eclipsing binary stars back to top



Bottom left: ULTRACAM images taken every 2 seconds of the eclipsing binary star NN Ser and a nearby field star Bottom right: The resulting light curve of NN Ser, showing the deep eclipse when the white dwarf primary is obscured by the red dwarf secondary star. These data have been used to measure the rate at which the orbital period of the binary is decreasing and will be used to measure the mass and radius of the white dwarf.

Brinkworth, Marsh, Dhillon, Knigge, MNRAS, 2005, in press (astro-ph/0510331)