Misaligned Circumbinary Disks as Efficient Progenitors of Interstellar Asteroids

Childs, Anna C.; Martin, Rebecca G.

doi:10.3847/2041-8213/ac8880

Cited by 9 publications

(6 citation statements)

References 69 publications

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“…Formation of terrestrial planets from a misaligned disc of planetestimals after the gas disc has dissipated may also be difficult, unless the disc is close to coplanar or polar alignment (Childs & Martin 2021a,b, 2022a. A highly misaligned disc of planetesimals around a binary may be largely ejected (Childs & Martin 2022b). Therefore, multiple low mass CBP systems may be not applicable for our study.…”

Section: Discussionmentioning

confidence: 99%

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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Section: Discussionmentioning

confidence: 99%

Orbital stability of two circumbinary planets around misaligned eccentric binaries

Chen¹,

Lubow²,

Martin³

et al. 2023

Preprint

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“…Detailed studies by Veras & Tout (2012) and Veras et al (2014) found that exocomets are more likely to escape from post-main-sequence binaries than from single stars, especially for wide-separation and eccentric stellar companions. Notably, binary stars have been proposed as prolific producers of interstellar small bodies (Ćuk 2018;Jackson et al 2018;Childs & Martin 2022) during the (pre-)main-sequence. Planetary perturbers could similarly affect ejection fractions, and indeed a population of giant planets is required to generate the initial exo-Oort Clouds (Dones et al 2004).…”

Section: Other Dynamical Considerationsmentioning

confidence: 99%

Interstellar Comets from Post-main-sequence Systems as Tracers of Extrasolar Oort Clouds

et al. 2023

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Interstellar small bodies are unique probes into the histories of exoplanetary systems. One hypothesized class of interlopers are “Jurads,” exocomets released into the Milky Way during the post-main-sequence as the thermally pulsing asymptotic giant branch (AGB) host stars lose mass. In this study, we assess the prospects for the Legacy Survey of Space and Time (LSST) to detect a Jurad and examine whether such an interloper would be observationally distinguishable from exocomets ejected during the (pre-)main-sequence. Using analytic and numerical methods, we estimate the fraction of exo–Oort Cloud objects that are released from 1–8 M ⊙ stars during post-main-sequence evolution. We quantify the extent to which small bodies are altered by the increased luminosity and stellar outflows during the AGB, finding that some Jurads may lack hypervolatiles and that stellar winds could deposit dust that covers the entire exocomet surface. Next, we construct models of the interstellar small body reservoir for various size–frequency distributions and examine the LSST’s ability to detect members of those hypothesized populations. Combining these analyses, we highlight the joint constraints that the LSST will place on power-law size–frequency distribution slopes, characteristic sizes, and the total mass sequestered in the minor planets of exo–Oort Clouds. Even with the LSST’s increased search volume compared to contemporary surveys, we find that detecting a Jurad is unlikely but not infeasible given the current understanding of (exo)planet formation.

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“…Even widely spaced planetary systems can be unstable around a tilted binary (see Section 2.2). Thus the ejection of planets from a misaligned binary system can be far more efficient compared to a single star or coplanar binary system (see also Childs & Martin 2022).…”

Section: Introductionmentioning

confidence: 99%

Tilted Circumbinary Planetary Systems as Efficient Progenitors of Free-floating Planets

Chen,

Martin,

Lubow

et al. 2024

ApJL

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The dominant mechanism for generating free-floating planets has so far remained elusive. One suggested mechanism is that planets are ejected from planetary systems due to planet–planet interactions. Instability around a single star requires a very compactly spaced planetary system. We find that around binary star systems instability can occur even with widely separated planets that are on tilted orbits relative to the binary orbit due to combined effects of planet–binary and planet–planet interactions, especially if the binary is on an eccentric orbit. We investigate the orbital stability of planetary systems with various planet masses and architectures. We find that the stability of the system depends upon the mass of the highest-mass planet. The order of the planets in the system does not significantly affect stability, but, generally, the most massive planet remains stable and the lower-mass planets are ejected. The minimum planet mass required to trigger the instability is about that of Neptune for a circular orbit binary and a super-Earth of about 10 Earth masses for highly eccentric binaries. Hence, we suggest that planet formation around inclined binaries can be an efficient formation mechanism for free-floating planets. While most observed free-floating planets are giant planets, we predict that there should be more low-mass free-floating planets that are as of yet unobserved than higher-mass planets.

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Misaligned Circumbinary Disks as Efficient Progenitors of Interstellar Asteroids

Cited by 9 publications

References 69 publications

Orbital stability of two circumbinary planets around misaligned eccentric binaries

Orbital stability of two circumbinary planets around misaligned eccentric binaries

Interstellar Comets from Post-main-sequence Systems as Tracers of Extrasolar Oort Clouds

Tilted Circumbinary Planetary Systems as Efficient Progenitors of Free-floating Planets

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