Asteroid belt survival through stellar evolution: dependence on the stellar mass

Martin, Rebecca G.; Livio, Mario; Smallwood, Jeremy L.; Chen, Cheng

doi:10.1093/mnrasl/slaa030

Cited by 12 publications

(5 citation statements)

References 89 publications

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“…Not included in our computations were the interactions between the stellar wind and the grains, an effect which has been studied in giant star planetary sytems for decades (e.g., Livio & Soker 1984;Martin et al 2020). Dong et al (2010) estimated that the critical grain size below which entrainment is possible is a function of the density and speed of the wind as well at those of the grain.…”

Section: Discussionmentioning

confidence: 99%

The grain size survival threshold in one-planet post-main-sequence exoplanetary systems

Zotos

Veras

2020

A&A

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The size distribution and orbital architecture of dust, grains, boulders, asteroids, and major planets during the giant branch phases of evolution dictate the preponderance and observability of the eventual debris, which have been found to surround white dwarfs and pollute their atmospheres with metals. Here, we utilize the photogravitational planar restricted three-body problem in one-planet giant branch systems in order to characterize the orbits of grains as the parent star luminosity and mass undergo drastic changes. We perform a detailed dynamical analysis of the character of grain orbits (collisional, escape, or bounded) as a function of location and energy throughout giant branch evolution. We find that for stars with main-sequence masses of 2.0 M⊙, giant branch evolution, combined with the presence of a planet, ubiquitously triggers escape in grains smaller than about 1 mm, while leaving grains larger than about 5 cm bound to the star. This result is applicable for systems with either a terrestrial or giant planet, is largely independent of the location of the planet, and helps establish a radiative size threshold for escape of small particles in giant branch planetary systems.

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Section: Discussionmentioning

confidence: 99%

The grain size survival threshold in one-planet post-main-sequence exoplanetary systems

Zotos

Veras

2020

A&A

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“…Thus, given a planetesimal belt similar in mass to the present-day asteroid belt, secular chaos driven by planets larger than ∼ 10M⊕ beyond ∼ 10 au can sustain metal ac-cretion rates consistent with observations across most of the WD cooling sequence. The amount of mass that is expected to remain in a planetesimal belt after stellar evolution is uncertain, although some theoretical limits exist for the post-MS survival of planetesimals as a function of size, location, and stellar mass (e.g., Bonsor & Wyatt 2010;Veras et al 2014;Martin et al 2020). However, it is encouraging that the accretion rates produced by secular chaos broadly agree with observations given only the mass of the Solar System asteroid belt.…”

Section: Metal Accretion Rate Vs Cooling Agementioning

confidence: 99%

Secular chaos in white-dwarf planetary systems: origins of metal pollution and short-period planetary companions

O'Connor,

Teyssandier,

Lai

2021

Preprint

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Secular oscillations in multi-planet systems can drive chaotic evolution of an inner body through non-linear resonant perturbations. This "secular chaos" readily pushes the particle to an extreme eccentricity, triggering tidal interactions or collision with the central star. We present a numerical study of secular chaos in systems with two planets and a test particle using the ring-averaging method, with emphasis on the relationship between the planets' properties and the time-scale of chaotic diffusion. We find that secular chaos can excite extreme eccentricities on time-scales spanning several orders of magnitude in a given system. We apply our results to the evolution of planetary systems around white dwarfs (WDs), specifically the tidal disruption and high-eccentricity migration of planetesimals and planets. We find that secular chaos driven by large ( 10M ⊕ ), distant ( 10 au) planets can sustain metal accretion onto the WD from tidal disruption of planetesimals over Gyr time-scales. The accretion rate is consistent with that inferred for WDs with atmospheric pollution along the cooling sequence if the total mass of planetesimals in the chaotic zone at the beginning of the WD stage is similar to that of the Solar System's main asteroid belt. Based on the occurrence of long-period exoplanets and exo-asteroid belts, we conclude that secular chaos can be a significant (perhaps dominant) channel for polluting WDs. Secular chaos can also produce short-period planets and planetesimals around WDs in concert with various circularization mechanisms. We discuss prospects for detecting exoplanets driving secular chaos using direct imaging and microlensing.

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“…The prevailing scenario for the provision of long term accretion of metal-rich material is that planetary debris are excited onto star-grazing orbits and ultimately become disintegrated by tidal forces, forming a debris disc around the white dwarf (Gänsicke et al 2006;Kilic et al 2006;von Hippel et al 2007;Farihi et al 2009;Jura et al 2009;Farihi et al 2010a;Melis et al 2010;Brown et al 2017;Bonsor et al 2017;Xu et al 2018a;Debes et al 2019;Wilson et al 2019). The planetary debris that have been hypothesized as a source include asteroids (Jura 2003(Jura , 2006Jura et al 2009;Debes et al 2012;Veras et al 2013b;Wyatt et al 2014;Frewen & Hansen 2014;Smallwood et al 2018b;Mustill et al 2018;Makarov & Veras 2019;Martin et al 2020), comets (Veras et al 2014b;Stone et al 2015;Caiazzo & Heyl 2017), and moons (Payne et al 2016(Payne et al , 2017. There is also evidence for pollution of the atmospheres of white dwarfs in close-in binaries which contain a circumbinary debris disc (Farihi et al 2017).…”

Section: Introductionmentioning

confidence: 99%

On the role of resonances in polluting white dwarfs by asteroids

Smallwood,

Martin,

Livio

et al. 2021

Preprint

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Pollution of white dwarf atmospheres may be caused by asteroids that originate from the locations of secular and mean-motion resonances in planetary systems. Asteroids in these locations experience increased eccentricity, leading to tidal disruption by the white dwarf. We examine how the ν 6 secular resonance shifts outwards into a previously stable region of the asteroid belt, as the star evolves to a white dwarf. Analytic secular models require a planet to be engulfed in order to shift the resonance. We show with numerical simulations that as a planet gets engulfed by the evolving star, the secular resonance shifts and the rate of tidal disruption events increases with the engulfed planet's mass and its orbital separation. We also investigate the behaviour of mean-motion resonances. The width of a mean-motion resonance increases as the star loses mass and becomes a white dwarf. The ν 6 secular resonance is more efficient at driving tidal disruptions than mean-motion resonances with Jupiter. By examining 230 observed exoplanetary systems whose central star will evolve into a white dwarf, we find that along with an Earth mass planet at 1 au, hot Jupiters at a semi-major axis a 0.05 au and super-Earths of mass 10 M ⊕ at a 0.3 au represent planet types whose engulfment shifts resonances enough to cause pollution of the white dwarfs to a degree in agreement with observations.

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Asteroid belt survival through stellar evolution: dependence on the stellar mass

Cited by 12 publications

References 89 publications

The grain size survival threshold in one-planet post-main-sequence exoplanetary systems

The grain size survival threshold in one-planet post-main-sequence exoplanetary systems

Secular chaos in white-dwarf planetary systems: origins of metal pollution and short-period planetary companions

On the role of resonances in polluting white dwarfs by asteroids

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