The overcontact binary V563 Lyrae

• Robert H. Nelson ^{[1] [2] [3]}
  1. [1] Mountain Ash Observatory, Prince George, BC, Canada
  2. [2] Desert Blooms Observatory, Benson, AZ
  3. [3] Guest User, Canadian Astronomy Data Centre, which is operated by the Dominion Astrophysical Observatory for the National Research Council of Canada’s Herzberg Institute of Astrophysics

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• Localización: Revista mexicana de astronomía y astrofísica, ISSN-e 0185-1101, Vol. 58, Nº. 2, 2022, págs. 223-235
• Idioma: inglés
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  • español

    Presentamos curvas de velocidad radial (RV) y de luz (LC) para la binaria en sobrecontacto V563 Lyr, y se analizan con la versión 2003 del código Wilson- Devinney (WD). Los resultado son: K1 = 147.4 ± 2.1 km/s, K2 = 247.2 ± 1.1 km/s, RVγ = 22.5 ± 1.5 km/s, qsp = 0.596 ± 0.008, M1 = 2.49(4)M⊙, M2 = 1.45(4)M⊙, R1 = 2.23(2)R⊙, R2 = 1.81(2)R⊙. Se identifica una tercera componente con velocidad radial RV3 = 18.8 ± 6.7 km/s. Al insertar los parámetros del par eclipsante en un diagrama Log (L)-Log (Teff) para cada estrella usando los datos de Yakut y Eggleton (2005) se infiere que ambas estrellas son sobre-luminosas y han evolucionado hasta el punto terminal de la secuencia principal (TAMS), o más allá. La tercera estrella tiene un tipo espectral estimado de A0 ± 1, pero no puede estar ligada gravitatoriamente al par eclipsante, pues su flujo dominaría al del par, lo cual no se observa. La tercera estrella tiene que estar a mayor distancia.

  • English

    Radial velocity (RV) and light curve (LC) data for the overcontact binary V563 Lyr have been obtained and analysed with the 2003 version of the Wilson-Devinney (WD) code with results K1 = 147.4 ± 2.1 km/s, K2 = 247.2 ± 1.1 km/s, RVγ = 22.5 ± 1.5 km/s, qsp = 0.596 ± 0.008, M1 = 2.49(4)M⊙, M2 = 1.45(4)M⊙, R1 = 2.23(2)R⊙, R2 = 1.81(2)R⊙. A third component was identified, with radial velocity RV3 = 18.8 ± 6.7 km/s. Inserting the derived parameters of the eclipsing pair into a Log (L)-Log (Teff) plot for each star using data from Yakut and Eggleton (2005) suggested that both stars are over-luminous and evolved to, and perhaps past, the terminal age main sequence (TAMS). The companion (star 3) has a spectral type of A0 ± 1 spectral subclass but cannot be gravitationally bound to the eclipsing pair, as its flux would dominate that of the pair, which was not observed. The companion must lie at some other distance.