The pulse-timing and emission-line orbits of the white dwarf in the cataclysmic variable AE Aquarii

Details The pulse-timing and emission-line orbits of the white dwarf in the cataclysmic variable AE Aquarii The pulse-timing and emission-line orbits of the white dwarf in the cataclysmic variable AE Aquarii

Jun 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...374..298r&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 374, June 10, 1991, p. 298-306.

Astronomy and Astrophysics

Astrophysics

31

Cataclysmic Variables, Emission Spectra, Stellar Orbits, Stellar Oscillations, Variable Stars, White Dwarf Stars, K Stars, Novae, Stellar Mass, Stellar Rotation, Stellar Spectrophotometry

Scientific paper

The emission-line and the pulse-timing orbits of AE Aqr have been remeasured. From the emission-line orbit, an improved value for the orbital period, 0.4116580 (+ or - 2) days, and an improved value for the amplitude of the radial velocity variations, 141 + or - 8 km/s are derived. Based on the new photometry, the revised ephemeris for the 16.5 s component of the 33 s modulation is Tmax = BJED 2,445,171.999844(+ or - 1) + 0.000191416425(+ or - 1)E, and the semiamplitude of the pulse-timing orbit is 2.30 + or - 0.07 s, which is equivalent to K(pulse) = 122 + or - 4 km/s. It is shown that the pulse-timing orbit is distorted, probably by reprocessing of the pulses in the accreting gas, and cannot be used to estimate the orbit of the white dwarf reliably.

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