Frequency of Planets in Binaries

Bonavita, M.; Desidera, S.

doi:10.3390/galaxies8010016

Cited by 31 publications

(12 citation statements)

References 103 publications

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“…A shortfall of close binaries (<50-100 AU) among planet hosts has been vastly reported in observational surveys (Roell et al, 2012;Bergfors et al, 2013;Wang et al, 2014;Kraus et al, 2016;Moe and Kratter, 2019;Bonavita and Desidera, 2020). This feature is generally attributed to a hindrance of planet formation in very tight binaries, and is also predicted in theoretical models (Thebault and Haghighipour, 2015).…”

Section: Completeness and Survey Limitationsmentioning

confidence: 77%

“…We complemented the multiplicity data from these databases with the Catalogue of Exoplanets in Binary Star Systems 5 (Schwarz et al, 2016). We added to this all systems from published surveys searching for visual stellar companions to circumprimary planetary systems (Luhman and Jayawardhana, 2002;Patience et al, 2002;Udry et al, 2004;Mugrauer et al, 2006;Mugrauer et al, 2007a;Mugrauer et al, 2007b;Raghavan et al, 2006;, Eggenberger et al, 2011Daemgen et al, 2009;Mugrauer and Neuhäuser, 2009;Adams et al, 2012;Adams et al, 2013;Ginski et al, 2012, Ginski et al, 2016Ginski et al, 2020;Lillo-Box et al, 2012;Bergfors et al, 2013;Faedi et al, 2013;Lodieu et al, 2014;Wang et al, 2014;Mugrauer and Ginski, 2015;Wöllert et al, 2015;Deacon et al, 2016;Kraus et al, 2016;Ngo et al, 2016;Ngo et al, 2017;Furlan et al, 2017;Moutou et al, 2017;Coker et al, 2018;Dietrich and Ginski, 2018;Ziegler et al, 2018;Fontanive et al, 2019;Mugrauer, 2019;Bohn et al, 2020;Southworth et al, 2020) or reviews of planets in binaries (Bonavita and Desidera, 2007;Bonavita and Desidera, 2020;…”

Section: Binaries In Surveys and The Literaturementioning

confidence: 99%

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The Census of Exoplanets in Visual Binaries: Population Trends from a Volume-Limited Gaia DR2 and Literature Search

Fontanive

Gagliuffi

2021

Front. Astron. Space Sci.

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We present results from an extensive search in the literature and Gaia DR2 for visual co-moving binary companions to stars hosting exoplanets and brown dwarfs within 200 pc. We found 218 planet hosts out of the 938 in our sample to be part of multiple-star systems, with 10 newly discovered binaries and 2 new tertiary stellar components. This represents an overall raw multiplicity rate of 23.2 ± 1.6 % for hosts to exoplanets across all spectral types, with multi-planet systems found to have a lower stellar duplicity frequency at the 2.2-σ level. We found that more massive hosts are more often in binary configurations, and that planet-bearing stars in multiple systems are predominantly observed to be the most massive component of stellar binaries. Investigations of the multiplicity of planetary systems as a function of planet mass and separation revealed that giant planets with masses above 0.1 MJup are more frequently seen in stellar binaries than small sub-Jovian planets with a 3.6-σ difference, a trend enhanced for the most massive (>7 MJup) short-period (<0.5 AU) planets and brown dwarf companions. Binarity was however found to have no significant effect on the demographics of low- mass planets (<0.1 MJup) or warm and cool gas giants (>0.5 AU). While stellar companion mass appears to have no impact on planet properties, binary separation seems to be an important factor in the resulting structure of planetary systems. Stellar companions on separations <1000 AU can play a role in the formation or evolution of massive, close-in planets, while planets in wider binaries show similar properties to planets orbiting single stars. Finally, our analyses indicate that numerous stellar companions on separations smaller than 1–3 arcsec likely remain undiscovered to this date. Continuous efforts to complete our knowledge of stellar multiplicity on separations of tens to hundreds of AU are essential to confirm the reported trends and further our understanding of the roles played by multiplicity on exoplanets.

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Section: Completeness and Survey Limitationsmentioning

confidence: 77%

Section: Binaries In Surveys and The Literaturementioning

confidence: 99%

The Census of Exoplanets in Visual Binaries: Population Trends from a Volume-Limited Gaia DR2 and Literature Search

Fontanive

Gagliuffi

2021

Front. Astron. Space Sci.

