<i>XMM-Newton</i> discovery of transient X-ray pulsar in NGC 1313

Trudolyubov, S.

doi:10.1111/j.1745-3933.2008.00478.x

Cited by 21 publications

(13 citation statements)

References 43 publications

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“…We note that two more extragalactic transient pulsators share striking similarities with the above group, i.e. super-Eddington luminosities and/or large first period derivative, namely XMMU J031747.5-663010 in NGC1313 (∼766 s ;Trudolyubov 2008) and CXOU J073709.1+653544 in NGC2403 (∼18 s; Trudolyubov et al 2007). We suggest here for the first time that they could be two other PULXs that went unnoticed so far.…”

Section: Introductionsupporting

confidence: 53%

Discovery of a 2.8 s pulsar in a 2 d orbit High-Mass X-ray Binary powering the Ultraluminous X-ray source ULX-7 in M51

Castillo,

Israel,

Belfiore

et al. 2019

Preprint

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We discovered 2.8 s pulsations in the X-ray emission of the ultraluminous X-ray source (ULX) M51 ULX-7 within the UNSEeN project, which was designed to hunt for new pulsating ULXs (PULXs) with XMM-Newton. The pulse shape is sinusoidal and large variations of its amplitude were observed even within single exposures (pulsed fraction from less than 5% to 20%). M51 ULX-7 is a variable source, generally observed at an X-ray luminosity between 10 39 and 10 40 erg s −1 , located in the outskirts of the spiral galaxy M51a at a distance of 8.6 Mpc. According to our analysis, the X-ray pulsar orbits in a 2-d binary with a projected semi-major axis a X sin i 28 lt-s. For a neutron star (NS) of 1.4 M , this implies a lower limit on the companion mass of 8 M , placing the system hosting M51 ULX-7 in the high-mass X-ray binary class. The barycentric pulse period decreased by 0.4 ms in the 31 d spanned by our May-June 2018 observations, corresponding to a spinup rate Ṗ −1.5 × 10 −10 s s −1 . In an archival 2005 XMM-Newton exposure, we measured a spin period of ∼3.3 s, indicating a secular spin-up of Ṗsec −10 −9 s s −1 , a value in the range of other known PULXs. Our findings suggest that the system consists of an OB giant and a moderately magnetic (dipole field component in the range 10 12 G B dip 10 13 G) accreting NS with weakly beamed emission (1/12 b 1/4).

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Section: Introductionsupporting

confidence: 53%

Discovery of a 2.8 s pulsar in a 2 d orbit High-Mass X-ray Binary powering the Ultraluminous X-ray source ULX-7 in M51

Castillo,

Israel,

Belfiore

et al. 2019

Preprint

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“…Up to now, 7 sources are believed to be ULX pulsars: M82 X-2 [10], NGC 7793 P13 [11,12], NGC 5907 ULX1 [13], NGC 300 ULX1 [14], NGC 1313 X-2 [15], M51 ULX7 [16], and a source within the Milky Way, Swift J0243.6+6124. XMMU J031747.5-663010 in NGC 1313 [17], SMC X-3 [18,19] and M51 ULX8 [20] may also be ULX pulsars. Recently, Song et al [21] identified 25 sources with their flux changes of more than one order of magnitude from 296 ULXs, and claimed these are possible ULX pulsar candidates.…”

Section: Introductionmentioning

confidence: 98%

Studying magnetic fields of ultraluminous X-ray pulsars using different accretion torques

Chen¹,

Wang²,

Tong³

2021

Preprint

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The magnetic field of ultraluminous X-ray (ULX) pulsars is the key parameter to understand the nature and accretion physics. However, the typical magnetic field values in these ULX pulsars are still under debate. We used six different torque models to study the magnetic fields of ULX pulsars, to see how derived magnetic fields change with different models, and to determine which models are more suitable for ULX pulsars. We took the currently available period, period derivative, and flux data of 7 confirmed ULX pulsars, M82 X-2, ULX NGC 7793 P13, ULX NGC 5907, NGC 300 ULX1, NGC 1313 X-2, M51 ULX-7, Swift J0243.6+6124, plus one potential ULX pulsars, SMC X-3. The magnetic fields of these ULX pulsars were constrained from two physical conditions: the spin-up process and near equilibrium. We checked possible dependence of the magnetic field estimations on the different torque models. The calculations suggest the accretion torque models by Ghosh & Lamb [1], Wang [2], Kluźniak & Rappaport [3] and Campbell [4] are more likely to support magnetar models for ULX pulsars, while Lovelace, Romanova & Bisnovatyi-Kogan [5]'s model generally predicts the magnetic field in normal neutron stars. Implications of our results combined with other independent methods are also discussed, which will help us to understand the nature and rotational behavior of these ULX pulsars.

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“…Ultraluminous X-ray sources (ULXs) are extragalactic, non-AGN X-ray sources with luminosities exceeding 10 39 erg s −1 (Kaaret et al 2017). Observations, in a handful of ULXs, of coherent pulsations of ∼ 1 s periodicities (Bachetti et al 2014;Fürst et al 2016;Israel et al 2017a,b;Carpano et al 2018;Motch et al 2014;Fürst et al 2018;Heida et al 2019;Trudolyubov 2008;Doroshenko et al 2018;Tsygankov et al 2017;Townsend et al 2017;Brightman et al 2018) have shown that at least some of these sources are powered by slowly rotating neutron stars accreting above their critical limits, ṀEdd = ηL Edd /c 2 , where η ∼ 0.2 is the binding energy per unit mass at the surface of the neutron star (Syunyaev & Shakura 1986) and L Edd = 4πGM m p c/σ T is the Eddington luminosity of an object with mass, M .…”

Section: Introductionmentioning

confidence: 99%

Beamed emission from a neutron-star ULX in a GRRMHD simulation

Abarca,

Parfrey,

Kluźniak

2021

Preprint

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We perform a global 2.5D general-relativistic radiation magnetohydrodynamic simulation of supercritical accretion onto a neutron star with a 2 × 10 10 G dipolar magnetic field, as a model of a neutronstar-powered ultraluminous X-ray source (ULX). We compute a lower limit on the total luminosity of ∼ 2.5 L Edd , and find the radiation to be highly beamed by the accretion disk outflows. The apparent isotropic luminosity, which is a function of the viewing angle, reaches a maximum above 100 L Edd , consistent with the luminosities observed in ULXs.

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XMM-Newton discovery of transient X-ray pulsar in NGC 1313

Cited by 21 publications

References 43 publications

Discovery of a 2.8 s pulsar in a 2 d orbit High-Mass X-ray Binary powering the Ultraluminous X-ray source ULX-7 in M51

Discovery of a 2.8 s pulsar in a 2 d orbit High-Mass X-ray Binary powering the Ultraluminous X-ray source ULX-7 in M51

Studying magnetic fields of ultraluminous X-ray pulsars using different accretion torques

Beamed emission from a neutron-star ULX in a GRRMHD simulation

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