The First Circumbinary Planet Discovered with Radial Velocities

Standing, Matthew R.; Lalitha, S.; V., Martin, David; Triaud, A. H. M. J.; Correia, A. C. M.; Coleman, Gavin A. L.; Baycroft, Thomas A.; Kunovac, Vedad; Boisse, I.; Cameron, A. Collier; Dransfield, Georgina; Faria, J. P.; Gillon, M.; Hara, N.; Hellier, C.; Howard, Jonathon; Lane, Ellie; Mardling, Rosemary A.; Maxted, P. F. L.; Miller, Nicola J.; Nelson, Richard P.; Orosz, Jerome A.; Pepe, Franscesco; Santerne, A.; Sebastian, Daniel; Udry, S.; Welsh, William F.

doi:10.48550/arxiv.2301.10794

Cited by 4 publications

(5 citation statements)

References 56 publications

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“…Given the similarity in the binary properties between Kepler-16 and TOI-1338/BEBOP-1c, we can compare the population to the observed planets, finding that the inner planet is well placed amongst the population of super-Earth-Neptune mass planets orbiting just exterior to the zone of dynamical instability, with the outer planet being situated near the edge of surviving planets. Typically such planets that formed were part of a multiple planet system, indicating that there could be additional planets in the system, as has been found by Standing et al (2023).…”

Section: Toi-1338/bebop-1mentioning

confidence: 53%

“…TOI-1338/BEBOP-1 is the first such system found with TESS where a 7R⊕ planet is orbiting near the zone of dynamical instability in a binary system with a similar mass ratio and binary eccentricity to Kepler-16, although the combined binary mass is ∼50% larger than Kepler-16 (Kostov et al 2020). Radial velocity observations from the BEBOP program (Martin et al 2019) have recently discovered an additional ∼ 65 M⊕ planet on a longer period orbit than the transiting planet (Standing et al 2023). The transiting planet seen by TESS was not seen in the radial velocity data yielding an upper mass limit of 22 M⊕.…”

Section: Toi-1338/bebop-1mentioning

confidence: 99%

“…The discovery of the Kepler-47 system of three circumbinary planets (Orosz et al 2012) holds the current record for the largest known multiplicity within a circumbinary system. More recently TESS found a transiting planet orbiting TOI-1338/BEBOP-1 (Kostov et al 2020), whilst radial velocity observations of the system have found an additional planet orbiting further out in the system, whilst also placing an upper limit on the mass of the transiting planet (Standing et al 2023). One interesting feature shared by the majority of the circumbinary planetary systems is that they host a body that Email: gavin.coleman@qmul.ac.uk orbits near to the zone of dynamical instability (Holman & Wiegert 1999), inside of which a planet would be dynamically unstable due to gravitational perturbations from the central binary (see Martin 2018, for a review of discovered circumbinary planets).…”

Section: Introductionmentioning

confidence: 99%

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Global N-body simulations of circumbinary planet formation around Kepler-16 and -34 analogues I: Exploring the pebble accretion scenario

Coleman

Nelson

Triaud

2023

Monthly Notices of the Royal Astronomical Society

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Numerous circumbinary planets have been discovered in surveys of transiting planets. Often, these planets are found to orbit near to the zone of dynamical instability, close to the central binary. The existence of these planets has been explained by hydrodynamical simulations that show that migrating circumbinary planets, embedded in circumbinary discs, halt at the central cavity that is formed by the central binary. Transit surveys are naturally most sensitive to finding circumbinary planets with the shortest orbital periods. The future promise of detecting longer period systems using radial-velocity searches, combined with the anticipated detection of numerous circumbinary planets by ESA’s PLATO mission, points to the need to model and understand the formation and evolution of circumbinary planets in a more general sense than has been considered before. With this goal in mind, we present a newly developed global model of circumbinary planet formation that is based on the mercury6 symplectic N-body integrator, combined with a model for the circumbinary disc and prescriptions for a range of processes involved in planet formation such as pebble accretion, gas envelope accretion and migration. Our results show that under reasonable assumptions, the pebble accretion scenario can produce circumbinary systems that are similar to those observed, and in particular is able to produce planets akin to Kepler-16b and Kepler-34b. Comparing our results to other systems, we find that our models also adequately reproduce such systems, including multi-planet systems. Resonances between neighbouring planets are frequently obtained, whilst ejections of planets by the central binary acts as an effective source of free floating planets.

