Hot Subdwarf Stars Identified in Gaia DR2 with Spectra of LAMOST DR6 and DR7. II. Kinematics

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F20%3A00534444" target="_blank" >RIV/67985815:_____/20:00534444 - isvavai.cz</a>

Výsledek na webu

<a href="https://doi.org/10.3847/1538-4357/ab98f3" target="_blank" >https://doi.org/10.3847/1538-4357/ab98f3</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.3847/1538-4357/ab98f3" target="_blank" >10.3847/1538-4357/ab98f3</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Hot Subdwarf Stars Identified in Gaia DR2 with Spectra of LAMOST DR6 and DR7. II. Kinematics

Popis výsledku v původním jazyce

We present a kinematic population classification of the four hot subdwarf helium groups based on their positions in the U - V velocity diagram, the J(Z)- eccentricity diagram, and their Galactic orbits. The overall tendency of the fractional distributions of the four hot subdwarf helium groups in the halo, thin disk, and thick disk is largely consistent with the findings reported by Luo et al. based on LAMOST DR5, which appears to support predictions of binary population synthesis. He-deficient stars with -2.2 <= log(y) < -1 likely originate from a stable Roche lobe overflow channel, He-deficient stars with log(y) < -2.2 from the common envelope ejection channel, and He-rich stars with log(y) >= 0 from the merger channel of double He white dwarf stars. The fraction of He-rich hot subdwarf stars with -1 <= log (y) < 0 in the thin disk and the halo is far higher than that in the thick disk, which implies that these stars have different formation channels in the thin disk and in the halo.

Název v anglickém jazyce

Hot Subdwarf Stars Identified in Gaia DR2 with Spectra of LAMOST DR6 and DR7. II. Kinematics

Popis výsledku anglicky

We present a kinematic population classification of the four hot subdwarf helium groups based on their positions in the U - V velocity diagram, the J(Z)- eccentricity diagram, and their Galactic orbits. The overall tendency of the fractional distributions of the four hot subdwarf helium groups in the halo, thin disk, and thick disk is largely consistent with the findings reported by Luo et al. based on LAMOST DR5, which appears to support predictions of binary population synthesis. He-deficient stars with -2.2 <= log(y) < -1 likely originate from a stable Roche lobe overflow channel, He-deficient stars with log(y) < -2.2 from the common envelope ejection channel, and He-rich stars with log(y) >= 0 from the merger channel of double He white dwarf stars. The fraction of He-rich hot subdwarf stars with -1 <= log (y) < 0 in the thin disk and the halo is far higher than that in the thick disk, which implies that these stars have different formation channels in the thin disk and in the halo.

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/GA18-20083S" target="_blank" >GA18-20083S: Gaia-GALEX přehled horkých podtrpaslíků</a><br>

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2020

Kód důvěrnosti údajů

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

Název periodika

Astrophysical Journal

ISSN

1538-4357

e-ISSN

—

Svazek periodika

898

Číslo periodika v rámci svazku

1

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

10

Strana od-do

64

Kód UT WoS článku

000555732800001

EID výsledku v databázi Scopus

2-s2.0-85088981737