LOW-FREQUENCY QUASI-PERIODIC OSCILLATION FROM THE 11 Hz ACCRETING PULSAR IN TERZAN 5: NOT FRAME DRAGGING

被引：29

作者：

Altamirano, D. ^{[1
]}

Ingram, A. ^{[2
]}

van der Klis, M. ^{[1
]}

Wijnands, R. ^{[1
]}

Linares, M. ^{[3
]}

Homan, J. ^{[3
]}

机构：

[1] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands

[2] Univ Durham, Dept Phys, Durham DH1 3LE, England

[3] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2012年 / 759卷 / 01期

关键词：

binaries: close; stars: individual (IGR J17480; 2446; Terzan; 5); X-rays: binaries; X-RAY BINARIES; BLACK-HOLE CANDIDATES; LENS-THIRRING PRECESSION; ROTATING NEUTRON-STARS; ATOLL SOURCE STATES; SOURCE GX 340+0; IGR J17480-2446; RELATIVISTIC PRECESSION; SPECTRAL PROPERTIES; POWER SPECTRA;

D O I：

10.1088/2041-8205/759/1/L20

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report on six RXTE observations taken during the 2010 outburst of the 11 Hz accreting pulsar IGR J17480-2446 located in the globular cluster Terzan 5. During these observations we find power spectra which resemble those seen in Z-type high-luminosity neutron star low-mass X-ray binaries, with a quasi-periodic oscillation (QPO) in the 35-50 Hz range simultaneous with a kHz QPO and broadband noise. Using well-known frequency-frequency correlations, we identify the 35-50 Hz QPOs as the horizontal branch oscillations, which were previously suggested to be due to Lense-Thirring (LT) precession. As IGR J17480-2446 spins more than an order of magnitude more slowly than any of the other neutron stars where these QPOs were found, this QPO cannot be explained by frame dragging. By extension, this casts doubt on the LT precession model for other low-frequency QPOs in neutron stars and perhaps even black hole systems.

引用

页数：5

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