Orbital Parameters and Chemical Composition of Four White Dwarfs in Post-Common-Envelope Binaries

Abstract

We present FUSE observations of the hot white dwarfs in the post-common-envelope binaries Feige 24, EUVE J0720-317, BPM 6502, and EUVE J2013+400. The spectra show numerous photospheric absorption lines, which trace the white dwarf orbital motion. We report the detection of C III, O VI, P V, and Si IV in the spectra of Feige 24, EUVE J0720-317, and EUVE J2013+400 and the detection of C III, N II, Si III, Si IV, and Fe III in the spectra of BPM 6502. Abundance measurements support the possibility that white dwarfs in post-common-envelope binaries accrete material from the secondary star wind. The FUSE observations of BPM 6502 and EUVE J2013+400 cover a complete binary orbit. We used the FUSE spectra to measure the radial velocities traced by the white dwarf in the four binaries, where the zero-point velocities were fixed using the ISM velocities in the line of sight of the stellar systems. For BPM 6502 we determined a white dwarf velocity semiamplitude of K_WD = 18.6 +/- 0.5 km s^-1, and with the velocity semiamplitude of the red dwarf companion (K_RD = 75.2 +/- 3.1 km s^-1), we estimate the mass ratio to be q = 0.25 +/- 0.01. Adopting a spectroscopic mass determination for the white dwarf, we infer a low secondary mass of M_RD = 0.14 +/- 0.01 M_⊙. For EUVE J2013+400 we determine a white dwarf velocity semiamplitude of K_WD = 36.7 +/- 0.7 km s^-1. The FUSE observations of EUVE J0720-317 cover approximately 30% of the binary period and, combined with the HST GHRS measurements, we update the binary properties. FUSE observations of Feige 24 cover approximately 60% of the orbit, and we combine this data set with HST STIS data to update the binary properties.