Shell helium-burning hot subdwarf B stars as candidates for blue large-amplitude pulsators

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F22%3A00604502" target="_blank" >RIV/67985815:_____/22:00604502 - isvavai.cz</a>

Výsledek na webu

<a href="https://hdl.handle.net/11104/0361929" target="_blank" >https://hdl.handle.net/11104/0361929</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/202244571" target="_blank" >10.1051/0004-6361/202244571</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Shell helium-burning hot subdwarf B stars as candidates for blue large-amplitude pulsators

Popis výsledku v původním jazyce

Blue large-amplitude pulsators (BLAPs) are a newly discovered type of variable star. Their typical pulsation periods are on the order of a few tens of minutes, with relatively large amplitudes of 0.2-0.4 mag in optical bands, and their rates of period changes are on the order of 10(-7) yr(-1) (both positive and negative). They are extremely rare objects and attempts to explain their origins and internal structures have attracted a great deal of attention. Previous studies have proposed that BLAPs may be pre-white dwarfs, with masses around 0.3 M circle dot, or core-helium-burning stars in the range of similar to 0.7-1.1 M circle dot. In this work, we use a number of MESA models to compute and explore whether BLAPs could be explained as shell helium-burning subdwarfs type B (SHeB sdBs). The models that best match existing observational constraints have helium core masses in the range of similar to 0.45-0.5 M circle dot. Our model predicts that the positive rate of period change may evolve to negative. The formation channels for SHeB sdBs involve binary evolution and although the vast majority of BLAPs do not appear to be binaries (with the exception of HD 133729), the observational constraints are still very poor. Motivated by these findings, we explored the Roche lobe overflow channel. Of the 304 binary evolution models we computed, about half of them are able to produce SHeB sdBs in long-period binaries that evade detection from the limited observations that are currently available.

Název v anglickém jazyce

Shell helium-burning hot subdwarf B stars as candidates for blue large-amplitude pulsators

Popis výsledku anglicky

Blue large-amplitude pulsators (BLAPs) are a newly discovered type of variable star. Their typical pulsation periods are on the order of a few tens of minutes, with relatively large amplitudes of 0.2-0.4 mag in optical bands, and their rates of period changes are on the order of 10(-7) yr(-1) (both positive and negative). They are extremely rare objects and attempts to explain their origins and internal structures have attracted a great deal of attention. Previous studies have proposed that BLAPs may be pre-white dwarfs, with masses around 0.3 M circle dot, or core-helium-burning stars in the range of similar to 0.7-1.1 M circle dot. In this work, we use a number of MESA models to compute and explore whether BLAPs could be explained as shell helium-burning subdwarfs type B (SHeB sdBs). The models that best match existing observational constraints have helium core masses in the range of similar to 0.45-0.5 M circle dot. Our model predicts that the positive rate of period change may evolve to negative. The formation channels for SHeB sdBs involve binary evolution and although the vast majority of BLAPs do not appear to be binaries (with the exception of HD 133729), the observational constraints are still very poor. Motivated by these findings, we explored the Roche lobe overflow channel. Of the 304 binary evolution models we computed, about half of them are able to produce SHeB sdBs in long-period binaries that evade detection from the limited observations that are currently available.

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

2022

Kód důvěrnosti údajů

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

Název periodika

Astronomy & Astrophysics

ISSN

0004-6361

e-ISSN

1432-0746

Svazek periodika

668

Číslo periodika v rámci svazku

Dec.

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

22

Strana od-do

A112

Kód UT WoS článku

000931907600008

EID výsledku v databázi Scopus

2-s2.0-85145442140