The observed distribution of spectroscopic binaries from the Anglo-Australian Planet Search

Jenkins, James S.; Díaz, Matías R.; Jones, H. R. A.; Butler, R. Paul; Tinney, C. G.; O’Toole, S. J.; Carter, B. D.; Wittenmyer, Robert A.; Pinfield, D. J.

doi:10.1093/mnras/stv1596

Cited by 20 publications

(31 citation statements)

References 70 publications

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“…HD 120690: SB with an orbital solution from [36,92]. The companion also has direct detection, which yields a mass close to the minimum mass from the spectroscopic orbit [86].…”

Section: Id Plx (Mas) Rho ( ) Ecc a (Au) A Crit (Au) Mmentioning

confidence: 91%

“…HD 145825: New binary from the RV orbital solution [38], with mass in the stellar regime. HD 150248: SB with orbital solution from [36]. The star was already in BD07 as a ∆µ binary.…”

Section: Id Plx (Mas) Rho ( ) Ecc a (Au) A Crit (Au) Mmentioning

confidence: 99%

“…HD 169586: SB with an orbital solution from [36]. The star was already included in BD07 as a ∆µ binary.…”

Section: Id Plx (Mas) Rho ( ) Ecc a (Au) A Crit (Au) Mmentioning

confidence: 99%

“…The works by [35,36], which included spectroscopic orbital solutions for binaries detected in the surveys that formed the UD sample.…”

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confidence: 99%

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Frequency of Planets in Binaries

Bonavita

Desidera

2020

Galaxies

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The frequency of planets in binaries is an important issue in the field of extrasolar planet studies because of its relevance in the estimation of the global planet population of our galaxy and the clues it can give to our understanding of planet formation and evolution. Multiple stars have often been excluded from exoplanet searches, especially those performed using the radial velocity technique, due to the technical challenges posed by such targets. As a consequence and despite recent efforts, our knowledge of the frequency of planets in multiple stellar systems is still rather incomplete. On the other hand, the lack of knowledge about the binarity at the time of the compilation of the target samples means that our estimate of the planet frequency around single stars could be tainted by the presence of unknown binaries, especially if these objects have a different behavior in terms of planet occurrence. In a previous work we investigated the binarity of the objects included in the Uniform Detectability sample defined by Fisher and Valenti (2005), showing how more than 20% of their targets were, in fact, not single stars. Here, we present an update of this census, made possible mainly by the information now available thanks to the second Gaia Data Release. The new binary sample includes a total of 313 systems, of which 114 were added through this work. We were also able to significantly improve the estimates of masses and orbital parameters for most of the pairs in the original list, especially those at close separations. A few new systems with white dwarf companions were also identified. The results of the new analysis are in good agreement with the findings of our previous work, confirming the lack of difference in the overall planet frequency between binaries and single stars but suggesting a decrease in the planet frequency for very close pairs. Galaxies 2020, 8, 16 G (1) Mass(J) = 3.95501 − 2.87761 * M J + 1.58846 * M 2 J − 0.568685 * M 3 J + 0.125674 * M 4 J −0.0169899 * M 5 J + 0.00136157 * M 6 J − 5.91812e − 05 * M 7 J + 1.07257e − 06 * M 8 J (2) Mass(K)

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“…HD 120690: SB with an orbital solution from [36,92]. The companion also has direct detection, which yields a mass close to the minimum mass from the spectroscopic orbit [86].…”

Section: Id Plx (Mas) Rho ( ) Ecc a (Au) A Crit (Au) Mmentioning

confidence: 91%

“…HD 145825: New binary from the RV orbital solution [38], with mass in the stellar regime. HD 150248: SB with orbital solution from [36]. The star was already in BD07 as a ∆µ binary.…”

Section: Id Plx (Mas) Rho ( ) Ecc a (Au) A Crit (Au) Mmentioning

confidence: 99%

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Frequency of Planets in Binaries

Bonavita

Desidera

2020

Galaxies

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“…′′ 2 visual binary B 413 with a large ∆V = 5.6 mag, an estimated period of ∼3 kyr, and the correspondingly slow relative motion. The RV variation of the brighter component A was noted by Jenkins et al (2015) during search for exo-planets. They determined a preliminary orbit with P = 312 days and e = 0.75, although the coverage of the RV curve was incomplete.…”

Section: Hip 8353 (Triple)mentioning

confidence: 94%

Spectroscopic Orbits of Subsystems in Multiple Stars. V.

Tokovinin

2019

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New spectroscopic binary companions of giant stars and updated metallicity distribution for binary systems

Bluhm

Jones

Vanzi

et al. 2016

A&A

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We report the discovery of 24 spectroscopic binary companions to giant stars. We fully constrain the orbital solution for 6 of these systems. We cannot unambiguously derive the orbital elements for the remaining stars because the phase coverage is incomplete. Of these stars, 6 present radial velocity trends that are compatible with long-period brown dwarf companions. The orbital solutions of the 24 binary systems indicate that these giant binary systems have a wide range in orbital periods, eccentricities, and companion masses. For the binaries with restricted orbital solutions, we find a range of orbital periods of between ∼ 97-1600 days and eccentricities of between ∼ 0.1-0.4. In addition, we studied the metallicity distribution of single and binary giant stars. We computed the metallicity of a total of 395 evolved stars, 59 of wich are in binary systems. We find a flat distribution for these binary stars and therefore conclude that stellar binary systems, and potentially brown dwarfs, have a different formation mechanism than planets. This result is confirmed by recent works showing that extrasolar planets orbiting giants are more frequent around metal-rich stars. Finally, we investigate the eccentricity as a function of the orbital period. We analyzed a total of 130 spectroscopic binaries, including those presented here and systems from the literature. We find that most of the binary stars with periods 30 days have circular orbits, while at longer orbital periods we observe a wide spread in their eccentricities. hand, the planetary formation follows the planet-metallicity correlation. This correlation tells us that planets form more efficiently around metal-rich stars (Gonzalez, 1997;Santos et al. 2001). When one of the stars in older stellar systems evolves off of the main sequence, the mutual effect of tidal interaction between them might dictate the final orbital configuration of the system. Verbunt & Phinney (1995) studied the orbital properties of binaries containing giant stars in open clusters. They showed that most of the binaries with periods shorter than ∼ 200 days present nearly circular orbits, which is most likely explained by the effect of the tidal circularization (Zahn 1977(Zahn , 1989Tassoul 1987Tassoul , 1988Tassoul , 1992. Similarly, Pan et al. (1998) showed that the predictions of Zahn's theories on synchronization for main-sequence binary systems are compatible with observational data. In addition, Massarotti et al. (2008, MAS08 hereafter) showed based on a sample 761 giant stars that all stars in binary systems with periods shorter than 20 days have circularized orbits. They also demonstrated that ∼50% of the orbits that have periods in the range of 20-100 days show significant eccentricity. This result shows the importance of studying the eccentricity distribution of binary Article number, page 1 of 17 A&A proofs: manuscript no. PBluhm

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The observed distribution of spectroscopic binaries from the Anglo-Australian Planet Search

Cited by 20 publications

References 70 publications

Frequency of Planets in Binaries

Frequency of Planets in Binaries

Spectroscopic Orbits of Subsystems in Multiple Stars. V.

New spectroscopic binary companions of giant stars and updated metallicity distribution for binary systems

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