Based on observations carried out at the Observatório do Pico dos Dias/Laboratório Nacional de Astrofísica (OPD/LNA) in Brazil.
A photometric and spectroscopic study of NSVS 14256825: the second sdOB+dM eclipsing binary★
Article first published online: 10 APR 2012
© 2012 The Authors Monthly Notices of the Royal Astronomical Society © 2012 RAS
Monthly Notices of the Royal Astronomical Society
Volume 423, Issue 1, pages 478–485, June 2012
How to Cite
Almeida, L. A., Jablonski, F., Tello, J. and Rodrigues, C. V. (2012), A photometric and spectroscopic study of NSVS 14256825: the second sdOB+dM eclipsing binary. Monthly Notices of the Royal Astronomical Society, 423: 478–485. doi: 10.1111/j.1365-2966.2012.20891.x
- Issue published online: 30 MAY 2012
- Article first published online: 10 APR 2012
- Accepted 2012 March 8. Received 2012 March 8; in original form 2012 January 13
- binaries: eclipsing;
- stars: fundamental parameters;
- stars: individual: NSVS 14256825;
- stars: low-mass;
We present an analysis of UBVRCICJH photometry and phase-resolved optical spectroscopy of NSVS 14256825, an HW Vir type binary. The members of this class consist of a hot subdwarf and a main-sequence low-mass star in a close orbit (Porb∼ 0.1 d). Using the primary-eclipse timings, we refine the ephemeris for the system, which has an orbital period of 0.110 37 d. From the spectroscopic data analysis, we derive the effective temperature, T1= 40 000 ± 500 K, the surface gravity, log g1= 5.50 ± 0.05, and the helium abundance, , for the hot component. Simultaneously modelling the photometric and spectroscopic data using the Wilson–Devinney code, we obtain the geometrical and physical parameters of NSVS 14256825. Using the fitted orbital inclination and mass ratio (i= 82°.5 ± 0°.3 and q=M2/M1= 0.260 ± 0.012, respectively), the components of the system have M1= 0.419 ± 0.070 M⊙, R1= 0.188 ± 0.010 R⊙, M2= 0.109 ± 0.023 M⊙ and R2= 0.162 ± 0.008 R⊙. From its spectral characteristics, the hot star is classified as a subdwarf OB (sdOB) star.