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The peculiar binary system HR 8891 (ET And)

Published online by Cambridge University Press:  26 May 2016

R. Kuschnig ,
W. W. Weiss ,
N. Piskounov ,
T. Ryabchikova ,
T.J. Kreidl ,
M. Alvarez ,
S.G. Bedolla ,
S.J. Bus ,
Z. Guo  and
J. Hao
...Show all authors
R. Kuschnig
Affiliation:
Institute for Astronomy, Vienna
W. W. Weiss
Affiliation:
Institute for Astronomy, Vienna
N. Piskounov
Affiliation:
Astronomical Institute of the Russian Academy of Sciences, Moscow
T. Ryabchikova
Affiliation:
Astronomical Institute of the Russian Academy of Sciences, Moscow
T.J. Kreidl
Affiliation:
Lowell Observatory, Flagstaff
M. Alvarez
Affiliation:
Instituto de Astronomia - UNAM, Mexico
S.G. Bedolla
Affiliation:
Instituto de Astronomia - UNAM, Mexico
S.J. Bus
Affiliation:
Lowell Observatory, Flagstaff
Z. Guo
Affiliation:
Beijing Astronomical Observatory
J. Hao
Affiliation:
Beijing Astronomical Observatory
L. Huang
Affiliation:
Beijing Astronomical Observatory
F. Kupka
Affiliation:
Institute for Astronomy, Vienna
D. Le Contel
Affiliation:
Observatoire de la Côte d'Azur, Nice
J.M. Le Contel
Affiliation:
Observatoire de la Côte d'Azur, Nice
D.J. Osip
Affiliation:
Lowell Observatory, Flagstaff
K. Panov
Affiliation:
Institute of Astronomy, Sofia
N. Polosukchina
Affiliation:
Crimean Astrophysical Observatory, Ukraine
J.P. Sareyan
Affiliation:
Observatoire de la Côte d'Azur, Nice
H. Schneider
Affiliation:
Universitätssternwarte, Göttingen
J.C. Valtier
Affiliation:
Observatoire de la Côte d'Azur, Nice
M. Zboril
Affiliation:
Astronomical Institute of the Slovak Academy of Sciences, Tatranska Lomnica
J. Žižňovský
Affiliation:
Astronomical Institute of the Slovak Academy of Sciences, Tatranska Lomnica
J. Zverko
Affiliation:
Astronomical Institute of the Slovak Academy of Sciences, Tatranska Lomnica

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ET And is a binary system with a B9 Si star as the main component (Porb = 48.308d, e=0.46). Controversial claims in the literature concerning pulsation with periods ranging from few minutes to few hours and with variable amplitudes indicated a challenging target and motivated us to organize several photometric and spectroscopic observing campaigns. The problem with pulsation of ET And is that Teff and log g put this star in the cool domain of Slowly Pulsating B-type (SPB) stars, but the pulsation periods would be too short by a factor of about four, relatively to the shortest hitherto known periods for SPB stars.

Type
1. Pulsation and Rotation
Information
Symposium - International Astronomical Union , Volume 162: Pulsation, Rotation and Mass Loss in Early-Type Stars , 1994 , pp. 43 - 46
Copyright
Copyright © Kluwer 1994