Formation of phase lags at the cyclotron energies in the pulse profiles of magnetized, accreting neutron stars
Creators
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1.
Leibniz Institute for Astrophysics Potsdam
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2.
University of Geneva
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3.
University of Tübingen
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4.
European Space Astronomy Centre
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5.
George Mason University
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6.
United States Naval Research Laboratory
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7.
Goddard Space Flight Center
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8.
International Space Science Institute
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9.
California Institute of Technology
Abstract
Context. Accretion-powered X-ray pulsars show highly energy-dependent and complex pulse-profile morphologies. Significant deviations from the average pulse profile can appear, in particular close to the cyclotron line energies. These deviations can be described as energy-dependent phase lags, that is, as energy-dependent shifts of main features in the pulse profile. Aims. Using a numerical study we explore the effect of cyclotron resonant scattering on observable, energy-resolved pulse profiles. Methods. We generated the observable emission as a function of spin phase, using Monte Carlo simulations for cyclotron resonant scattering and a numerical ray-tracing routine accounting for general relativistic light-bending effects on the intrinsic emission from the accretion columns. Results. We find strong changes in the pulse profile coincident with the cyclotron line energies. Features in the pulse profile vary strongly with respect to the average pulse profile with the observing geometry and shift and smear out in energy additionally when assuming a non-static plasma. Conclusions. We demonstrate how phase lags at the cyclotron energies arise as a consequence of the effects of angular redistribution of X-rays by cyclotron resonance scattering in a strong magnetic field combined with relativistic effects. We also show that phase lags are strongly dependent on the accretion geometry. These intrinsic effects will in principle allow us to constrain a system's accretion geometry.
Additional Information
© 2014 ESO. Received 6 August 2013. Accepted 9 March 2014. Published online 04 April 2014. We thank the International Space Science Institute ISSI in Bern (CH) for granting two International Team meetings on "The physics of the accretion column of X-ray pulsars", which have much inspired this collaborative work. We also thank the Bundesministerium für Wirtschaft und Technologie for funding through Deutsches Zentrum für Luft- und Raumfahrt grant 50 OR 1113. M.T.W. is supported by the US Office of Naval Research and the NASA ADAP Program under grant NNH13AV18I. We thank the anonymous referee for very useful comments.Attached Files
Published - aa22448-13.pdf
Submitted - 1405.6855v2.pdf
Files
1405.6855v2.pdf
Additional details
Identifiers
- Eprint ID
- 46057
- Resolver ID
- CaltechAUTHORS:20140603-143146615
Related works
- Describes
- http://arxiv.org/abs/1405.6855 (URL)
Funding
- International Space Science Institute (ISSI)
- Deutsches Zentrum für Luft- und Raumfahrt (DLR)
- 50 OR 1113
- Office of Naval Research (ONR)
- NASA
- NNH13AV18I
Dates
- Created
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2014-06-03Created from EPrint's datestamp field
- Updated
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2021-11-10Created from EPrint's last_modified field