Constraining planet formation around 6-8 M&amp;#9737; stars

Veras, Dimitri; Tremblay, Pier-Emmanuel; Hermes, J. J.; McDonald, Catriona; Kennedy, Grant; Meru, Farzana; Gänsicke, B. T.

doi:10.5194/epsc2020-412

Cited by 1 publication

(1 citation statement)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The reservoirs of bodies smaller than exo-asteroids, however, remain largely unexplored. Some of these reservoirs will carry over from the giant branch phase of stellar evolution (Bonsor & Wyatt 2010;Martin et al 2020;Veras et al 2020b), where the enhanced stellar luminosity will easily spin up 100 m -10 km bodies within 7 au to their breaking point due to the YORP effect (Veras et al 2014b;Veras & Scheeres 2020). Further, extant debris discs from main sequence evolution have been observed orbiting giant stars at distances of tens of au (Bonsor et al 2013(Bonsor et al , 2014.…”

Section: Small Body Reservoirsmentioning

confidence: 99%

Generating metal-polluting debris in white dwarf planetary systems from small-impact crater ejecta

Veras

Kurosawa

2020

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

Metal pollution in white dwarf photospheres originates from the accretion of some combination of planets, moons, asteroids, comets, boulders, pebbles and dust. When large bodies reside in dynamically stagnant locations -unable themselves to pollute nor even closely approach the white dwarf -then smaller reservoirs of impact debris may become a complementary or the primary source of metal pollutants. Here, we take a first step towards exploring this possibility by computing limits on the recoil mass that escapes the gravitational pull of the target object following a single impact onto an atmosphere-less surface. By considering vertical impacts only with the full-chain analytical prescription from Kurosawa & Takada (2019), we provide lower bounds for the ejected mass for basalt, granite, iron and water-rich target objects across the radii range 10 0−3 km. Our use of the full-chain prescription as opposed to physical experiments or hydrocode simulations allows us to quickly sample a wide range of parameter space appropriate to white dwarf planetary systems. Our numerical results could be used in future studies to constrain freshly-generated small debris reservoirs around white dwarfs given a particular planetary system architecture, bombardment history, and impact geometries.

show abstract