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Cited by 18Astrophysics and Star Formation StudiesStellar, planetary, and galactic studiesAstro and Planetary Science

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Number of stars in the Sun’s birth cluster revisited

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Arakawa, Sota, Kokubo, Eiichiro·2023·Astronomy & Astrophysics
DOI 10.1051/0004-6361/202244743
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Abstract

The Sun is thought to have been formed within a star cluster. The coexistence of 26 Al-rich and 26 Al-poor calcium–aluminum-rich inclusions indicates that a direct injection of 26 Al-rich materials from a nearby core-collapse supernova would be expected to occur in the first 10 5 years of the existence of the Solar System. Therefore, at least one core-collapse supernova ought to occur within the duration of star formation in the Sun’s birth cluster. Here, we revisit the number of stars in the Sun’s birth cluster from the point of view of the probability of experiencing at least one core-collapse supernova within the finite duration of star formation within the birth cluster. We find that the number of stars in the birth cluster may be significantly greater than that previously considered, depending on the duration of star formation.

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Fig. 1 Schematic of the direct injection of SLRs into the early Solar System within the birth cluster. Massive stars those were born in the cluster would trigger CCSNe when they finished their lifetime, t ? . To explain the coexistence of 26 Al-rich and 26 Al-poor CAIs in the early Solar System, a direct injection of SLR-rich dust grains from a CCSN should occur during CAI formation in the Solar System. A necessary condition for Solar System formation is that at least one CCSN occurs in the birth cluster within the duration of star formation, t SF .
Fig. 1 Schematic of the direct injection of SLRs into the early Solar System within the birth cluster. Massive stars those were born in the cluster would trigger CCSNe when they finished their lifetime, t ? . To explain the coexistence of 26 Al-rich and 26 Al-poor CAIs in the early Solar System, a direct injection of SLR-rich dust grains from a CCSN should occur during CAI formation in the Solar System. A necessary condition for Solar System formation is that at least one CCSN occurs in the birth cluster within the duration of star formation, t SF .CC-BY · From the PDF
Fig. 2 Relation between the maximum stellar mass in the birth cluster, m max, and the total number of stars, N cl .
Fig. 2 Relation between the maximum stellar mass in the birth cluster, m max, and the total number of stars, N cl .CC-BY · From the PDF
Fig. 3 Relation between the lifetime of stars (i.e., the time lag from the birth of a star to trigger CCSN), t ? , and the stellar mass, m ? . We also show the main-sequence lifetime (i.e., the duration of H-burning) as reference. Circle plots are data taken from Ekström et al. (2012) and the solid curve is the empirical fitting.
Fig. 3 Relation between the lifetime of stars (i.e., the time lag from the birth of a star to trigger CCSN), t ? , and the stellar mass, m ? . We also show the main-sequence lifetime (i.e., the duration of H-burning) as reference. Circle plots are data taken from Ekström et al. (2012) and the solid curve is the empirical fitting.CC-BY · From the PDF
Fig. 4 Probability of acquiring at least one core-collapse supernova with mass in the range of 20-60 M within the duration of star formation, P SN. Here, we assume that m max depends on N cl and it is given by Eq. (1).
Fig. 4 Probability of acquiring at least one core-collapse supernova with mass in the range of 20-60 M within the duration of star formation, P SN. Here, we assume that m max depends on N cl and it is given by Eq. (1).CC-BY · From the PDF
Fig. 5 Probability for acquiring at least one core-collapse supernova with mass in the range of 20-60 M within the duration of star formation, P SN. Here, we assume that m max = 100 M and does not depend on N cl .
Fig. 5 Probability for acquiring at least one core-collapse supernova with mass in the range of 20-60 M within the duration of star formation, P SN. Here, we assume that m max = 100 M and does not depend on N cl .CC-BY · From the PDF
Fig. 6 Contour chart of P SN in N clt SF plane. We note that P SN = 0 outside the shaded area.
Fig. 6 Contour chart of P SN in N clt SF plane. We note that P SN = 0 outside the shaded area.CC-BY · From the PDF

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Citations

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Metadata

Authors
Arakawa, S., & Kokubo, E.
Affiliations
  • Japan Agency for Marine-Earth Science and Technology (JP)
  • National Astronomical Observatory of Japan (JP)
ORCID
Venue
Astronomy & Astrophysics
Publisher
EDP Sciences
Published
2023-02
Volume
670
Pages
A105
ISSN
  • 0004-6361 (ISSN-L)
  • 1432-0746
DOI
10.1051/0004-6361/202244743
OpenAlex
W4315631752
Cited by
18
References
4
Citations by year
2026: 1 · 2025: 7 · 2024: 7 · 2023: 3
FWCI
2.10
Type
journal article
Language
en
Open access
Licence
Locations
  • Astronomy and Astrophysics (publishedVersion, cc-by)
  • arXiv (Cornell University) (submittedVersion)
  • Springer Link (Chiba Institute of Technology) (submittedVersion)
  • arXiv (Cornell University)
Funders
Japan Society for the Promotion of Science (JP20J00598, 18H05438)
Topics
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysics and Star Formation Studies
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
  • Physical Sciences › Earth and Planetary Sciences › Space and Planetary Science › Astro and Planetary Science
Keywords
core-collapse supernovae, calcium-aluminum-rich inclusions, 26Al, cluster size, solar system formation

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