companion search project lowers the overall fraction of planets in binary systems, but the detections in our survey reveal that planets can form in binaries separated by less than 50 AU.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Geophysics

View Paper: https://www.semanticscholar.org/paper/91808ccb6aee8b4e5ef48303cc968a98bd6634ec

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Citations in the corpus

The M-dwarfs in Multiples (MinMs) survey – I. Stellar multiplicity among low-mass stars within 15 pc (2015, background): “The companion star fraction (CSF) quantifies the total number of companions within the sample as the following: CSF = b+ 2t+ 3q + ... s+ b+ t+ q + ... , (4) (Patience et al. 2002).”
Structure and Evolution of Nearby Stars with Planets. II. Physical Properties of ~1000 Cool Stars from the SPOCS Catalog (2006, background): “The planetary system τ Boo is associated with a visual binary companion at ∼ 240AU (Hale 1994; Patience et al. 2002).”
Two Suns in The Sky: Stellar Multiplicity in Exoplanet Systems (2006, methodology): “The multiplicity of this system has been previously identified (Patience et al. 2002; Lowrance et al. 2002; Eggenberger et al. 2004).”
THE HAWAII INFRARED PARALLAX PROGRAM. I. ULTRACOOL BINARIES AND THE L/T TRANSITION, (2012, unknown): “…& Hillenbrand (2004); (68) Metchev & Hillenbrand (2006); (69) Montagnier et al. (2006); (70) Mugrauer et al. (2007); (71) Nielsen et al. (2012); (72) Patience et al. (2002); (73) Potter et al. (2002); (74) Pravdo et al. (2005); (75) Reid et al. (2001); (76) Reid et al. (2006a); (77) Reid et…”
Discovery of Two T Dwarf Companions with the Spitzer Space Telescope (2006, background): “Several direct imaging surveys have focused on known extrasolar planetary systems (Luhman & Jayawardhana 2002; Patience et al. 2002; Mugrauer et al. 2005; Chauvin et al. 2006), producing one companion that was initially described as a brown dwarf (Els et al. 2001) but later shown to be a white…”
Properties of planets in binary systems - The role of binary separation (2006, background): “However, the latest position measurement by Patience et al. (2002) indicates a larger separation and similar position angle than predicted by the preliminary orbit.”
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.”
THE LICK-CARNEGIE EXOPLANET SURVEY: A URANUS-MASS FOURTH PLANET FOR GJ 876 IN AN EXTRASOLAR LAPLACE CONFIGURATION (2010, unknown): “These include Leinert et al. (1997), Patience et al. (2002), Hinz et al. (2002), Trilling et al. (2000), Lestrade et al. (2006), Shankland et al. (2008), and Bryden et al. (2009).”
MODULES FOR EXPERIMENTS IN STELLAR ASTROPHYSICS (MESA): PLANETS, OSCILLATIONS, ROTATION, AND MASSIVE STARS (2013, background): “…of the formation and migration of giant planets, and of the importance of factors such as stellar mass (Laughlin et al. 2004; Alibert et al. 2011; Boss 2011), composition (Fischer & Valenti 2005; Young et al. 2012), and binarity (Patience et al. 2002; Mugrauer & Neuhäuser 2009; Roell et al. 2012).”