Speeding past planets? Asteroids radiatively propelled by giant branch Yarkovsky effects

Veras, Dimitri; Higuchi, Arika; Ida, Shigeru

doi:10.1093/mnras/stz421

Cited by 35 publications

(42 citation statements)

References 125 publications

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“…Rozitis & Green 2012Cotto-Figueroa et al 2015;Yu et al 2018;Hirabayashi & Scheeres 2019). Contrastingly, only a handful of basic dedicated extrasolar post-main-sequence studies have been published for the Yarkovsky effect (Veras et al 2015a(Veras et al , 2019b and the YORP effect (Veras et al 2014a;Veras & Scheeres 2020).…”

Section: Minor Planet Survivalmentioning

confidence: 99%

Constraining planet formation around 6–8 M⊙ stars

Veras

Tremblay

Hermes

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Identifying planets around O-type and B-type stars is inherently difficult; the most massive known planet host has a mass of only about 3M ⊙ . However, planetary systems which survive the transformation of their host stars into white dwarfs can be detected via photospheric trace metals, circumstellar dusty and gaseous discs, and transits of planetary debris crossing our line-of-sight. These signatures offer the potential to explore the efficiency of planet formation for host stars with masses up to the corecollapse boundary at ≈ 8M ⊙ , a mass regime rarely investigated in planet formation theory. Here, we establish limits on where both major and minor planets must reside around ≈ 6M ⊙ − 8M ⊙ stars in order to survive into the white dwarf phase. For this mass range, we find that intact terrestrial or giant planets need to leave the main sequence beyond approximate minimum star-planet separations of respectively about 3 and 6 au. In these systems, rubble pile minor planets of radii 10, 1.0, and 0.1 km would have been shorn apart by giant branch radiative YORP spin-up if they formed and remained within, respectively, tens, hundreds and thousands of au. These boundary values would help distinguish the nature of the progenitor of metal-pollution in white dwarf atmospheres. We find that planet formation around the highest mass white dwarf progenitors may be feasible, and hence encourage both dedicated planet formation investigations for these systems and spectroscopic analyses of the highest mass white dwarfs.

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Section: Minor Planet Survivalmentioning

confidence: 99%

Constraining planet formation around 6–8 M⊙ stars

Veras

Tremblay

Hermes

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…The interaction is complex since it depends upon the shape, orientation and albedo of each asteroid. Asteroids can be radiatively pushed by the Yarkovsky effect (Bottke et al 2001(Bottke et al , 2006Veras et al 2019). The Yarkovsky drift may be several orders of magnitude larger than that from Poynting-Robertson and radiation pressure (Veras et al 2015a).…”

Section: Planetesimal Survivalmentioning

confidence: 99%

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

Martin

Livio

Smallwood

et al. 2020

Monthly Notices of the Royal Astronomical Society: Letters

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Polluted white dwarfs are generally accreting terrestrial-like material that may originate from a debris belt like the asteroid belt in the solar system. The fraction of white dwarfs that are polluted drops off significantly for white dwarfs with masses M WD 0.8 M ⊙ . This implies that asteroid belts and planetary systems around main-sequence stars with mass M MS 3 M ⊙ may not form because of the intense radiation from the star. This is in agreement with current debris disc and exoplanet observations. The fraction of white dwarfs that show pollution also drops off significantly for low mass white dwarfs (M WD 0.55 M ⊙ ). However, the low-mass white dwarfs that do show pollution are not currently accreting but have accreted in the past. We suggest that asteroid belts around main sequence stars with masses M MS 2 M ⊙ are not likely to survive the stellar evolution process. The destruction likely occurs during the AGB phase and could be the result of interactions of the asteroids with the stellar wind, the high radiation or, for the lowest mass stars that have an unusually close-in asteroid belt, scattering during the tidal orbital decay of the inner planetary system.

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“…However, investigations which have considered the interaction between major planets and smaller bodies during this stellar phase have generally treated the smaller bodies as point particles. Few investigations have studied the combined effect of giant branch stellar radiation, mass loss and planetary perturbations on finite-sized small bodies (Dong et al 2010;Veras, Higuchi & Ida 2019). Here we also analyze this situation, but from a different perspective: through the photogravitational planar restricted three-body problem (PPRTBP).…”

Section: Introductionmentioning

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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Speeding past planets? Asteroids radiatively propelled by giant branch Yarkovsky effects

Cited by 35 publications

References 125 publications

Constraining planet formation around 6–8 M⊙ stars

Constraining planet formation around 6–8 M⊙ stars

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

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

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