Origin and Evolution of Short-period Comets

Kód výsledku v 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>

Výsledek na webu

<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>

Jazyk výsledku

angličtina

Název v původním jazyce

Origin and Evolution of Short-period Comets

Popis výsledku v původním jazyce

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.

Název v anglickém jazyce

Origin and Evolution of Short-period Comets

Popis výsledku anglicky

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.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

<a href="/cs/project/GA13-01308S" target="_blank" >GA13-01308S: Dynamika malých těles sluneční soustavy</a><br>

Návaznosti

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

Rok uplatnění

2017

Kód důvěrnosti údajů

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

Název periodika

Astrophysical Journal

ISSN

0004-637X

e-ISSN

—

Svazek periodika

845

Číslo periodika v rámci svazku

1

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

25

Strana od-do

—

Kód UT WoS článku

000407329800006

EID výsledku v databázi Scopus

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