How many explosions does one need? Quantifying supernovae in globular clusters from iron abundance spreads
The result's identifiers
Result code in IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F21%3A10438681" target="_blank" >RIV/00216208:11320/21:10438681 - isvavai.cz</a>
Result on the web
<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=0xGxR~xPdU" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=0xGxR~xPdU</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.1093/mnras/stab2011" target="_blank" >10.1093/mnras/stab2011</a>
Alternative languages
Result language
angličtina
Original language name
How many explosions does one need? Quantifying supernovae in globular clusters from iron abundance spreads
Original language description
Many globular clusters (GCs) are known to host multiple populations distinguishable by their light-element content. Less common are GCs displaying iron abundance spreads that are seen as evidence for enrichment through core collapse supernovae (SNe). We present a simple analytical method to estimate the number of SNe required to have occurred in a GC from its metallicity and iron abundance spread. We then use this result to estimate how long star formation (SF) lasted to build the GC. We apply our method to up-to-date measurements and find that, assuming the correctness of these measurements, multiple SNe (up to 10(5)) are required in most GCs with iron abundance spreads. The number of SNe events that contributed to the enrichment of the GCs studied here is typically a factor of 10 less than the expected number of SNe in a canonical initial mass function (IMF). This indicates that gas expulsion from the forming GC occurred after the first 10 per cent of SNe exploded. We compute that for the GCs typically SF ends after only a few Myr (extending up to approximate to 30 Myr in a few cases). We also discuss possible improvements of this method and especially its sensitivity to the error of iron abundance measurements of individual stars of a GC. The method presented here can quickly give an estimate for the number of SNe required to explain the iron abundance spread in a GC without the requirement of any hydrodynamical simulations.
Czech name
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Czech description
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Classification
Type
J<sub>imp</sub> - Article in a specialist periodical, which is included in the Web of Science database
CEP classification
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OECD FORD branch
10308 - Astronomy (including astrophysics,space science)
Result continuities
Project
<a href="/en/project/GA20-21855S" target="_blank" >GA20-21855S: The dynamics of dense star clusters with primordial binaries and massive black holes</a><br>
Continuities
P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)
Others
Publication year
2021
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Data specific for result type
Name of the periodical
Monthly Notices of the Royal Astronomical Society
ISSN
0035-8711
e-ISSN
—
Volume of the periodical
506
Issue of the periodical within the volume
3
Country of publishing house
GB - UNITED KINGDOM
Number of pages
8
Pages from-to
4131-4138
UT code for WoS article
000685245200073
EID of the result in the Scopus database
2-s2.0-85112167490