Period Variation Study and Light Curve Analysis of the Eclipsing Binary GSC 02013- 00288

• N.S. Awadalla ^[1] ; M.A. Hanna ^[1] ; M.N. Ismail ^[2] ; I.A. Hassan ^[2] ; M.A. Elkhamisy ^[1]
  1. [1] National Research Institute of Astronomy and Geophysics

     National Research Institute of Astronomy and Geophysics

     Egipto

     
  2. [2] El Azhar University, Cairo
• Localización: Applied Mathematics and Nonlinear Sciences, ISSN-e 2444-8656, Vol. 1, Nº. 2, 2016, págs. 321-334
• Idioma: inglés
• DOI: 10.21042/amns.2016.2.00027
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• Resumen

  • We analyzed the first set of complete CCD light curves of the W UMa type eclipsing binary IK Boo in the BVRI bands by using the PHOEBE code and deduced its first photometric parameters with, mass ratio q=0.648q=0.648 and orbital inclination i=63oi=63o. We have applied a spotted model due to the light curves asymmetry. The system shows a distinct O'Connell effect. The best solution fit to the light curves suggested the influence of star spot ss on both components. Such presence of star spotss is common among the RS CVn and W UMa chromospheric active late type stars.

    We also present an analysis of mid-eclipse time measurements of IK Boo. The analysis indicates a period decrease rate dP/dt=−1.68×10−7d/yrdP/dt=−1.68×10−7d/yr, which can be interpreted in terms of mass transfer of rate 3.1×10−7M⊙/yr3.1×10−7M⊙/yr, from the more massive to the less massive component.