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Very massive stars in not so massive clusters

The result's identifiers

  • Result code in IS VaVaI

    <a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F18%3A10388466" target="_blank" >RIV/00216208:11320/18:10388466 - isvavai.cz</a>

  • Result on the web

    <a href="https://doi.org/10.1093/mnras/sty2245" target="_blank" >https://doi.org/10.1093/mnras/sty2245</a>

  • DOI - Digital Object Identifier

    <a href="http://dx.doi.org/10.1093/mnras/sty2245" target="_blank" >10.1093/mnras/sty2245</a>

Alternative languages

  • Result language

    angličtina

  • Original language name

    Very massive stars in not so massive clusters

  • Original language description

    Very young star clusters in the Milky Way exhibit a well-defined relation between their maximum stellar mass, m(max), and their mass in stars, M-ecl. A recent study shows that the young intermediate-mass star cluster VVV CL041 possibly hosts a greater than or similar to 80M(circle dot) star, WR62-2, which appears to violate the existence of the m(max)-M-ecl relation since the mass of the star is almost two times higher than that expected from the relation. By performing direct N-body calculations with the same mass as the cluster VVV CL041 (approximate to 3000M(circle dot)), we study whether such a very massive star can be formed via dynamically induced stellar collisions in a binaryrich star cluster that initially follows the m(max)-M-ecl relation. Eight out of 100 clusters form a star more massive than 80M(circle dot) through multiple stellar collisions. This suggests that the VVV CL041 cluster may have become an outlier of the relation because of its early-dynamical evolution, even if the cluster followed the relation at birth. We find that more than half of our model clusters host a merger product as its most massive member within the first 5 Myr of cluster evolution. Thus, the existence of stars more massive than the m(max)-M-ecl relation in some young clusters is expected due to dynamical processes despite the validity of the m(max)-M-ecl relation. We briefly discuss evolution of binary populations in our model.

  • Czech name

  • Czech description

Classification

  • Type

    J<sub>imp</sub> - Article in a specialist periodical, which is included in the Web of Science database

  • CEP classification

  • OECD FORD branch

    10308 - Astronomy (including astrophysics,space science)

Result continuities

  • Project

  • Continuities

    I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Others

  • Publication year

    2018

  • 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

    481

  • Issue of the periodical within the volume

    1

  • Country of publishing house

    GB - UNITED KINGDOM

  • Number of pages

    11

  • Pages from-to

    153-163

  • UT code for WoS article

    000449651400011

  • EID of the result in the Scopus database

    2-s2.0-85054078164