Pulse-to-pulse variations in accreting X-ray pulsars

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https://www.epj-conferences.org/articles/epjconf/abs/2014/01/epjconf_mag2013_06012/epjconf_mag2013_06012.html

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https://doi.org/10.1051/epjconf/20136406012
 http://hdl.handle.net/11603/29594

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UMBC Center for Space Sciences and Technology (CSST) / Center for Research and Exploration in Space Sciences & Technology II (CRSST II)
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UMBC Physics Department
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https://orcid.org/0000-0002-4656-6881

Date

2014-01-08

Type of Work

conference papers and proceedings
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Citation of Original Publication

Kretschmar, Peter, Diana Marcu, Matthias Kühnel, Dmitry Klochkov, Katja Pottschmidt, Rüdiger Staubert, Colleen A. Wilson-Hodge, Peter A. Jenke, Isabel Caballero, and Felix Fürst. “Pulse-to-Pulse Variations in Accreting X-Ray Pulsars.” EPJ Web of Conferences 64 (2014): 06012. https://doi.org/10.1051/epjconf/20136406012.

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This work was written as part of one of the author's official duties as an Employee of the United States Government and is therefore a work of the United States Government. In accordance with 17 U.S.C. 105, no copyright protection is available for such works under U.S. Law.
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Abstract

In most accreting X-ray pulsars, the periodic signal is very clear and easily shows up as soon as data covering sufficient pulse periods (a few ten) are available. The mean pulse profile is often quite typical for a given source and with minor variations repeated and recognisable across observations done years or even decades apart. At the time scale of individual pulses, significant pulse-to-pulse variations are commonly observed. While at low energies some of these variations might be explained by absorption, in the hard X-rays they will reflect changes in the accretion and subsequent emission. The amount of these variations appears to be quite different between sources and contains information about the surrounding material as well ass possibly interactions at the magnetosphere. We investigate such variations for a sample of well-known sources.