On the eclipsing cataclysmic variable star HBHA 4705-03

TL;DR

This paper presents detailed observations and modeling of the eclipsing binary star HBHA 4705-03, estimating its fundamental parameters, analyzing its variability, and classifying it as a nova-like variable star.

Contribution

The study provides the first detailed parameter estimation and light curve analysis of HBHA 4705-03, including mass ratio, component masses, and accretion rate, using decomposition and modeling techniques.

Findings

Mass ratio q=0.62 ± 0.07

White dwarf mass ~0.8 M_sun

Accretion rate ~2.5 x 10^{18} g/s

Abstract

We present observations and analysis of a new eclipsing binary HBHA 4705-03. Using decomposition of the light curve into accretion disk and hot spot components, we estimated photometrically the mass ratio of the studied system to be q=0.62 +-0.07. Other fundamental parameters was found with modeling. This approach gave: white dwarf mass M_1 = (0.8 +- 0.2) M_sun, secondary mass M_2=(0.497 +- 0.05) M_sun, orbital radius a=1.418 R_sun, orbital inclination i = (81.58 +- 0.5) deg, accretion disk radius r_d/a = 0.366 +- 0.002, and accretion rate dot{M} = (2.5 +- 2) * 10^{18}[g/s], (3*10^{-8} [M_sun/yr]). Power spectrum analysis revealed ambiguous low-period Quasi Periodic Oscillations centered at the frequencies f_{1}=0.00076 Hz, f_2=0.00048 Hz and f_3=0.00036 Hz. The B-V=0.04 [mag] color corresponds to a dwarf novae during an outburst. The examined light curves suggest that HBHA 4705-03 is a nova-like variable star.