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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 &lt; 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&apos;s aspect ratio. We provide a fitting formula for how the PIM depends on the planet&apos;s eccentricity. However, for alpha &gt; 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&apos;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