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Luminosity Dependent Changes of Pulse Profiles in the X-ray Binary GX 1+4

Published online by Cambridge University Press:  05 March 2013

J. G. Greenhill ,
D. Galloway  and
M. C. Storey
J. G. Greenhill
Affiliation:
Physics Department, University of Tasmania, GPO Box 252C, Hobart, Tas. 7001, Australia; [email protected]
D. Galloway
Affiliation:
Physics Department, University of Tasmania, GPO Box 252C, Hobart, Tas. 7001, Australia; [email protected] Special Research Centre for Theoretical Astrophysics, School of Physics, University of Sydney, NSW 2006, Australia; [email protected]
M. C. Storey
Affiliation:
Special Research Centre for Theoretical Astrophysics, School of Physics, University of Sydney, NSW 2006, Australia; [email protected]
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Abstract

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We have reviewed the X-ray pulse profiles from a large number of observations of the accreting binary pulsar GX 1+4 obtained during the last 25 years. The profiles cover various energy ranges between 1 and 100 keV. Using these data we present a coherent picture of present and past pulse profiles and the variations of these pulse profiles with time. The pulse shape is dependent on both the X-ray luminosity and whether the pulsar is spinning up or down. Profiles measured during the GX 1+4 high state in the 1970s are all trailing edge bright. Subsequently the profiles have generally been symmetric or leading edge bright. Rossi X-ray Timing Explorer (RXTE) satellite data taken in July 1996 show that similar pulse shape variations can occur on a timescale of hours. The implications of this new information for accretion models is discussed.

Keywords

X-rays: starsaccretion diskspulsars: individual: GX 1+4
Type
Research Article
Information
Publications of the Astronomical Society of Australia , Volume 15 , Issue 2 , 1998 , pp. 254 - 258
Copyright
Copyright © Astronomical Society of Australia 1998

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