THE PROPERTIES OF DYNAMICALLY EJECTED RUNAWAY AND HYPER-RUNAWAY STARS

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F12%3A10129557" target="_blank" >RIV/00216208:11320/12:10129557 - isvavai.cz</a>

Výsledek na webu

<a href="http://dx.doi.org/10.1088/0004-637X/751/2/133" target="_blank" >http://dx.doi.org/10.1088/0004-637X/751/2/133</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1088/0004-637X/751/2/133" target="_blank" >10.1088/0004-637X/751/2/133</a>

Jazyk výsledku

angličtina

Název v původním jazyce

THE PROPERTIES OF DYNAMICALLY EJECTED RUNAWAY AND HYPER-RUNAWAY STARS

Popis výsledku v původním jazyce

Runaway stars are stars observed to have large peculiar velocities. Two mechanisms are thought to contribute to the ejection of runaway stars, both of which involve binarity (or higher multiplicity). In the binary supernova scenario, a runaway star receives its velocity when its binary massive companion explodes as a supernova (SN). In the alternative dynamical ejection scenario, runaway stars are formed through gravitational interactions between stars and binaries in dense, compact clusters or clustercores. Here we study the ejection scenario. We make use of extensive N-body simulations of massive clusters, as well as analytic arguments, in order to characterize the expected ejection velocity distribution of runaway stars. We find that the ejection velocity distribution of the fastest runaways (upsilon greater than or similar to 80 km s(-1)) depends on the binary distribution in the cluster, consistent with our analytic toy model, whereas the distribution of lower velocity runaways a

Název v anglickém jazyce

THE PROPERTIES OF DYNAMICALLY EJECTED RUNAWAY AND HYPER-RUNAWAY STARS

Popis výsledku anglicky

Runaway stars are stars observed to have large peculiar velocities. Two mechanisms are thought to contribute to the ejection of runaway stars, both of which involve binarity (or higher multiplicity). In the binary supernova scenario, a runaway star receives its velocity when its binary massive companion explodes as a supernova (SN). In the alternative dynamical ejection scenario, runaway stars are formed through gravitational interactions between stars and binaries in dense, compact clusters or clustercores. Here we study the ejection scenario. We make use of extensive N-body simulations of massive clusters, as well as analytic arguments, in order to characterize the expected ejection velocity distribution of runaway stars. We find that the ejection velocity distribution of the fastest runaways (upsilon greater than or similar to 80 km s(-1)) depends on the binary distribution in the cluster, consistent with our analytic toy model, whereas the distribution of lower velocity runaways a

Druh

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

CEP obor

BN - Astronomie a nebeská mechanika, astrofyzika

OECD FORD obor

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Projekt

<a href="/cs/project/GA202%2F09%2F0772" target="_blank" >GA202/09/0772: Aktuální problémy gravitace, obecné relativity a relativistické astrofyziky</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

2012

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

751

Číslo periodika v rámci svazku

2

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

6

Strana od-do

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Kód UT WoS článku

000304204600054

EID výsledku v databázi Scopus

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