Newborn Be star systems observed shortly after mass transfer

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F25%3A00617424" target="_blank" >RIV/67985815:_____/25:00617424 - isvavai.cz</a>

Výsledek na webu

<a href="https://hdl.handle.net/11104/0365938" target="_blank" >https://hdl.handle.net/11104/0365938</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/202347275" target="_blank" >10.1051/0004-6361/202347275</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Newborn Be star systems observed shortly after mass transfer

Popis výsledku v původním jazyce

Many classical Be stars acquire their very rapid rotation by mass- and angular-momentum transfer in massive binaries, marking the first phase of the evolutionary chain. Later-stage products, such as Be+subdwarf- and Be+neutron-star binaries (Be X-ray binaries), are also well known, although the search for definitive proof of Be+white dwarf companions is ongoing. Short-lived intermediate-phase objects, that is, binaries past the interaction stage but with a donor star that has not yet reached the end of its evolution or contraction, have only recently been discovered. Aims. The main hallmark of this kind of binary is a system of absorption lines with low width, significant radial-velocity variations, and peculiar relative line strengths. Data archives and the literature can be searched for additional candidates exhibiting this pattern, and follow-up observations can be obtained in order to increase the number of these systems with quantitatively known orbits, providing a basis for an initial statistical investigation and to develop observational strategies for abundance analyses. Methods. We identified 13 candidates at various confidence levels. To verify their nature, we derived orbital elements from new high-quality spectra and interferometric observations where possible. We also performed qualitative analyses of other basic parameters, and preliminarily evaluated indicators of advanced stages of nucleosynthesis. Results. Adding to the two known systems identified as classical Be star+pre-subdwarf binaries (LB-1 and HR 6819), we confirm two more (V742 Cas, HD 44637) with interferometry, with V742 Cas setting a new record for the smallest visually observed angular semi-major axis, at a = 0.663 mas. Two further systems (V447 Sct, V1362 Cyg) are not resolved interferometrically, but other evidence puts them at the same confidence level as LB-1. V2174 Cyg is a candidate with very high confidence, but was not observed interferometrically. The remaining systems are either candidates with varying levels of confidencemainly due to the lack of available spectroscopic or interferometric observations for comparison with the others and orbit determination- or could be rejected as candidates with the followup observations. Conclusions. Of a mostly magnitude-complete sample of 328 Be stars, 0.5-1% are found to have recently completed the mass overflow that led to their formation. Another 5% are systems with a compact subdwarf companionthat is, they are further evolved after a previous overflow- and a further 2% possibly harbor white dwarfs. All these systems are early B subtypes, but if the original sample is restricted to early subtypes (136 objects), these percentages increase by a factor of about 2.5, while dropping to zero for the mid and late subtypes (together 204 objects). This strongly suggests that early-type versus mid- and late-type Be stars follow differently weighted channels to acquire their rapid rotation, namely binary interaction versus evolutionary spin up.

Název v anglickém jazyce

Newborn Be star systems observed shortly after mass transfer

Popis výsledku anglicky

Many classical Be stars acquire their very rapid rotation by mass- and angular-momentum transfer in massive binaries, marking the first phase of the evolutionary chain. Later-stage products, such as Be+subdwarf- and Be+neutron-star binaries (Be X-ray binaries), are also well known, although the search for definitive proof of Be+white dwarf companions is ongoing. Short-lived intermediate-phase objects, that is, binaries past the interaction stage but with a donor star that has not yet reached the end of its evolution or contraction, have only recently been discovered. Aims. The main hallmark of this kind of binary is a system of absorption lines with low width, significant radial-velocity variations, and peculiar relative line strengths. Data archives and the literature can be searched for additional candidates exhibiting this pattern, and follow-up observations can be obtained in order to increase the number of these systems with quantitatively known orbits, providing a basis for an initial statistical investigation and to develop observational strategies for abundance analyses. Methods. We identified 13 candidates at various confidence levels. To verify their nature, we derived orbital elements from new high-quality spectra and interferometric observations where possible. We also performed qualitative analyses of other basic parameters, and preliminarily evaluated indicators of advanced stages of nucleosynthesis. Results. Adding to the two known systems identified as classical Be star+pre-subdwarf binaries (LB-1 and HR 6819), we confirm two more (V742 Cas, HD 44637) with interferometry, with V742 Cas setting a new record for the smallest visually observed angular semi-major axis, at a = 0.663 mas. Two further systems (V447 Sct, V1362 Cyg) are not resolved interferometrically, but other evidence puts them at the same confidence level as LB-1. V2174 Cyg is a candidate with very high confidence, but was not observed interferometrically. The remaining systems are either candidates with varying levels of confidencemainly due to the lack of available spectroscopic or interferometric observations for comparison with the others and orbit determination- or could be rejected as candidates with the followup observations. Conclusions. Of a mostly magnitude-complete sample of 328 Be stars, 0.5-1% are found to have recently completed the mass overflow that led to their formation. Another 5% are systems with a compact subdwarf companionthat is, they are further evolved after a previous overflow- and a further 2% possibly harbor white dwarfs. All these systems are early B subtypes, but if the original sample is restricted to early subtypes (136 objects), these percentages increase by a factor of about 2.5, while dropping to zero for the mid and late subtypes (together 204 objects). This strongly suggests that early-type versus mid- and late-type Be stars follow differently weighted channels to acquire their rapid rotation, namely binary interaction versus evolutionary spin up.

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

Astronomy & Astrophysics

ISSN

0004-6361

e-ISSN

1432-0746

Svazek periodika

694

Číslo periodika v rámci svazku

Feb.

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

15

Strana od-do

A172

Kód UT WoS článku

001418747000025

EID výsledku v databázi Scopus

2-s2.0-85217853116