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“…Despite the potential complications for planet formation induced by the gravitational perturbations from the binary, more than 100 planets in binary systems have already been discovered (e.g., Martin 2018;Bonavita & Desidera 2020) 1 . Most of these planets are found to orbit only one of the binary stars (i.e., 'S-type ', i.e., circumstellar planets).…”

Section: Introductionmentioning

confidence: 99%

Gap, shadows, spirals, and streamers: SPHERE observations of binary-disk interactions in GG Tauri A

Keppler

Penzlin

Benisty

et al. 2020

A&A

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Context. A large portion of stars is found to be part of binary or higher-order multiple systems. The ubiquity of planets found around single stars raises the question of whether and how planets in binary systems form. Protoplanetary disks are the birthplaces of planets, and characterizing them is crucial in order to understand the planet formation process. Aims. Our goal is to characterize the morphology of the GG Tau A disk, one of the largest and most massive circumbinary disks. We also aim to trace evidence for binary-disk interactions. Methods. We obtained observations in polarized scattered light of GG Tau A using the SPHERE/IRDIS instrument in the H-band filter. We analyzed the observed disk morphology and substructures. We ran 2D hydrodynamical models to simulate the evolution of the circumbinary ring over the lifetime of the disk. Results. The disk and also the cavity and the inner region are highly structured, with several shadowed regions, spiral structures, and streamer-like filaments. Some of these are detected here for the first time. The streamer-like filaments appear to connect the outer ring with the northern arc. Their azimuthal spacing suggests that they may be generated through periodic perturbations by the binary, which tear off material from the inner edge of the outer disk once during each orbit. By comparing observations to hydrodynamical simulations, we find that the main features, in particular, the gap size, but also the spiral and streamer filaments, can be qualitatively explained by the gravitational interactions of a binary with a semimajor axis of ~35 au on an orbit coplanar with the circumbinary ring.

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“…Despite the drop, the order of the top five candidates for the study remains the same, although changes would be necessary to prioritize repeated observations (see Table 4). However, a more recent study found that although there is reduction in occurrence rate for binaries with a critical radius < 2.5 AU, there is a boosted rate when the critical radius > 3 AU (Bonavita & Desidera 2020, cf. Fontanive & Bardalez Gagliuffi 2021.…”

Section: Discussionmentioning

confidence: 96%

Exoplanets with ELT-METIS I: Estimating the direct imaging exoplanet yield around stars within 6.5 parsecs

Bowens,

Meyer,

Delacroix

et al. 2021

Preprint

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Direct imaging is a powerful exoplanet discovery technique that is complementary to other techniques and offers great promise in the era of 30 meter class telescopes. Space-based transit surveys have revolutionized our understanding of the frequency of planets at small orbital radii around Sun-like stars. The next generation of extremely large ground-based telescopes will have the angular resolution and sensitivity to directly image planets with R < 4R ⊕ around the very nearest stars. Here, we predict yields from a direct imaging survey of a volume-limited sample of Sun-like stars with the Mid-Infrared ELT Imager and Spectrograph (METIS) instrument, planned for the 39 m European Southern Observatory (ESO) Extremely Large Telescope (ELT) that is expected to be operational towards the end of the decade. Using Kepler occurrence rates, a sample of stars with spectral types A-K within 6.5 pc, and simulated contrast curves based on an advanced model of what is achievable from coronagraphic imaging with adaptive optics, we estimated the expected yield from METIS using Monte Carlo simulations. We find the METIS expected yield of planets in the N2 band (10.10 -12.40 µm) is 1.14 planets, which is greater than comparable observations in the L (3.70 -3.95 µm) and M (4.70 -4.90 µm) bands. We also determined a 24.6% chance of detecting at least one Jovian planet in the background limited regime assuming a 1 hour integration. We calculated the yield per star and estimate optimal observing revisit times to increase the yield. We also analyzed a northern hemisphere version of this survey and found there are additional targets worth considering. In conclusion, we present an observing strategy aimed to maximize the possible yield for limited telescope time, resulting in 1.48 expected planets in the N2 band.

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Frequency of Planets in Binaries

Cited by 31 publications

References 103 publications

The Census of Exoplanets in Visual Binaries: Population Trends from a Volume-Limited Gaia DR2 and Literature Search

The Census of Exoplanets in Visual Binaries: Population Trends from a Volume-Limited Gaia DR2 and Literature Search

Gap, shadows, spirals, and streamers: SPHERE observations of binary-disk interactions in GG Tauri A

Exoplanets with ELT-METIS I: Estimating the direct imaging exoplanet yield around stars within 6.5 parsecs

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