Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998aas...192.8206c&link_type=abstract
American Astronomical Society, 192nd AAS Meeting, #82.06; Bulletin of the American Astronomical Society, Vol. 30, p.1156
Astronomy and Astrophysics
Astronomy
3
Scientific paper
We have observed EY Cyg at low and high dispersion during minimum light. We found a K1V spectral type for the secondary star. The measured radial velocity curve of the emission and absorption components, yield semiamplitudes Kem = 30 +/- 2 km s(-1) and Kabs = 64 +/- 5 km s(-1) . The orbital period is 0.450617 +/- 0.000001 days, a value much larger than previously reported. The observed rotational velocity of the secondary is Vrot sin i = 30 +/- 5 km s(-1) , consistent with the predicted rotational velocity assuming that EY Cyg B fills its Roche-Lobe and co-rotates with the binary. This also implies that the assumption K_W = Kem and K_R = Kabs is valid. The masses and the binary separation of the components are M_W sin(3) i = 0.0264 +/- 0.0060 Msun, M_R sin(3) i = 0.0124 +/- 0.0027 Msun, and a sin i = 0.8369 +/- 0.0623 Rsun. Very tight limits for the inclination angle can be imposed for this cataclysmic variable, with values between 15 to 17 degrees. The most likely value is i = 16(o) , consistent with an analysis of the mass and radius of the secondary star. For this value M_R = 0.59 Msun, M_W = 1.26 Msun and a= 3.03 Rsun. These results imply that EY Cyg B is in fact a K5 star with a mean radius 25 percent greater than a normal main sequence star for the same mass, and with its surface heated, probably by the accretion disk and/or the white dwarf.
Costero Rafael
Echevarria J. J.
Pineda L.
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