A new analysis of the radial velocity variations of the eclipsing and spectroscopic binary EN Lacertae

Details A new analysis of the radial velocity variations of the eclipsing and spectroscopic binary EN Lacertae A new analysis of the radial velocity variations of the eclipsing and spectroscopic binary EN Lacertae

Feb 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001a%26a...367..236l&link_type=abstract

Astronomy and Astrophysics, v.367, p.236-249 (2001)

Astronomy and Astrophysics

Astrophysics

16

Stars: Binaries: Close, Stars: Binaries: Eclipsing, Stars: Binaries: Spectroscopic, Stars: Fundamental Parameters, Stars: Oscillations, Stars: Individual: En Lac

Scientific paper

An analysis of 1236 new electronic spectra of the eclipsing binary EN Lac from four observatories and of 994 radial velocities (RV hereafter) from photographic spectra, published by several authors, has allowed us to disentangle the RV variations due to orbital motion and due to pulsations of the star. New, accurate orbital elements as well as precise values of the three pulsation periods, already known from the previous studies, were derived. The accuracy of the orbital solution has been substantially improved after the observed RV changes were properly prewhitened for the short-term oscillations. The amplitude of the dominant RV oscillation with a period of P_1=0fd16916703 was found to vary with a 74 year cycle. The amplitudes of the two other RV oscillations, having periods of P_3=0fd 18173256 and P_2=0fd 17085554, vary on much shorter time scales of 674 d and 331 d, respectively. The value of P_2 derived here does not correspond to a one year alias of the value found by several authors from photometry but appears to be an intrinsic period. The time scales of the amplitude modulations found for P_1 and P_3 are in good agreement with previous photometric results. For the first time we present evidence of line profile variations of EN Lac. They correlate well with the short-term RV variations but they alternatively occur with periods corresponding either to the fundamental periods or to the first harmonics of P_1 to P_3. An analysis of the RV scatter along the orbital phase curve for the new spectra, obtained over a relatively short interval of time, gives some indication of a sharp increase of this scatter when the stars are approaching periastron. Since this could be a signature of forced oscillations, the effect is worth further study, though it appears rather marginal at present.
Table 3 is only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/367/236. This research is based on spectra from the Tautenburg, Dominion Astrophysical, Ondřejov, and Haute Provence Observatories.

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