The giants that were born swiftly - implications of the top-heavy stellar initial mass function on the birth conditions of globular clusters

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F22%3A10455578" target="_blank" >RIV/00216208:11320/22:10455578 - isvavai.cz</a>

Výsledek na webu

<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=9puAwPZDU9" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=9puAwPZDU9</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1093/mnras/stac2424" target="_blank" >10.1093/mnras/stac2424</a>

Jazyk výsledku

angličtina

Název v původním jazyce

The giants that were born swiftly - implications of the top-heavy stellar initial mass function on the birth conditions of globular clusters

Popis výsledku v původním jazyce

Recent results suggest that the initial mass function (IMF) of globular clusters (GCs) is metallicity and density dependent. Here, it is studied how this variation affects the initial masses and the numbers of core-collapse supernovae (CCSNe) required to reproduce the observed iron spreads in GCs. The IMFs of all of the investigated GCs were top-heavy implying larger initial masses compared to previous results computed assuming an invariant canonical IMF. This leads to more CCSNe being required to explain the observed iron abundance spreads. The results imply that the more massive GCs formed at smaller Galactocentric radii, possibly suggesting in situ formation of the population II halo. The time until star formation ended within a proto-GC is computed to be 3.5-4 Myr, being slightly shorter than the 4 Myr obtained using the canonical IMF. Therefore, the impact of the IMF on the time for which IMF lasts is small.

Název v anglickém jazyce

The giants that were born swiftly - implications of the top-heavy stellar initial mass function on the birth conditions of globular clusters

Popis výsledku anglicky

Recent results suggest that the initial mass function (IMF) of globular clusters (GCs) is metallicity and density dependent. Here, it is studied how this variation affects the initial masses and the numbers of core-collapse supernovae (CCSNe) required to reproduce the observed iron spreads in GCs. The IMFs of all of the investigated GCs were top-heavy implying larger initial masses compared to previous results computed assuming an invariant canonical IMF. This leads to more CCSNe being required to explain the observed iron abundance spreads. The results imply that the more massive GCs formed at smaller Galactocentric radii, possibly suggesting in situ formation of the population II halo. The time until star formation ended within a proto-GC is computed to be 3.5-4 Myr, being slightly shorter than the 4 Myr obtained using the canonical IMF. Therefore, the impact of the IMF on the time for which IMF lasts is small.

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/GA20-21855S" target="_blank" >GA20-21855S: Dynamika hustých hvězdokup s primordiálními dvojhvězdami a černými veledírami</a><br>

Návaznosti

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

Rok uplatnění

2022

Kód důvěrnosti údajů

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

Název periodika

Monthly Notices of the Royal Astronomical Society

ISSN

0035-8711

e-ISSN

1365-2966

Svazek periodika

516

Číslo periodika v rámci svazku

3

Stát vydavatele periodika

GB - Spojené království Velké Británie a Severního Irska

Počet stran výsledku

12

Strana od-do

3342-3353

Kód UT WoS článku

000854276200011

EID výsledku v databázi Scopus

2-s2.0-85143395949