Light curve modeling of eclipsing binaries towards the constellation of Carina

• Published in: arXiv.org 2015-02
• Main Authors: Dey, Aniruddha, Deb, Sukanta, Kumar, Subhash, Bharadwaj, Hrishabh, Bhattacharya, Barnmoy, Richa, Sharma, Angad, Chauhan, Akshyata, Tiwari, Neha, Kaur, Sharanjit, Kumar, Suman, Abhishek
• Format: Article
• Language: English
• Subjects: Binary stars; Celestial bodies; Classification; Constellations; Eclipsing binary stars; European Southern Observatory; Hubble constant; Light; Light curve; Luminosity; Mass ratios; Mathematical models; Modelling; Parameters; Photometry; Physical properties; Starbursts; Stars & galaxies; Universe; Very Large Telescope
• ISSN: 2331-8422

We present a detailed V-band photometric light curve modeling of 30 eclipsing binaries using the data from Pietrukowicz et al. (2009) collected with the European Southern Observatory Very Large Telescope (ESO VLT) of diameter 8-m. The light curve of these 30 eclipsing binaries were selected out of 148 of them available in the database on the basis of complete phase coverage, regular and smooth phased light curve shapes. Eclipsing binaries play pivotal role in the direct measurement of astronomical distances more accurately simply from their geometry of light curves. The accurate value of Hubble constant (H0) which measures the rate of expansion of the Universe heavily relies on extragalactic distance scale measurements. Classification of the selected binary stars in the sample were done, preliminarily on the basis of Fourier parameters in the a2-a4 plane and final classification was obtained from the Roche lobe geometry. Out of these 30 eclipsing binaries, only one was found to be detached binary system while the rest 29 of them belong to the contact binary systems. These contact binaries were further classified into the A-type and W-type based on their mass ratios. Since spectroscopic mass ratio measurements were not available for any of these binary stars, we determined the mass ratios through photometric light curve modeling with the aid of Wilson-Devinney code as implemented in PHOEBE. Various geometrical parameters and physical parameters of astrophysical importance viz., mass, radius and luminosity were obtained from the light curves of the selected stars.