Three New “51 Pegasi–Type” Planets

Butler, R. Paul; Marcy, Geoffrey W.; Williams, Eric; Hauser, Heather M.; Shirts, Phil

doi:10.1086/310444

Cited by 455 publications

(337 citation statements)

References 26 publications

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“…Eggenberger et al (2004) announced a sample of 15 new wide low-mass companions to planet-host stars and suggested a possible difference in the mass-period and eccentricity-period distributions, trend previously reported in Zucker & Mazeh (2002). These discoveries and potential differences in the properties of planets orbiting single stars and planets orbiting stars in multiple systems triggered dedicated searches by several groups (Butler et al 1997;Mugrauer et al 2004aMugrauer et al ,b, 2005aMugrauer et al ,b, 2006aMugrauer et al , 2007aKonacki 2005;Eggenberger et al 2006;Desidera & Barbieri 2007;Bonavita & Desidera 2007) to confirm (or otherwise) those trends in the properties of exoplanets. These searches also led to the discoveries of the first wide brown dwarf companion to HD 3651 (Mugrauer et al 2006b), a K7 dwarf with a sub-Saturn mass planet (Fischer et al 2004;Santos et al 2005), and the most evolved multiple system with an exoplanet (Butler et al 2001), composed of a K subgiant and a white dwarf (HD 27442; Chauvin et al 2006;Raghavan et al 2006;Mugrauer et al 2007a).…”

Section: Introductionmentioning

confidence: 74%

Binary frequency of planet-host stars at wide separations

Lodieu

Pérez‐Garrido

Béjar

et al. 2014

A&A

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Aims. The aim of the project is to improve our knowledge on the multiplicity of planet-host stars at wide physical separations. Methods. We cross-matched approximately 6200 square degree area of the southern sky imaged by the Visible Infrared Survey Telescope for Astronomy (VISTA) Hemisphere Survey (VHS) with the Two Micron All Sky Survey (2MASS) to look for wide common proper motion companions to known planet-host stars. We complemented our astrometric search with photometric criteria. Results. We confirmed spectroscopically the co-moving nature of seven sources out of 16 companion candidates and discarded eight, while the remaining one stays as a candidate. Among these new wide companions to planet-host stars, we discovered a T4.5 dwarf companion at 6.3 arcmin (∼9000 au) from HIP 70849, a K7V star which hosts a 9 Jupiter mass planet with an eccentric orbit. We also report two new stellar M dwarf companions to one G and one metal-rich K star. We infer stellar and substellar binary frequencies for our complete sample of 37 targets of 5.4 ± 3.8% and 2.7 ± 2.7% (1σ confidence level), respectively, for projected physical separations larger than ∼60-160 au assuming the range of distances of planet-host stars (24-75 pc). These values are comparable to the frequencies of non planet-host stars. We find that the period-eccentricity trend holds with a lack of multiple systems with planets at large eccentricities (e > 0.2) for periods less than 40 days. However, the lack of planets more massive than 2.5 Jupiter masses and short periods (<40 days) orbiting single stars is not so obvious due to recent discoveries by ground-based transit surveys and space missions.

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Section: Introductionmentioning

confidence: 74%

Binary frequency of planet-host stars at wide separations

Lodieu

Pérez‐Garrido

Béjar

et al. 2014

A&A

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“…of their primaries, 50-100 times closer than Jupiter is to our Sun. At such orbital distances, due to stellar irradiation alone, an EGP can have an effective temperature greater than 600 K. Indeed, the EGPs HD187123b, HD209458b, T Boo b, HD75289b, 51 Peg b, v And b, and HD217107b (Mayor and Queloz 1995;Marcy and Butler 1995;Butler et al 1997Butler et al , 1998Fischer et al 1999;Henry et al 2000;Charbonneau et al 2000) likely all have TeffS above 1000 K. This is to be compared with TeffS for Jupiter and Saturn of 125 K and 95 K, respectively. Despite such proximity, these planets are stable to tidal stripping and significant evaporation (Guillot et al 1996).…”

Section: New Worldsmentioning

confidence: 94%

New Insights into Extrasolar Giant Planets

Burrows

2004

Symp. - Int. Astron. Union

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“…Firstly, Tau Boo has an extremely high level of surface differential rotation at almost 10 times the solar value and Donati et al (2008) suggest that such a high level of differential rotation could well be responsible for the rapid magnetic cycle of the star. However, Tau Boo is also the host of a "Hot Jupiter" with a period of a few days (Butler et al 1997) and Farès et al (2009) suggest that this could be responsible.…”

Section: The Evolution Of Magnetic Topologiesmentioning

confidence: 99%

Do young Suns undergo magnetic reversals?

et al. 2009

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Abstract.A key part of the modern-day regenerative solar magnetic dynamo is the reversal of the Sun's global magnetic field every eleven years. However, recent theoretical models indicate that young-rapidly rotating Sun-like stars may not always undergo full magnetic reversals, but instead may sometimes undergo "attempted" reversals where the magnetic field declines in strength only to return with the same polarity. Using the technique of Zeeman Doppler imaging we have mapped the magnetic field topology of a small sample of young Sun-like stars at multiple epochs, and present tentative evidence of an "attempted" magnetic field reversal on one of our stars.

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Three New “51 Pegasi–Type” Planets

Cited by 455 publications

References 26 publications

Binary frequency of planet-host stars at wide separations

Binary frequency of planet-host stars at wide separations

New Insights into Extrasolar Giant Planets

Do young Suns undergo magnetic reversals?

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