Are binary-star populations regionally different?

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F25%3A10509597" target="_blank" >RIV/00216208:11320/25:10509597 - isvavai.cz</a>

Výsledek na webu

<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=Igk6eiR-2i" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=Igk6eiR-2i</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.31577/caosp.2025.55.3.217" target="_blank" >10.31577/caosp.2025.55.3.217</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Are binary-star populations regionally different?

Popis výsledku v původním jazyce

For synthesising star clusters and whole galaxies, stellar populations need to be modelled by a set of four functions that define their initial distribution of stellar masses and of the orbital properties of their binary-star populations. The initial binaries are dynamically processed in different embedded clusters explaining differences in the observed populations. The approach summarised here, for which the Aarseth Nbody codes have been instrumental, allows inference of the initial conditions of the globular cluster omega Cen and the quantification of the stellar merger rate as a function of stellar spectral type, of the role of multiples and mergers for the Cepheid population, and predictions of extragalactic observables. The observability of the four initial distribution functions and their physical and philosophical meaning are also briefly raised. Evidence for the variation of these functions on the physical conditions of star formation and future steps towards extensions to include higher-order multiple systems are touched upon.

Název v anglickém jazyce

Are binary-star populations regionally different?

Popis výsledku anglicky

For synthesising star clusters and whole galaxies, stellar populations need to be modelled by a set of four functions that define their initial distribution of stellar masses and of the orbital properties of their binary-star populations. The initial binaries are dynamically processed in different embedded clusters explaining differences in the observed populations. The approach summarised here, for which the Aarseth Nbody codes have been instrumental, allows inference of the initial conditions of the globular cluster omega Cen and the quantification of the stellar merger rate as a function of stellar spectral type, of the role of multiples and mergers for the Cepheid population, and predictions of extragalactic observables. The observability of the four initial distribution functions and their physical and philosophical meaning are also briefly raised. Evidence for the variation of these functions on the physical conditions of star formation and future steps towards extensions to include higher-order multiple systems are touched upon.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

—

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2025

Kód důvěrnosti údajů

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

Název periodika

Contributions of the Astronomical Observatory Skalnaté Pleso

ISSN

1335-1842

e-ISSN

1336-0337

Svazek periodika

55

Číslo periodika v rámci svazku

3

Stát vydavatele periodika

SK - Slovenská republika

Počet stran výsledku

17

Strana od-do

217-233

Kód UT WoS článku

001509136400018

EID výsledku v databázi Scopus

2-s2.0-105005852395