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Binary Planet Formation by Gas-assisted Encounters of Planetary Embryos

The result's identifiers

  • Result code in IS VaVaI

    <a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F18%3A10391431" target="_blank" >RIV/00216208:11320/18:10391431 - isvavai.cz</a>

  • Result on the web

    <a href="https://doi.org/10.3847/1538-4357aaeb93" target="_blank" >https://doi.org/10.3847/1538-4357aaeb93</a>

  • DOI - Digital Object Identifier

    <a href="http://dx.doi.org/10.3847/1538-4357aaeb93" target="_blank" >10.3847/1538-4357aaeb93</a>

Alternative languages

  • Result language

    angličtina

  • Original language name

    Binary Planet Formation by Gas-assisted Encounters of Planetary Embryos

  • Original language description

    We present radiation hydrodynamic simulations in which binary planets form by close encounters in a system of several super-Earth embryos. The embryos are embedded in a protoplanetary disk consisting of gas and pebbles and evolve in a region where the disk structure supports convergent migration due to Type I torques. As the embryos accrete pebbles, they become heated and thus affected by the thermal torque and the hot-trail effect, which excites orbital eccentricities. Motivated by findings of Eklund &amp; Masset, we assume that the hot-trail effect also operates vertically and reduces the efficiency of inclination damping. Non-zero inclinations allow the embryos to become closely packed and also vertically stirred within the convergence zone. Subsequently, close encounters of two embryos assisted by the disk gravity can form transient binary planets that quickly dissolve. Binary planets with a longer lifetime of similar to 10(4) yr form in three-body interactions of a transient pair with one of the remaining embryos. The separation of binary components generally decreases in subsequent encounters and because of pebble accretion until the binary merges, forming a giant planet core. We provide an order-of-magnitude estimate of the expected occurrence rate of binary planets, yielding one binary planet per similar or equal to(2-5) x 10(4) planetary systems. Therefore, although rare, binary planets may exist in exoplanetary systems and they should be systematically searched for.

  • 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/GA18-06083S" target="_blank" >GA18-06083S: Evolution of solid bodies in protoplanetary disks and during collisions</a><br>

  • Continuities

    P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)

Others

  • Publication year

    2018

  • Confidentiality

    S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Data specific for result type

  • Name of the periodical

    Astrophysical Journal

  • ISSN

    0004-637X

  • e-ISSN

  • Volume of the periodical

    868

  • Issue of the periodical within the volume

    2

  • Country of publishing house

    US - UNITED STATES

  • Number of pages

    14

  • Pages from-to

  • UT code for WoS article

    000452414800003

  • EID of the result in the Scopus database