Spectroscopy of the extreme-ultraviolet source Feige 24 - The binary orbit and the mass of the white dwarf

Details Spectroscopy of the extreme-ultraviolet source Feige 24 - The binary orbit and the mass of the white dwarf Spectroscopy of the extreme-ultraviolet source Feige 24 - The binary orbit and the mass of the white dwarf

Jul 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...223..260t&link_type=abstract

Astrophysical Journal, Part 1, vol. 223, July 1, 1978, p. 260-265.

Astronomy and Astrophysics

Astronomy

47

Astronomical Spectroscopy, Binary Stars, Emission Spectra, Ultraviolet Astronomy, White Dwarf Stars, Astronomical Photometry, Far Ultraviolet Radiation, Line Spectra, Radial Velocity

Scientific paper

Results are reported for coude spectroscopy of the extreme-ultraviolet white dwarf Feige 24. Radial velocities of the H-alpha, He I 5876-A, and He I 6678-A emission lines, and the underlying M-dwarf absorption features, were determined from spectrograms obtained with the Lick 3-m telescope. The velocities show a binary period of 4.239(+ or - 0.0015) days. The emission-line and absorption-line velocities agree in phase, which indicates that the emission lines originate in the atmosphere of the M-dwarf secondary as a result of reprocessing of the EUV radiation. This effect is modeled, and the observed amplitude of the emission-line variability is used to place a lower limit on the orbital inclination. From these and other data it is shown that the mass of the white dwarf lies between 0.46 and 1.24 solar masses. Some possible implications for the evolution of binary stars are briefly discussed.

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