Enlightening differences in AMSPs behavior: XTE J1751-305 vs. XTE J1814-338

被引：0
作者：
Papitto, A. [1 ,2 ]
Riggio, A. [3 ]
Di Salvo, T. [4 ]
Burderi, L. [3 ]
Menna, M. T. [2 ]
机构：
[1] Univ Roma Tor Vergata, Dip Fis, Via Ricerca Sci 1, I-00133 Rome, Italy
[2] INAF OAR, I-00040 Monte Porzio Catone, Italy
[3] Univ Cagliari, Dipartimento Fis, I-09024 Cagliari, Italy
[4] Univ Palermo, Dipartimento Sci Fis Astronomiche, I-90123 Palermo, Italy
来源：
DECADE OF ACCRETING MILLISECOND X-RAY PULSARS | 2008年 / 1068卷
关键词：
stars: neutron; stars: magnetic fields; pulsars: general; pulsars: individual: XTE J1814-338; pulsars: individual: XTE J1751-305; X-ray: binaries;
D O I：
暂无
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
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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页码：51 / +
页数：2
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