Orbital Decay and Evidence of Disk Formation in the X-Ray Binary Pulsar Oao 1657–415

Jenke, P.; Finger, Mark H.; Wilson-Hodge, C.; Camero-Arranz, A.

doi:10.1088/0004-637x/759/2/124

Cited by 60 publications

(74 citation statements)

References 27 publications

(47 reference statements)

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“…The absorbing column density is ≥ 2 × 10 22 cm −2 . The accretion mode alternates between disk and wind accretion (Jenke et al, 2012). The wind density profile could be constrained by the hard X-ray eclipse profile (Denis et al, 2010).…”

Section: Discussionmentioning

confidence: 99%

High-mass X-ray binaries in the Milky Way

Walter

Lutovinov

Bozzo

et al. 2015

Astron Astrophys Rev

228

234

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High-mass X-ray binaries are fundamental in the study of stellar evolution, nucleosynthesis, structure and evolution of galaxies and accretion processes. Hard X-rays observations by INTEGRAL and Swift have broadened significantly our understanding in particular for the super-giant systems in the Milky Way, which number has increased by almost a factor of three. INTEGRAL played a crucial role in the discovery, study and understanding of heavily obscured systems and of fast X-ray transients. Most super-giant systems can now be classified in three categories: classical/obscured, eccentric and fast transient.The classical systems feature low eccentricity and variability factor of ∼ 10 3 , mostly driven by hydrodynamic phenomena occurring on scales larger than the accretion radius. Among them, systems with short orbital periods and close to Roche-Lobe overflow or with slow winds, appear highly obscured. In eccentric systems, the variability amplitude can reach even higher factors, because of the contrast of the wind density along the orbit. Four super-giant systems, featuring fast outbursts, very short orbital periods and anomalously low accretion rates, are not yet understood.Simulations of the accretion processes on relatively large scales have progressed and reproduce parts of the observations. The combined effects of wind

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Section: Discussionmentioning

confidence: 99%

High-mass X-ray binaries in the Milky Way

Walter

Lutovinov

Bozzo

et al. 2015

Astron Astrophys Rev

228

234

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“…Additional simulations presented by also showed that a more erratic or periodic behaviour of the flares can be obtained by assuming different properties of the poorly known density and velocity asymmetry of the accretion flow. The presence of short-lived accretion discs in SFXTs (and other NS HMXBs in general) could be tested observationally through the detection of rapid spin-up phases (Klochkov et al 2011;Jenke et al 2012). However, IGR J17544−2619 has not displayed convincing evidence of pulsations in the past (see Sect.…”

Section: Discussionmentioning

confidence: 99%

Giant outburst from the supergiant fast X-ray transient IGR J17544−2619: accretion from a transient disc?

Romano

Bozzo

Mangano

et al. 2015

A&A

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Supergiant fast X-ray transients (SFXTs) are high mass X-ray binaries associated with OB supergiant companions and characterized by an X-ray flaring behaviour whose dynamical range reaches 5 orders of magnitude on time scales of a few hundred to thousands of seconds. Current investigations concentrate on finding possible mechanisms to inhibit accretion in SFXTs and to explain their unusually low average X-ray luminosity. We present the Swift observations of an exceptionally bright outburst displayed by the SFXT IGR J17544−2619 on 2014 October 10 when the source achieved a peak luminosity of 3 × 10 38 erg s −1 . This extends the total source dynamic range to > ∼ 10 6 , the largest (by a factor of 10) recorded so far from an SFXT. Tentative evidence for pulsations at a period of 11.6 s is also reported. We show that these observations challenge, for the first time, the maximum theoretical luminosity achievable by an SFXT and propose that this giant outburst was due to the formation of a transient accretion disc around the compact object.

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“…We added a set of harmonically-related sinusoids (WAVE parameters in Tempo2) to obtain a model with nearly white residuals. The results of the coherent timing analysis are summarized in Table 2. A search for pulsations was performed in the direction of RX J0209.6−7427 in GBM data around the NICER frequency in the manner described in Finger et al (1999) and Jenke et al (2012). Specifically we used CTIME data products.…”

Section: Temporal Propertiesmentioning

confidence: 99%

The 2019 super-Eddington outburst of RX J0209.6−7427: detection of pulsations and constraints on the magnetic field strength

Vasilopoulos

Ray

Gendreau

et al. 2020

Monthly Notices of the Royal Astronomical Society

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In November 2019, MAXI detected an X-ray outburst from the known Be X-ray binary system RX J0209.6−7427 located in the outer wing of the Small Magellanic Cloud. We followed the outburst of the system with NICER which led to the discovery of X-ray pulsations with a period of 9.3 s. We analyzed simultaneous X-ray data obtained with NuSTAR and NICER allowing us to characterize the spectrum and provide an accurate estimate of its bolometric luminosity. During the outburst the maximum broadband X-ray luminosity of the system reached 1-2×10 39 erg s −1 , thus exceeding by about one order of magnitude the Eddington limit for a typical 1.4 M ⊙ mass neutron star (NS). Monitoring observations with Fermi/GBM and NICER allowed us to study the spin evolution of the NS and compare it with standard accretion torque models. We found that the NS magnetic field should be of the order of 3×10 12 G. We conclude that RX J0209.6−7427 exhibited one of the brightest outbursts observed from a Be X-ray binary pulsar in the Magellanic Clouds, reaching similar luminosity level to the 2016 outburst of SMC X-3. Despite the super-Eddington luminosity of RX J0209.6−7427, the NS appears to have only a moderate magnetic field strength.

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Orbital Decay and Evidence of Disk Formation in the X-Ray Binary Pulsar Oao 1657–415

Cited by 60 publications

References 27 publications

High-mass X-ray binaries in the Milky Way

High-mass X-ray binaries in the Milky Way

Giant outburst from the supergiant fast X-ray transient IGR J17544−2619: accretion from a transient disc?

The 2019 super-Eddington outburst of RX J0209.6−7427: detection of pulsations and constraints on the magnetic field strength

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