Computer Science
Scientific paper
Jun 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006javso..35..136e&link_type=abstract
The Journal of the American Association of Variable Star Observers, Vol. 35, No. 1, p. 136
Computer Science
1
Scientific paper
High-dispersion time-resolved spectroscopy of the cataclysmic variable AE Aqr has been obtained. The emission lines have a complex structure that make difficult to measure the motion of the white dwarf. The cross correlation for the absorption lines shows a clear asymmetric profile as expected from a heated side of the red star. The spectral type for the secondary star varies from K2 to K5; there are clear indications that the temperature varies as a function of star longitude. The radial velocity analysis yield Kab = 165.2 ± 0.6 Km s-1 for the cross-correlated secondary star. The rotational velocity of the red star has been measured as a function of orbital period. It shows ellipsoidal variations with a period half the orbital period. The rotational velocities vary within the range Vrot sin i = 105 ± 3 Km s-1 and Vrot sin i = 130 ± 3 Km s-1. The former can be used to constrain the white dwarf semi-amplitude value to yield Kem = 139 ± 4 Km s-1 consistent with derived values from published radial velocity measurements. From a variation in the absorption line strength of 30%, we constrain the inclination angle to i = 58° ± 3. The estimated masses of the binary are: Mw = 1.07 ± 0.07 M? and Mr = 0.90 ± 0.05 M?. If this is correct we should expect a spectral type of G5 if the secondary star is a main sequence star. We suggest that the discrepancy is explained if the star has a radius 40% greater than a main sequence star for a mass of 0.90 M?.
Connon Smith Robert
Diego Francisco
Echevarria J. J.
Mills Donald
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