Orbital Stability of Circumstellar Planets in Binary Systems

Quarles, Billy; Li, Gongjie; Kostov, Veselin B.; Haghighipour, Nader

doi:10.3847/1538-3881/ab64fa

Cited by 44 publications

(55 citation statements)

References 101 publications

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“…Being expelled from the binary star system is likely not conducive to planetary habitability. Since then, a substantial body of work has been dedicated to investigating the stability of planets in binary star systems (e.g., [26][27][28][29][30][31][32][33][34][35][36][37][38][39][40][41]). Among many other important results, it has been found that stable orbits are possible in the vicinity of circumstellar and circumbinary habitable zones, but that much depends on the exact setup of the systems involved.…”

Section: The Trouble With Two Starsmentioning

confidence: 99%

Habitable Zones in Binary Star Systems: A Zoology

Eggl

Georgakarakos²,

Pilat-Lohinger

2020

Galaxies

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Several concepts have been brought forward to determine where terrestrial planets are likely to remain habitable in multi-stellar environments. Isophote-based habitable zones, for instance, rely on insolation geometry to predict habitability, whereas radiative habitable zones take the orbital motion of a potentially habitable planet into account. Dynamically informed habitable zones include gravitational perturbations on planetary orbits, and full scale, self consistent simulations promise detailed insights into the evolution of select terrestrial worlds. All of the above approaches agree that stellar multiplicity does not preclude habitability. Predictions on where to look for habitable worlds in such environments can differ between concepts. The aim of this article is to provide an overview of current approaches and present simple analytic estimates for the various types of habitable zones in binary star systems.

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Section: The Trouble With Two Starsmentioning

confidence: 99%

Habitable Zones in Binary Star Systems: A Zoology

Eggl

Georgakarakos²,

Pilat-Lohinger

2020

Galaxies

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“…The closer a CBP is to a crit , the higher the amplitudes in a cbp and e cbp become, therefore the change in their amplitudes can vary more significantly, too. Additional research could also explore the role of inclination, which has can cause deviations from the Holman & Wiegert (1999) stability limit (Pilat-Lohinger et al 2003;Quarles et al 2020) and can significantly alter CBP orbital evolution, presumably affecting STEEP and habitability.…”

Section: Discussionmentioning

confidence: 99%

Orbital evolution of potentially habitable planets of tidally interacting binary stars

Graham

Fleming

Barnes

2021

A&A

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We simulate the coupled stellar and tidal evolution of short-period binary stars (orbital period P orb < ∼ 8 days) to investigate the orbital oscillations, instellation cycles, and orbital stability of circumbinary planets (CBPs). We consider two tidal models and show that both predict an outward-then-inward evolution of the binary's semi-major axis a bin and eccentricity e bin. This orbital evolution drives a similar evolution of the minimum CBP semi-major axis for orbital stability. By expanding on previous models to include the evolution of the mass concentration, we show that the maximum in the CBP orbital stability limit tends to occur 100 Myr after the planets form, a factor of 100 longer than previous investigations. This result provides further support for the hypothesis that the early stellar-tidal evolution of binary stars has removed CBPs from short-period binaries. We then apply the models to Kepler-47 b, a CBP orbiting close to its host stars' stability limit, to show that if the binary's initial e bin > ∼ 0.24, the planet would have been orbiting within the instability zone in the past and probably wouldn't have survived. For stable, hypothetical cases in which the stability limit does not reach a planet's orbit, we find that the amplitudes of a bin and e bin oscillations can damp by up to 10% and 50%, respectively. Finally, we consider equal-mass stars with P orb = 7.5 days and compare the HZ to the stability limit. We find that for stellar masses < ∼ 0.12M , the HZ is completely unstable, even if the binary orbit is circular. For e bin < ∼ 0.5, that limit increases to 0.17M , and the HZ is partially destabilized for stellar masses up to 0.45M. These results may help guide searches for potentially habitable CBPs, as well as characterize their evolution and likelihood to support life after they are found.

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“…Despite the fact that more recent studies by Baraffe et al (2015) and Forbes & Loeb (2019) show that the deuteriumburning limit is 73-74 M Jup , we take the older upper limit of 80 M Jup determined by Saumon & Marley (2008) to be inclusive of higher masses. Quarles et al (2020) find that for a companion to remain bound to its host in a binary star system with a bin , the orbit of the companion must have a/a bin <0.08 for a prograde orbit. For a retrograde orbit, this fraction increases to 0.10.…”

Section: Periodicitymentioning

confidence: 93%

An Asymmetric Eclipse Seen toward the Pre-main-sequence Binary System V928 Tau

Dam

Kenworthy

Mamajek

et al. 2020

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K2 observations of the weak-lined T Tauri binary V928 Tau A and B show the detection of a single, asymmetric eclipse, which may be due to a previously unknown substellar companion eclipsing one component of the binary with an orbital period >66 days. Over an interval of about 9 hr, one component of the binary dims by around 60%, returning to its normal brightness about 5 hr later. From modeling of the eclipse shape, we find evidence that the eclipsing companion may be surrounded by a disk or a vast ring system. The modeled disk has a radius of 0.9923±0.0005 R * , with an inclination of 56°.78±0°. 03, a tilt of 41°.22±0°. 05, an impact parameter of −0.2506±0.0002 R * , and an opacity of 1.00. The occulting disk must also move at a transverse velocity of 6.637±0.002 R * day −1 , which, depending on whether it orbits V928 Tau A or B, corresponds to approximately 73.53 or 69.26 km s −1. A search in ground-based archival data reveals additional dimming events, some of which suggest periodicity, but no unambiguous period associated with the eclipse observed by K2. We present a new epoch of astrometry that is used to further refine the orbit of the binary, presenting a new lower bound of 67 yr, and constraints on the possible orbital periods of the eclipsing companion. The binary is also separated by 18″ (∼2250 au) from the lower-mass CFHT-BD-Tau 7, which is likely associated with V928 Tau A and B. We also present new high-dispersion optical spectroscopy that we use to characterize the unresolved stellar binary.

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Orbital Stability of Circumstellar Planets in Binary Systems

Cited by 44 publications

References 101 publications

Habitable Zones in Binary Star Systems: A Zoology

Habitable Zones in Binary Star Systems: A Zoology

Orbital evolution of potentially habitable planets of tidally interacting binary stars

An Asymmetric Eclipse Seen toward the Pre-main-sequence Binary System V928 Tau

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