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Title:
Enlightening differences in AMSPs behavior: XTE J1751-305 vs. XTE J1814-338
Authors:
Papitto, A.; Riggio, A.; di Salvo, T.; Burderi, L.; Menna, M. T.
Affiliation:
AA(Dip. di Fisica, Univ. di Roma ``Tor Vergata'', via detta Ricerca Scientifica 1, 00133 Roma, Italy; INAF OAR, via di Frascati 33, Monte Porzio Catone, 00040 Italy), AB(Dip. di Fisica, Univ. di Cagliari, SP Monserrato-Sestu, KM 0.7, Monserrato, 09042 Italy), AC(Dip. di Scienze Fisiche ed Astronomiche, Univ. di Palermo, via Archirafi 36, Palermo, 90123, Italy), AD(Dip. di Fisica, Univ. di Cagliari, SP Monserrato-Sestu, KM 0.7, Monserrato, 09042 Italy), AE(INAF OAR, via di Frascati 33, Monte Porzio Catone, 00040 Italy)
Publication:
A DECADE OF ACCRETING MILLISECOND X-RAY PULSARS. AIP Conference Proceedings, Volume 1068, pp. 51-54 (2008). (AIPC Homepage)
Publication Date:
10/2008
Origin:
AIP
PACS Keywords:
X-ray emission spectra and fluorescence, Pulsars, X-ray binaries
DOI:
10.1063/1.3031205
Bibliographic Code:
2008AIPC.1068...51P

Abstract

We summarize here the main results of the timing analysis performed on the pulsed X-ray emission of XTE J1751-305 and XTE J1814-338. These two sources encompass some of the main issues regarding the rotational evolution of Accreting Millisecond Pulsars: they have an opposite rotational reaction to the accretion of mass and only the phases of XTE J1751-305 evolve smoothly, while in XTE J1814-338 a modulation around an average trend appears in anti correlation with variations of the emitted X-ray flux. We explore the possibility that this phenomenon is related to variations of the mass accretion rate on each spot, but only the behavior of the fundamental Fourier component could be fully reproduced according to the considered model. The most favorable explanation of this effect therefore appears to be still in terms of motions of the accretion path from the disk to the Neutron Star.
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