Mass Distribution for Single-lined Hot Subdwarf Stars in LAMOST

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F23%3A00574936" target="_blank" >RIV/67985815:_____/23:00574936 - isvavai.cz</a>

Výsledek na webu

<a href="https://hdl.handle.net/11104/0345567" target="_blank" >https://hdl.handle.net/11104/0345567</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.3847/1538-4357/ace25e" target="_blank" >10.3847/1538-4357/ace25e</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Mass Distribution for Single-lined Hot Subdwarf Stars in LAMOST

Popis výsledku v původním jazyce

Masses for 664 single-lined hot subdwarf stars identified in LAMOST were calculated by comparing synthetic fluxes from spectral energy distribution with observed fluxes from a Virtual Observatory service. Three groups of hot subdwarf stars were selected from the whole sample according to their parallax precision to study the mass distributions. We found.that He-poor sdB/sdOB stars present a wide mass distribution from 0.1 to 1.0 M-circle dot with a sharp mass peak at around 0.46 M-circle dot, which is consistent with canonical binary model prediction. He-rich sdB/sdOB/sdO stars present a much flatter mass distribution than He-poor sdB/sdOB stars and with a mass peak at around 0.42 M-circle dot. By comparing the observed mass distributions to the predictions of different formation scenarios, we concluded that the binary merger channel, including two helium white dwarfs (He-WDs) and He-WD + mainsequence mergers, cannot be the only main formation channel for He-rich hot subdwarfs, and other formation channels, such as the surviving companions from Type Ia supernovae, could also make impacts on producing this special population, especially for He-rich hot subdwarfs with masses less than 0.44 M-circle dot. He-poor sdO stars also present a flatter mass distribution with an inconspicuous peak mass at 0.18 M-circle dot. The similar mass-Delta RVmax distribution between He-poor sdB/sdOB and sdO stars supports the scenario that He-poor sdO stars could be the subsequent evolution stage of He-poor sdB/sdOB stars.

Název v anglickém jazyce

Mass Distribution for Single-lined Hot Subdwarf Stars in LAMOST

Popis výsledku anglicky

Masses for 664 single-lined hot subdwarf stars identified in LAMOST were calculated by comparing synthetic fluxes from spectral energy distribution with observed fluxes from a Virtual Observatory service. Three groups of hot subdwarf stars were selected from the whole sample according to their parallax precision to study the mass distributions. We found.that He-poor sdB/sdOB stars present a wide mass distribution from 0.1 to 1.0 M-circle dot with a sharp mass peak at around 0.46 M-circle dot, which is consistent with canonical binary model prediction. He-rich sdB/sdOB/sdO stars present a much flatter mass distribution than He-poor sdB/sdOB stars and with a mass peak at around 0.42 M-circle dot. By comparing the observed mass distributions to the predictions of different formation scenarios, we concluded that the binary merger channel, including two helium white dwarfs (He-WDs) and He-WD + mainsequence mergers, cannot be the only main formation channel for He-rich hot subdwarfs, and other formation channels, such as the surviving companions from Type Ia supernovae, could also make impacts on producing this special population, especially for He-rich hot subdwarfs with masses less than 0.44 M-circle dot. He-poor sdO stars also present a flatter mass distribution with an inconspicuous peak mass at 0.18 M-circle dot. The similar mass-Delta RVmax distribution between He-poor sdB/sdOB and sdO stars supports the scenario that He-poor sdO stars could be the subsequent evolution stage of He-poor sdB/sdOB stars.

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/GA22-34467S" target="_blank" >GA22-34467S: Interakce dvojhvězd na větvi červených obrů: horcí podtrpaslíci jako testovací případ.</a><br>

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2023

Kód důvěrnosti údajů

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

Název periodika

Astrophysical Journal

ISSN

0004-637X

e-ISSN

1538-4357

Svazek periodika

953

Číslo periodika v rámci svazku

2

Stát vydavatele periodika

GB - Spojené království Velké Británie a Severního Irska

Počet stran výsledku

16

Strana od-do

122

Kód UT WoS článku

001046038300001

EID výsledku v databázi Scopus

2-s2.0-85167894997