Lucky planets: how circum-binary planets survive the supernova in one of  the inner-binary components

Auer, Fedde Fagginger; Zwart, Simon Portegies

doi:10.21468/scipostastro.2.1.002

Cited by 3 publications

(2 citation statements)

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“…In the first scenario, the survival of a planet in a stable orbit is questionable, since neutron stars (NS) form in violent type II supernova explosions (SN II) (see e.g. Podsiadlowski 1993;Veras et al 2011;Fagginger Auer & Portegies Zwart 2022). Moreover, in this case, a massive planet-hosting progenitor is required, at least 8M , which is much higher than the largest planet-hosting star observed today.…”

Section: Introductionmentioning

confidence: 99%

Lost in space: companions' fatal dance around massive dying stars

Regály¹,

Viktoria²,

Vinkó³

2022

Preprint

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Discoveries of planet-and stellar remnant-hosting pulsars challenge our understanding as the violent supernova explosion that forms the pulsar presumably destabilizes the system. Type II supernova explosions lead to the formation of eccentric bound systems, free-floating planets, neutron stars, pulsars, and white dwarfs. Analytical and numerical studies of high mass-loss rate systems based on perturbation theory so far have focused mainly on planet-star systems. In this paper, we extend our understanding of the fate of planet-star and binary systems by assuming a homologous envelope expansion model using a plausible ejection velocity (1000 − 10000 km/s), envelope-and neutron star masses. The investigation covers secondary masses of 1 − 10 M J for planetary, and 1 − 20 M for stellar companions. We conduct and analyze over 2.5 million simulations assuming different semi-major axes (2.23−100 au), eccentricities (0−0.8), and true-anomalies (0−2π) for the companion. In a homologous expansion scenario, we confirm that the most probable outcome of the explosion is the destabilization of the system, while the retention of a bound system requires a highly eccentric primordial orbit. In general, a higher ejecta velocity results in a lower eccentricity orbit independent of secondary mass. The explanation of close-in pulsar planets requires exotic formation scenarios, rather than survival through the type II supernova explosion model. Post-explosion bound star systems gain a peculiar velocity (<100 km/s), even though the explosion model is symmetric. The applied numerical model allows us to derive velocity components for dissociating systems. The peculiar velocities of free-floating planets and stellar corpses are in the range of 10 −6 − 275 km/s.

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Section: Introductionmentioning

confidence: 99%

Lost in space: companions' fatal dance around massive dying stars

Regály¹,

Viktoria²,

Vinkó³

2022

Preprint

View full text Add to dashboard Cite

show abstract

“…The existence of planets and especially planetary systems around stellar remnants challenges our understanding. In the first scenario, the survival of a planet in a stable orbit is questionable, since neutron stars (NSs) form in violent type II supernova explosions (SN II; see, e.g., Podsiadlowski 1993;Veras et al 2011;Fagginger Auer & Portegies Zwart 2022). Moreover, in this case, a massive planet-hosting progenitor is required, at least 8M e , which is much higher than the largest planet-hosting star observed today.…”

Section: Introductionmentioning

confidence: 99%

Lost in Space: Companions’ Fatal Dance around Massive Dying Stars

Regály

Viktoria

Vinkó

2022

ApJ

View full text Add to dashboard Cite

Discoveries of planet and stellar remnant hosting pulsars challenge our understanding, as the violent supernova explosion that forms the pulsar presumably destabilizes the system. Type II supernova explosions lead to the formation of eccentric bound systems, free-floating planets, neutron stars, pulsars, and white dwarfs. Analytical and numerical studies of high mass-loss rate systems based on perturbation theory so far have focused mainly on planet-star systems. In this paper, we extend our understanding of the fate of planet-star and binary systems by assuming a homologous envelope expansion model using a plausible ejection velocity (1000–10,000 km s−1), and envelope and neutron star masses. The investigation covers secondary masses of 1–10 M J for planetary companions and 1–20 M ⊙ for stellar companions. We conduct and analyze over 2.5 million simulations assuming different semimajor axes (2.23–100 au), eccentricities (0–0.8), and true anomalies (0–2π) for the companion. In a homologous expansion scenario, we confirm that the most probable outcome of the explosion is the destabilization of the system, while the retention of a bound system requires a highly eccentric primordial orbit. In general, a higher ejecta velocity results in a lower eccentricity orbit independent of secondary mass. The explanation of close-in pulsar planets requires exotic formation scenarios, rather than survival through the type II supernova explosion model. Postexplosion bound star systems gain a peculiar velocity (<100 km s−1), even though the explosion model is symmetric. The applied numerical model allows us to derive velocity components for dissociating systems. The peculiar velocities of free-floating planets and stellar corpses are in the range of 10−6–275 km s−1.

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Statistics of Magrathea exoplanets beyond the main sequence

Columba,

Danielski,

Dorozsmai

et al. 2023

A&A

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Context. Notwithstanding the tremendous growth of the field of exoplanets in the last decade, limited attention has been paid to the planets around binary stars, which represent a small fraction of the total discoveries to date. Circumbinary planets (CBPs) have been discovered primarily with transit and eclipse timing variation methods, mainly around main sequence (MS) stars. No exoplanet has been found orbiting double white dwarf (DWD) binaries yet. Aims. In the interest of expanding our understanding of the final fate of CBPs, we modelled their long-term evolution, throughout the life stages of their hosts, from the MS to WD. Our goal is to provide the community with theoretical constraints on the evolution of CBPs beyond the MS and with the occurrence rates of planet survival throughout the ageing of the systems. Methods. We further developed the publicly available Triple Evolution Simulation (TRES) code, to adapt it to the mass range of sub-stellar objects (SSOs). We did so by implementing a variety of physical processes that affect giant planets and brown dwarfs. We used TRES to simulate the evolution, up to one Hubble time, of two synthetic populations of circumbinary giant planets. Each population was generated using different priors for the planetary orbital parameters. Results. In our simulated populations we identified several evolutionary categories, such as survived, merged, and destabilised systems. Our primary interest is those systems in which the planet survived the WD formation of both stars in the binary. We named these planets Magrathea. We found that a significant fraction of simulated CBPs survive the entire system evolution and become Magratheas, regardless of their mass. In the absence of multi-planet migration mechanisms, this category of CBPs is characterised by long orbital periods. Conclusions. Magrathea planets are a natural outcome of triple-system evolution, and our study indicates that they should be relatively common in the Galaxy. These gas giants can survive the death of their binary hosts if they orbit far enough away to avoid engulfment and instabilities. Our results can ultimately be a reference to orient future observations of this uncharted class of planets and to compare different theoretical models.

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Lucky planets: how circum-binary planets survive the supernova in one of the inner-binary components

Cited by 3 publications

References 35 publications

Lost in space: companions' fatal dance around massive dying stars

Lost in space: companions' fatal dance around massive dying stars

Lost in Space: Companions’ Fatal Dance around Massive Dying Stars

Statistics of Magrathea exoplanets beyond the main sequence

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