Repositorio Institucional
Repositorio Institucional
CONICET Digital
  • Inicio
  • EXPLORAR
    • AUTORES
    • DISCIPLINAS
    • COMUNIDADES
  • Estadísticas
  • Novedades
    • Noticias
    • Boletines
  • Ayuda
    • General
    • Datos de investigación
  • Acerca de
    • CONICET Digital
    • Equipo
    • Red Federal
  • Contacto
JavaScript is disabled for your browser. Some features of this site may not work without it.
  • INFORMACIÓN GENERAL
  • RESUMEN
  • ESTADISTICAS
 
Artículo

Long-term photometric behavior and orbital period variations in the supersoft X-ray source V617 Sgr

Zang, Lei; Zhao, Ergang; Fernandez Lajus, Eduardo EusebioIcon ; Zubairi, Ahmed Waqas; Sarotsakulchai, Nopphadon
Fecha de publicación: 10/2023
Editorial: Elsevier Science
Revista: New Astronomy
ISSN: 1384-1076
Idioma: Inglés
Tipo de recurso: Artículo publicado
Clasificación temática:
Astronomía

Resumen

V617 Sgr is one of the Galactic counterparts of supersoft X-ray sources as a member of the V Sagittae class, where a massive white dwarf is accreting material from its stellar companion and forming an accretion disk. Since 2014, we have monitored it for about nine years with the 2.15 m telescope at CASLEO. It is found that the light curve shows obviously fluctuations and flickering, which imply the presence of active hot-spots on the accretion disk. Meanwhile, the flat-bottomed depressions can be explained by the presence of circumbinary material. By collecting all available eclipse times from the literature together with 149 newly determined times of light minimum, we constructed the O-C diagram and analyzed the variations in the orbital period of the eclipsing binary V617 Sgr. It is confirmed that the orbital period is increasing continuously with a rate of P ̇=+ 1. 68 (3)×10−7 d⋅ yr−1 ̇. A cyclic variation is detected to be superimposed on the period increase with an amplitude of 4.6 min and a period of 26 yr. The continuous period increase is largely due to mass transfer from the donor secondary on its Kelvin–Helmholtz time-scale, while wind mass loss from the accretion disk surrounding the white dwarf may also contribute on the period change. In this case, the mass-transfer rate of V617 Sgr is estimated to be in the range of about 0.575×10−6 to 2.25×10−6 M⊙ yr−1 and the mass-accretion rate is less than 1.59×10−6 M⊙ yr−1. The cyclic change can be explained by the presence of a third body or magnetic activity cycles of the secondary.
Palabras clave: binaries: close , binaries: eclipsing , stars: evolution , stars: individual (V617 Sgr)
Ver el registro completo
 
Archivos asociados
Tamaño: 827.4Kb
Formato: PDF
.
Solicitar
Licencia
info:eu-repo/semantics/restrictedAccess Excepto donde se diga explícitamente, este item se publica bajo la siguiente descripción: Creative Commons Attribution-NonCommercial-ShareAlike 2.5 Unported (CC BY-NC-SA 2.5)
Identificadores
URI: http://hdl.handle.net/11336/235530
URL: https://linkinghub.elsevier.com/retrieve/pii/S1384107623000556
DOI: http://dx.doi.org/10.1016/j.newast.2023.102054
Colecciones
Articulos(IALP)
Articulos de INST.DE ASTROFISICA LA PLATA
Citación
Zang, Lei; Zhao, Ergang; Fernandez Lajus, Eduardo Eusebio; Zubairi, Ahmed Waqas; Sarotsakulchai, Nopphadon; Long-term photometric behavior and orbital period variations in the supersoft X-ray source V617 Sgr; Elsevier Science; New Astronomy; 103; 10-2023; 1-6
Compartir
Altmétricas
 

Enviar por e-mail
Separar cada destinatario (hasta 5) con punto y coma.
  • Facebook
  • X Conicet Digital
  • Instagram
  • YouTube
  • Sound Cloud
  • LinkedIn

Los contenidos del CONICET están licenciados bajo Creative Commons Reconocimiento 2.5 Argentina License

https://www.conicet.gov.ar/ - CONICET

Inicio

Explorar

  • Autores
  • Disciplinas
  • Comunidades

Estadísticas

Novedades

  • Noticias
  • Boletines

Ayuda

Acerca de

  • CONICET Digital
  • Equipo
  • Red Federal

Contacto

Godoy Cruz 2290 (C1425FQB) CABA – República Argentina – Tel: +5411 4899-5400 repositorio@conicet.gov.ar
TÉRMINOS Y CONDICIONES