Dynamics of dust particles released from Oort cloud comets and their contribution to radar meteors

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F11%3A10104318" target="_blank" >RIV/00216208:11320/11:10104318 - isvavai.cz</a>

Výsledek na webu

<a href="http://dx.doi.org/10.1088/0004-637X/743/1/37" target="_blank" >http://dx.doi.org/10.1088/0004-637X/743/1/37</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1088/0004-637X/743/1/37" target="_blank" >10.1088/0004-637X/743/1/37</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Dynamics of dust particles released from Oort cloud comets and their contribution to radar meteors

Popis výsledku v původním jazyce

The Oort Cloud Comets (OCCs), exemplified by the Great Comet of 1997 (Hale-Bopp), are occasional visitors from the heatless periphery of the solar system. Previous works hypothesized that a great majority of OCCs?t physically disrupt after one or two passages through the inner solar system, where strong thermal gradients can cause phase transitions or volatile pressure buildup. Here we study the fate of small debris particles produced by OCC disruptions to determine whether the imprints of a hypothetical population of OCC meteoroids can be found in the existing meteor radar data. We find that OCC particles with diameters D {~ 10 ?m are blown out from the solar system by radiation pressure, while those with D }~ 1 mm have a very low Earth-impact probability. The intermediate particle sizes, D ~ 100 ?m, represent a sweet spot. About 1% of these particles orbitally evolve by Poynting-Robertson drag to reach orbits with semimajor axis a ~ 1 AU. They are expected to produce meteors with rad

Název v anglickém jazyce

Dynamics of dust particles released from Oort cloud comets and their contribution to radar meteors

Popis výsledku anglicky

The Oort Cloud Comets (OCCs), exemplified by the Great Comet of 1997 (Hale-Bopp), are occasional visitors from the heatless periphery of the solar system. Previous works hypothesized that a great majority of OCCs?t physically disrupt after one or two passages through the inner solar system, where strong thermal gradients can cause phase transitions or volatile pressure buildup. Here we study the fate of small debris particles produced by OCC disruptions to determine whether the imprints of a hypothetical population of OCC meteoroids can be found in the existing meteor radar data. We find that OCC particles with diameters D {~ 10 ?m are blown out from the solar system by radiation pressure, while those with D }~ 1 mm have a very low Earth-impact probability. The intermediate particle sizes, D ~ 100 ?m, represent a sweet spot. About 1% of these particles orbitally evolve by Poynting-Robertson drag to reach orbits with semimajor axis a ~ 1 AU. They are expected to produce meteors with rad

Druh

J_x - Nezařazeno - Článek v odborném periodiku (Jimp, Jsc a Jost)

CEP obor

BN - Astronomie a nebeská mechanika, astrofyzika

OECD FORD obor

—

Projekt

<a href="/cs/project/GA205%2F08%2F0064" target="_blank" >GA205/08/0064: Jarkovského a YORP jevy v translační a rotační dynamice asteroidů</a><br>

Návaznosti

P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)<br>Z - Vyzkumny zamer (s odkazem do CEZ)

Rok uplatnění

2011

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

743

Číslo periodika v rámci svazku

1

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

12

Strana od-do

37, 1-12

Kód UT WoS článku

000297408300037

EID výsledku v databázi Scopus

—