SPIN-DOWN OF THE LONG-PERIOD ACCRETING PULSAR 4U 2206+54

被引：25

作者：

Finger, Mark H. ^{[1
,2
]}

Ikhsanov, Nazar R. ^{[1
,3
,4
]}

Wilson-Hodge, Colleen A. ^{[3
]}

Patel, Sandeep K. ^{[5
]}

机构：

[1] Natl Space Sci & Technol Ctr, Huntsville, AL USA

[2] Univ Space Res Assoc, Huntsville, AL 35806 USA

[3] NASA, Space Sci Off, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA

[4] Pulkovo Observ, St Petersburg 196140, Russia

[5] Opt Sci Corp, Huntsville, AL 35806 USA

来源：

ASTROPHYSICAL JOURNAL | 2010年 / 709卷 / 02期

基金：

美国国家航空航天局; 俄罗斯基础研究基金会;

关键词：

accretion; accretion disks; pulsars: individual (4U 2206+54); X-rays: binaries; X-RAY BINARY; MAGNETIC NEUTRON-STARS; SOURCE 4U-2206+54; WIND-ACCRETION; FIELD DECAY; ORIGIN; MODEL; DISKS;

D O I：

10.1088/0004-637X/709/2/1249

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

4U 2206+54 is a high-mass X-ray binary which has been suspected to contain a neutron star accreting from the wind of its companion, BD+53 degrees 2790. Reig et al. have recently detected 5560 s period pulsations in both Rossi X-ray Timing Explorer (RXTE) and International Gamma-ray Astrophysics Laboratory observations which they conclude are due to the spin of the neutron star. We present observations made with Suzaku which are contemporaneous with their RXTE observation of this source. We find strong pulsations at a period of 5554 +/- 9 s in agreement with their results. We also present a reanalysis of BeppoSAX observations of 4U 2206+54 made in 1998, in which we find strong pulsations at a period of 5420 +/- 28 s, revealing a spin-down trend in this long-period accreting pulsar. Analysis of these data suggests that the neutron star in this system is an accretion-powered magnetar.

引用

页码：1249 / 1256

页数：8

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