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Study of Pulsations in the Nova-like Variable KR Aur and the Intermediate Polar BG CMi

Published online by Cambridge University Press:  25 April 2016

J. Singh ,
P. C. Agrawal ,
M. V. K. Apparao ,
R. K. Manchanda ,
P. Vivekananda Rao  and
M. B. K. Sarma
J. Singh
Affiliation:
Tata Institute of Fundamental Research, Homi Bhabha Road, Bombay 400 005, India
P. C. Agrawal
Affiliation:
Tata Institute of Fundamental Research, Homi Bhabha Road, Bombay 400 005, India
M. V. K. Apparao
Affiliation:
Tata Institute of Fundamental Research, Homi Bhabha Road, Bombay 400 005, India
R. K. Manchanda
Affiliation:
Tata Institute of Fundamental Research, Homi Bhabha Road, Bombay 400 005, India
P. Vivekananda Rao
Affiliation:
Department of Astronomy, Osmania University, Hyderabad 500 007, India
M. B. K. Sarma
Affiliation:
Department of Astronomy, Osmania University, Hyderabad 500 007, India
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Abstract

Fast photometric observations of a nova-like variable KR Aurigae and the intermediate polar BG CMi (3A0729+103) were made in the B and U bands during 1984–89 to study pulsations in them. The light curves of KR Aur show large amplitude quasi-periodic pulsations with periods in the range 500–800s which can be ascribed to inhomogeneities in the accretion disc. The light curves of the X-ray emitting intermediate polar BG CMi show variable amplitude pulsations with 913s period. From the times of maxima of the pulsations obtained from observations over the period 1984–1989, the pulsation period is derived to be 0.010572966 ± 8 days and the spin-up rate to be (−5.7 ± 0.5) × 10−11 ss−1. The spin-up rate is consistent with the pulsating source being a white dwarf and not a neutron star.

Type
Galactic and Stellar
Information
Publications of the Astronomical Society of Australia , Volume 9 , Issue 2 , 1991 , pp. 279 - 280
Copyright
Copyright © Astronomical Society of Australia 1991

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