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Origin and Evolution of Short-period Comets

The result's identifiers

  • Result code in IS VaVaI

    <a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F17%3A10371939" target="_blank" >RIV/00216208:11320/17:10371939 - isvavai.cz</a>

  • Result on the web

    <a href="http://dx.doi.org/10.3847/1538-4357/aa7cf6" target="_blank" >http://dx.doi.org/10.3847/1538-4357/aa7cf6</a>

  • DOI - Digital Object Identifier

    <a href="http://dx.doi.org/10.3847/1538-4357/aa7cf6" target="_blank" >10.3847/1538-4357/aa7cf6</a>

Alternative languages

  • Result language

    angličtina

  • Original language name

    Origin and Evolution of Short-period Comets

  • Original language description

    Comets are icy objects that orbitally evolve from the trans-Neptunian region into the inner solar system, where they are heated by solar radiation and become active due to the sublimation of water ice. Here we perform simulations in which cometary reservoirs are formed in the early solar system and evolved over 4.5 Gyr. The gravitational effects of Planet. 9 (P9) are included in some simulations. Different models are considered for comets to be active, including a simple assumption that comets remain active for N-p(q) perihelion passages with perihelion distance q &lt; 2.5 au. The orbital distribution and number of active comets produced in our model is compared to observations. The orbital distribution of ecliptic comets (ECs) is well reproduced in models with N-p(2.5) similar or equal to 500 and without P9. With P9, the inclination distribution of model ECs is wider than the observed one. We find that the known Halley-type comets (HTCs) have a nearly isotropic inclination distribution. The HTCs appear to be an extension of the population of returning Oort-cloud comets (OCCs) to shorter orbital periods. The inclination distribution of model HTCs becomes broader with increasing N-p, but the existing data are not good enough to constrain Np from orbital fits. N-p(2.5)&gt; 1000 is required to obtain a steady-state population of large active HTCs that is consistent with observations. To fit the ratio of the returning-to-new OCCs, by contrast, our model implies that N-p(2.5) less than or similar to 10, possibly because the detected long-period comets are smaller and much easier to disrupt than observed HTCs.

  • 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/GA13-01308S" target="_blank" >GA13-01308S: Dynamics of small bodies in the solar system</a><br>

  • Continuities

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

Others

  • Publication year

    2017

  • 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

    845

  • Issue of the periodical within the volume

    1

  • Country of publishing house

    US - UNITED STATES

  • Number of pages

    25

  • Pages from-to

  • UT code for WoS article

    000407329800006

  • EID of the result in the Scopus database