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On the Binarity of the F0p Magnetic Stars ϒ Equ and 49 Cam

Published online by Cambridge University Press:  12 April 2016

D.E. Mkrtichian ,
N.N. Samus ,
N.A. Gorynya ,
P. North  and
A.P. Hatzes
D.E. Mkrtichian
Affiliation:
Astronomical Observatory, Odessa State University, Shevchenko Park, Odessa, 270014, Ukraine
N.N. Samus
Affiliation:
Institute of Astronomy, Russian Academy of Sciences, Pyatnitskaya Str. 48, Moscow 109017, Russia
N.A. Gorynya
Affiliation:
Institute of Astronomy, Russian Academy of Sciences, Pyatnitskaya Str. 48, Moscow 109017, Russia
P. North
Affiliation:
Institut d’Astronomiede, l’Universite de Lausanne, CH-1290 Chavannes-des-Bois, Switzerland
A.P. Hatzes
Affiliation:
McDonald Observatory, University of Texas at Austin, Austin, U.S.A.

Extract

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The magnetic field investigations of the rapidly-oscillating (ro)Ap star ϒ Equ show a very long magnetic (rotational) period of about 74 years (Leroy et al. 1994; Bychkov & Shtol 1997). No significant changes of radial velocities were detected during the history of investigations of this star. Recently, Scholz et al. (1997) (hereafter S97) reported a rapid increase of radial velocity (RV) of ϒ Equ from the mean value of -16.81 km s−1 up to a maximum at -4.28 km s−1 within the interval JD 2449608 – JD 2450356, and suggested that ϒ Equ is a long-period binary star with high eccentricity. Such a probable discovery of binary motion of ϒ Equ is very interesting, since it opens the possibility to compare asteroseismic parameters of the star with those obtained from the binary orbit.

Type
Part 8. Binary Stars
Information
International Astronomical Union Colloquium , Volume 170: Precise Stellar Radial Velocities , 1999 , pp. 331 - 334
Copyright
Copyright © Astronomical Society of the Pacific 1999

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