On the Orbital Period and Models of V Sge

• Autorzy: Smak J.

Identyfikatory

DOI

10.32023/0001-5237/72.1.2

• Języki publikacji: EN

Abstrakty

EN

The orbital period of V Sge is decreasing at a rate which increased from dP/dt=-(4.11±0.33)×10^-10 in 1962 to -(5.44±0.61)× 10^-10 in 2022. This implies that the mass transfer from the secondary component is accelerating. From the evidence based on the orbital period variations, combined with estimates of the mass loss from the system based on radio observations, it follows that (1) the mass transfer rate from the secondary component is larger than M₂=-5×10^-6 M_☉/yr, possibly as large as M₂=-2.5×10^-5 M_☉/yr, and (2) the mass loss rate from the primary component is M₁=-4×10^-7 M_☉/yr or larger. Close similarity of V Sge to binary Wolf-Rayet stars supports the model with primary component being a hot, evolved star loosing its mass. Several arguments are presented which exclude the alternative model with primary component being a white dwarf with an accretion disk.

Słowa kluczowe

EN

binaries: close; Stars: winds; outflows; X-rays: stars; Stars: mass-loss; Stars: individual: V Sge

• Wydawca: Copernicus Foundation for Polish Astronomy
• Czasopismo: Acta Astronomica
• Rocznik: 2022
• Tom: Vol. 72, No. 1
• Strony: 21--29
• Opis fizyczny: Bibliogr. 23 poz., tab., wykr.

Twórcy

autor

Smak J.

• N. Copernicus Astronomical Center, Polish Academy of Sciences, Bartycka 18, 00-716 Warsaw, Poland

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Uwagi

Opracowanie rekordu ze środków MEiN, umowa nr SONP/SP/546092/2022 w ramach programu "Społeczna odpowiedzialność nauki" - moduł: Popularyzacja nauki i promocja sportu (2022-2023)