VLTI/GRAVITY enables the determination of the first dynamical masses of a classical Be+ stripped and bloated pre-subdwarf binary

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F25%3A00617918" target="_blank" >RIV/67985815:_____/25:00617918 - isvavai.cz</a>

Výsledek na webu

<a href="https://hdl.handle.net/11104/0365968" target="_blank" >https://hdl.handle.net/11104/0365968</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/202453248" target="_blank" >10.1051/0004-6361/202453248</a>

Jazyk výsledku

angličtina

Název v původním jazyce

VLTI/GRAVITY enables the determination of the first dynamical masses of a classical Be+ stripped and bloated pre-subdwarf binary

Popis výsledku v původním jazyce

HR 6819 is the first post-mass transfer binary system composed of a classical Be star and a bloated pre-subdwarf stripped star directly confirmed by interferometry. While the Be star is already spun up to near-critical rotation and possesses a self-ejected viscous Keplerian disk, the stripped star is found in a short-lived evolutionary stage, in which it retains the spectral appearance of a B-type main-sequence star while contracting into a faint subdwarf OB-type star. Aims. In order to understand the evolution of intermediate-mass interacting binaries, the fundamental parameters of cornerstone objects such as HR 6819 need to be known. We aim to obtain orbital parameters and model-independent dynamical masses of this binary system to quantitatively characterize this rarely observed evolutionary stage. Methods. We analyzed a time series of 12 interferometric near-IR K-band observations from VLTI/GRAVITY with the help of the geometrical model-fitting tool PMOIRED. We included recently published radial velocities based on FEROS high-resolution spectroscopy for the binary orbital solution. Results. With the GRAVITY data, we obtained the astrometric orbit, relative fluxes of the components, and parameters of the circumstellar disk of the Be star, we also detected helium line signatures from the stripped star. Using the published radial velocities enabled us to obtain the dynamical masses of the components as well as the dynamical parallax. The Be star is the slightly brighter component in the K band and is almost 16 times as massive as the bloated stripped star, with the individual dynamical masses being 4.24 +/- 0.31 M circle dot for the Be star and 0.270 +/- 0.056 M circle dot for the stripped star. The orbit is slightly eccentric, with e = 0.0289 +/- 0.0058, and the semimajor axis of the orbit is 0.3800 +/- 0.0093 AU. The distance derived from the orbital solution is 296.0 +/- 8.0 pc, significantly lower than the distance from Gaia DR3, which is overestimated by similar to 24% due to the orbital motion. Conclusions. The newly obtained fundamental parameters provide an important anchor for evolutionary models of interacting binaries and for the physics of mass transfer. The low mass of the bloated star means that it may become completely undetectable once it settles into a faint subdwarf, which implies that many more Be stars may have low-mass companions despite appearing single.

Název v anglickém jazyce

VLTI/GRAVITY enables the determination of the first dynamical masses of a classical Be+ stripped and bloated pre-subdwarf binary

Popis výsledku anglicky

HR 6819 is the first post-mass transfer binary system composed of a classical Be star and a bloated pre-subdwarf stripped star directly confirmed by interferometry. While the Be star is already spun up to near-critical rotation and possesses a self-ejected viscous Keplerian disk, the stripped star is found in a short-lived evolutionary stage, in which it retains the spectral appearance of a B-type main-sequence star while contracting into a faint subdwarf OB-type star. Aims. In order to understand the evolution of intermediate-mass interacting binaries, the fundamental parameters of cornerstone objects such as HR 6819 need to be known. We aim to obtain orbital parameters and model-independent dynamical masses of this binary system to quantitatively characterize this rarely observed evolutionary stage. Methods. We analyzed a time series of 12 interferometric near-IR K-band observations from VLTI/GRAVITY with the help of the geometrical model-fitting tool PMOIRED. We included recently published radial velocities based on FEROS high-resolution spectroscopy for the binary orbital solution. Results. With the GRAVITY data, we obtained the astrometric orbit, relative fluxes of the components, and parameters of the circumstellar disk of the Be star, we also detected helium line signatures from the stripped star. Using the published radial velocities enabled us to obtain the dynamical masses of the components as well as the dynamical parallax. The Be star is the slightly brighter component in the K band and is almost 16 times as massive as the bloated stripped star, with the individual dynamical masses being 4.24 +/- 0.31 M circle dot for the Be star and 0.270 +/- 0.056 M circle dot for the stripped star. The orbit is slightly eccentric, with e = 0.0289 +/- 0.0058, and the semimajor axis of the orbit is 0.3800 +/- 0.0093 AU. The distance derived from the orbital solution is 296.0 +/- 8.0 pc, significantly lower than the distance from Gaia DR3, which is overestimated by similar to 24% due to the orbital motion. Conclusions. The newly obtained fundamental parameters provide an important anchor for evolutionary models of interacting binaries and for the physics of mass transfer. The low mass of the bloated star means that it may become completely undetectable once it settles into a faint subdwarf, which implies that many more Be stars may have low-mass companions despite appearing single.

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

13

Strana od-do

A208

Kód UT WoS článku

001421982100003

EID výsledku v databázi Scopus

2-s2.0-85217971543