Observational evidences of erratic 1st harmonic pulse phase shifts in accreting millisecond X-ray pulsars pulse phase evolution was reported by several authors. This effect always go together with much more stable 2nd harmonics pulse phase delays. Different possible explanations of these phase shifts have been given in literature. But all these interpretations do not explain why the 2nd harmonic are more stable than the 1st harmonic. The explanation of such a behaviour is of fundamental importance in order to gain an insight on the NS rotational behaviour and to remove the still present interpretative ambiguity on the results of timing analysis. We propose a simple toy-model to interpret these phenomena as effect of small variations of the ratio between the fluxes from the two hot-spots. We show how it affects the phase of the overall pulse profile, when the two amplitudes are similar and the two hot-spots are not perfectly antipodal. Using this model, we give a detailed explanation of the phase jump observed in the 2002 outburst of SAX J1808.4-3658.

A model to interpret pulse phase shifts in AMXPs: SAX J1808.4-3658 as a proof of concept

RIGGIO, ALESSANDRO;BURDERI, LUCIANO;
2011-01-01

Abstract

Observational evidences of erratic 1st harmonic pulse phase shifts in accreting millisecond X-ray pulsars pulse phase evolution was reported by several authors. This effect always go together with much more stable 2nd harmonics pulse phase delays. Different possible explanations of these phase shifts have been given in literature. But all these interpretations do not explain why the 2nd harmonic are more stable than the 1st harmonic. The explanation of such a behaviour is of fundamental importance in order to gain an insight on the NS rotational behaviour and to remove the still present interpretative ambiguity on the results of timing analysis. We propose a simple toy-model to interpret these phenomena as effect of small variations of the ratio between the fluxes from the two hot-spots. We show how it affects the phase of the overall pulse profile, when the two amplitudes are similar and the two hot-spots are not perfectly antipodal. Using this model, we give a detailed explanation of the phase jump observed in the 2002 outburst of SAX J1808.4-3658.
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11584/88295
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