An analysis of the light curves of the overcontact binary system V2388 Ophiuchi

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Yakut K. , Kalomeni B. , Ibanoglu C.

ASTRONOMY & ASTROPHYSICS, vol.417, no.2, pp.725-730, 2004 (Journal Indexed in SCI) identifier identifier

  • Publication Type: Article / Article
  • Volume: 417 Issue: 2
  • Publication Date: 2004
  • Doi Number: 10.1051/0004-6361:20031773
  • Title of Journal : ASTRONOMY & ASTROPHYSICS
  • Page Numbers: pp.725-730
  • Keywords: stars : binaries : eclipsing, stars : binaries : visual, stars : fundamental parameters, stars : individual : V2388 Oph, techniques : photometric, STARS, UMA, PHOTOMETRY, HIPPARCOS, ORBITS, MODELS, CYGNI


We present four seasons' (2000-2003) ground-based photometry of the short-period contact binary V2388 Oph. The system is the brighter component of visual binary HIP 87655. The magnitude difference between the visual companion and the eclipsing pair was estimated to be 1(m).19, 1(m).09 and 1(m).09 in B, V and R bandpasses, respectively. The light curves in BVR are solved by the WD code. Combining the parameters found by the light curve analysis with those of the radial velocity solution we derived the masses and radii of the star components as: M-1 = 1.80(2) M., M-2 = 0.34(1) M., R-1 = 2.60(2) R., R-2 = 1.30(1) R.. The primary component appears to be more evolved in the mass-radius, mass-luminosity planes and also in the HR diagram. It lies near the terminal-age main-sequence, which agrees well with the position of deeper-contact A-type systems. The large fill-out factor of 0.65 does also support this classification.