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Investigation of the Rapid Magnetic Field Variability in γ Equulei

Bychkov V. D., Bychkova L. V., Madej J.

Acta Astronomica

2005

Vol. 55, No. 1

141--149

We investigated magnetic variability of the roAp star &gamma Equ (HD 201601) with high time resolution. Measurements of the stellar longitudinal magnetic field Be were performed with the hydrogen line polarimeter and the 6-m optical telescope of the Special Astrophysical Observatory (Russia) on 20/21 August 1989. We obtained a single 3-hour series of 1720 rapid Be measurements for this star with the average time resolution of 6.6 sec. The averaged value of Be on this night equals to -750±22 G. Both the power spectrum and the amplitude spectrum of the Be time series are essentially flat. However, they show the presence of a marginally significant magnetic period at PB=3.596 min which is real with the probability of 67%. The amplitude of the magnetic field variations with this period equals 347±31 G. We did not detect variations of Be field in γ Equ with the well-known photometric period, Pphot=12.44 min.

The Influence of Reprocessing in the Column on the Light Curves of Accretion Powered Neutron Stars

Čemeljić M., Bulik T.

Acta Astronomica

1998

Vol. 48, No. 1

65--75

Flow of matter onto strongly magnetized neutron stars in X-ray binaries proceeds through accretion funnels that roughly follow geometry of the magnetic field. X-rays originate near the surface of the neutron star, and it may happen that the accretion flow passes through the line of sight as the star rotates. We consider the effects of such accretion flow eclipses on the X-ray light curves of accretion powered pulsars, and present a set of X-ray light curves measured by BATSE for A0535+262 for which this phenomenon is very likely to take place.