How the planetary eccentricity influences the pebble isolation mass
The result's identifiers
Result code in IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F22%3A10456637" target="_blank" >RIV/00216208:11320/22:10456637 - isvavai.cz</a>
Result on the web
<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=0L9kCIdTRu" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=0L9kCIdTRu</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.1093/mnras/stab3753" target="_blank" >10.1093/mnras/stab3753</a>
Alternative languages
Result language
angličtina
Original language name
How the planetary eccentricity influences the pebble isolation mass
Original language description
We investigate the pebble isolation mass (PIM) for a planet on a fixed eccentric orbit in its protoplanetary disc by conducting a set of two-dimensional (2D) hydrodynamical simulations, including dust turbulent diffusion. A range of planet eccentricities up to e = 0.2 is adopted. Our simulations also cover a range of a-turbulent viscosities, and for each pair {alpha, e} the PIM is estimated as the minimum planet mass in our simulations such that solids with a Stokes number greater than or similar to 0.05 do not flow across the planet orbit and remain trapped around a pressure bump outside the planet gap. For alpha < 10(-3), we find that eccentric planets reach a well-defined PIM, which can be smaller than for planets on circular orbits when the eccentricity remains smaller than the disc's aspect ratio. We provide a fitting formula for how the PIM depends on the planet's eccentricity. However, for alpha > 10(-3), eccentric planets cannot fully stall the pebbles flow and, thus, do not reach a well-defined PIM. Our results suggest that the maximum mass reached by rocky cores should exhibit a dichotomy depending on the disc's turbulent viscosity. While being limited to O(10 M-circle plus) in low-viscosity discs, this maximum mass could reach much larger values in discs with a high turbulent viscosity in the planet vicinity. Our results further highlight that pebble filtering by growing planets might not be as effective as previously thought, especially in high-viscosity discs, with important implications to protoplanetary discs observations.
Czech name
—
Czech description
—
Classification
Type
J<sub>imp</sub> - Article in a specialist periodical, which is included in the Web of Science database
CEP classification
—
OECD FORD branch
10308 - Astronomy (including astrophysics,space science)
Result continuities
Project
<a href="/en/project/GM21-23067M" target="_blank" >GM21-23067M: Hydrodynamic interactions of planets with protoplanetary disks and the origin of close-in exoplanetary systems</a><br>
Continuities
P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)
Others
Publication year
2022
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Data specific for result type
Name of the periodical
Monthly Notices of the Royal Astronomical Society
ISSN
0035-8711
e-ISSN
1365-2966
Volume of the periodical
510
Issue of the periodical within the volume
3
Country of publishing house
GB - UNITED KINGDOM
Number of pages
9
Pages from-to
3867-3875
UT code for WoS article
000749577000050
EID of the result in the Scopus database
2-s2.0-85126825520