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Section: Toi-1338/bebop-1mentioning

confidence: 53%

Section: Toi-1338/bebop-1mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Global N-body simulations of circumbinary planet formation around Kepler-16 and -34 analogues I: Exploring the pebble accretion scenario

Coleman

Nelson

Triaud

2023

Monthly Notices of the Royal Astronomical Society

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“…In the current observations, the Kepler-47 system has multiple CBPs but the binary orbit is nearly circular (e < 0.03) and the three Neptune-size planets are nearly coplanar (Orosz et al 2012b,a;Kostov et al 2013). Moreover, the TOI-1338 system has two saturnian CBPs detected by transit and radial velocity methods (Kostov et al 2020;Standing et al 2023), the NN Ser binary system that is comprised of a red dwarf and white dwarf hosts two Jupiter mass CBPs (Mustill et al 2013) and Kepler-451 has three Jupiter mass CBPs (Baran et al 2015;Esmer et al 2022). All of these planets are nearly coplanar to the binary orbital plane.…”

Section: Introductionmentioning

confidence: 57%

Orbital stability of two circumbinary planets around misaligned eccentric binaries

Chen¹,

Lubow²,

Martin³

et al. 2023

Preprint

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With n-body simulations we investigate the stability of tilted circumbinary planetary systems consisting of two nonzero mass planets. The planets are initially in circular orbits that are coplanar to each other, as would be expected if they form in a flat but tilted circumbinary gas disc and decouple from the disc within a time difference that is much less than the disc nodal precession period. We constrain the parameters of stable multiple planet circumbinary systems. Both planet-planet and planet-binary interactions can cause complex planet tilt oscillations which can destabilise the orbits of one or both planets. The system is considerably more unstable than the effects of these individual interactions would suggest, due to the interplay between these two interactions. The stability of the system is sensitive to the binary eccentricity, the orbital tilt and the semi-major axes of the two circumbinary planets. With an inner planet semi-major axis of 5 a b , where a b is semi-major axis of the binary, the system is generally stable if the outer planet is located at 8 a b , beyond the 2:1 mean motion resonance with the inner planet. For larger inner planet semi-major axis the system is less stable because the von-Zeipel-Kozai-Lidov mechanism plays a significant role, particularly for low binary-eccentricity cases. For the unstable cases, the most likely outcome is that one planet is ejected and the other remains bound on a highly eccentric orbit. Therefore we suggest that this instability is an efficient mechanism for producing free-floating planets.

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“…TIC 172900988 b; Kostov et al 2021). The first P-type planet discovered purely through RVs, TOI-1338/BEBOP-1 c, was also recently announced by Standing et al (2023). Despite these discoveries, no planets have yet been found with orbits of the scale of ∼ 3 au around a ∼ 1 au binary.…”

Section: Introductionmentioning

confidence: 99%

DMPP-3: confirmation of short-period S-type planet(s) in a compact eccentric binary star system, and warnings about long-period RV planet detections

Stevenson,

Haswell,

Barnes

et al. 2023

Monthly Notices of the Royal Astronomical Society

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We present additional HARPS radial velocity observations of the highly eccentric (e ∼ 0.6) binary system DMPP-3AB, which comprises a K0V primary and a low-mass companion at the hydrogen burning limit. The binary has a 507 d orbital period and a 1.2 au semi-major axis. The primary component harbours a known 2.2 M⊕ planet, DMPP-3A b, with a 6.67 day orbit. New HARPS measurements constrain periastron passage for the binary orbit and add further integrity to previously derived solutions for both companion and planet orbits. Gaia astrometry independently confirms the binary orbit, and establishes the inclination of the binary is 63.89 ± 0.78○. We performed dynamical simulations which establish that the previously identified ∼800 d RV signal cannot be attributed to an orbiting body. The additional observations, a deviation from strict periodicity, and our new analyses of activity indicators suggest the ∼800 d signal is caused by stellar activity. We conclude that there may be long period planet “detections” in other systems which are similar misinterpreted stellar activity artefacts. Without the unusual eccentric binary companion to the planet-hosting star we could have accepted the ∼800 d signal as a probable planet. Further monitoring of DMPP-3 will reveal which signatures can be used to most efficiently identify these imposters. We also report a threshold detection (0.2 per cent FAP) of a ∼2.26 d periodicity in the RVs, potentially attributed to an Earth-mass S-type planet interior to DMPP-3A b.

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The First Circumbinary Planet Discovered with Radial Velocities

Cited by 4 publications

References 56 publications

Global N-body simulations of circumbinary planet formation around Kepler-16 and -34 analogues I: Exploring the pebble accretion scenario

Global N-body simulations of circumbinary planet formation around Kepler-16 and -34 analogues I: Exploring the pebble accretion scenario

Orbital stability of two circumbinary planets around misaligned eccentric binaries

DMPP-3: confirmation of short-period S-type planet(s) in a compact eccentric binary star system, and warnings about long-period RV planet detections

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