An evolving jet from a strongly magnetized accreting X-ray pulsar

Eijnden, J. van den; Degenaar, N.; Russell, Thomas; Wijnands, Rudy; Miller-Jones, J. C. A.; Sivakoff, G. R.; Santisteban, J. V. Hernández

doi:10.1038/s41586-018-0524-1

Cited by 74 publications

(64 citation statements)

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“…For the two uncompressed magnetic field models, i.e., the GL model and r m1 in the SZL model, the distance has a similar value and agrees with the lower limit of 5.0 kpc at 99% confidence level given by van den Eijnden et al (2018). The magnetic field strength in the latter model is higher than the former one by a factor of 2, and they both are in line with conclusions by Doroshenko et al (2018) and Tsygankov et al (2018), who suggested ∼10 13 G. On the other hand, results of compressed models of r m2 and r m3 in the SZL model show much shorter distance than the uncompressed models, which appear to be at odds with the Gaia distance estimate. The magnetic field strength of r m2 is close to the uncompressed models, but for r m3 , it is much weaker.…”

Section: Fitting Resultssupporting

confidence: 88%

“…The broadband spectra (2-150 keV) of the source can be described with a cutoff power-law continuum with an additional soft blackbody component and a gaussian profile. We found that variations of the pulsed flux fraction with time are different in the three energy bands, which are likely related to changing patterns of the pulse profile reported in Tsygankov et al (2018) and associated with the onset of accretion column. No evidence is found for cyclotron line in the spectra of Insight-HXMT; perhaps there is no cyclotron resonant scattering process during this outburst, or it occurs at an energy higher than the maximum energy range of Insight-HXMT.…”

Section: Discussion and Summarymentioning

confidence: 75%

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Insight-HXMT Observations of Swift J0243.6+6124 during Its 2017–2018 Outburst

Zhang

Song

et al. 2019

ApJ

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The recently discovered neutron star transient Swift J0243.6+6124 has been monitored by the Hard X-ray Modulation Telescope. Based on the obtained data, we investigate the broadband spectrum of the source throughout the outburst. We estimate the broadband flux of the source and search for possible cyclotron line in the broadband spectrum. However, no evidence of line-like features is found up to 150 keV. In the absence of any cyclotron line in its energy spectrum, we estimate the magnetic field of the source based on the observed spin evolution of the neutron star by applying two accretion torque models. In both cases, we get consistent results with B∼10 13 G, D∼6 kpc and peak luminosity of >10 39 erg s −1 , which makes the source the first Galactic ultraluminous X-ray source hosting a neutron star.

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Section: Fitting Resultssupporting

confidence: 88%

Section: Discussion and Summarymentioning

confidence: 75%

Insight-HXMT Observations of Swift J0243.6+6124 during Its 2017–2018 Outburst

Zhang

Song

et al. 2019

ApJ

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“…It is important to note that this pulsar launched a jet when the X-ray luminosity was ≥4×10 36 erg s −1 during giant and fainter outbursts (for a distance of 7 kpc; van den Eijnden et al 2018Eijnden et al , 2019. At the same time, the luminositydependent emission lines were observed in the spectral range of NICER.…”

Section: Discussionmentioning

confidence: 76%

“…We also explored the correlation between Fe-line emission and the radio flux density as observed with VLA ( Figure 6). The radio data used here are taken from van den Eijnden et al (2018) and van den Eijnden et al (2019). The VLA observations were quasi-simultaneous to NICER pointings (Ob-sID 1050390105, 1050390116, 1050390118, 1050390122, 1050390134, and 1050390143) between 2017 October and 2018 February.…”

Section: Evolution Of Iron Linesmentioning

confidence: 99%

An Evolving Broad Iron Line from the First Galactic Ultraluminous X-Ray Pulsar Swift J0243.6+6124

Jaisawal

Wilson-Hodge

Fabian

et al. 2019

ApJ

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We present a spectral study of the ultraluminous Be/X-ray transient pulsar Swift J0243.6+6124 using Neutron Star Interior Composition Explorer (NICER) observations during the system's 2017-2018 giant outburst. The 1.2-10 keV energy spectrum of the source can be approximated with an absorbed cut-off power law model. We detect strong, luminosity-dependent emission lines in the 6-7 keV energy range. A narrow 6.42 keV line, observed in the sub-Eddington regime, is seen to evolve into a broad Fe-line profile in the super-Eddington regime. Other features are found at 6.67 and 6.97 keV in the Fe-line complex. An asymmetric broad line profile, peaking at 6.67 keV, is possibly due to Doppler effects and gravitational redshift. The 1.2-79 keV broadband spectrum from NuSTAR and NICER observations at the outburst peak is well described by an absorbed cut-off power law plus multiple Gaussian lines and a blackbody component. Physical reflection models are also tested to probe the broad iron line feature. Depending on the mass accretion rate, we found emission sites that are evolving from ∼5000 km to a range closer to the surface of the neutron star. Our findings are discussed in the framework of the accretion disk and its implication on the magnetic field, the presence of optically thick accretion curtain in the magnetosphere, jet emission, and the massive, ultra-fast outflow expected at super-Eddington accretion rates. We do not detect any signatures of a cyclotron absorption line in the NICER or NuSTAR data.

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“…Kaaret et al 2003;Webb et al 2012;Mezcua et al 2013). Winds have been seen through X-ray (Pinto et al 2016) and optical (Zepf et al 2008) spectroscopy of several targets, including one ULX pulsar (NGC 300 ULX-1; Kosec et al 2018a). However, the extragalactic nature of ULXs complicates the study of their outflows.…”

Section: Introductionmentioning

confidence: 99%

Chandra reveals a possible ultrafast outflow in the super-Eddington Be/X-ray binary Swift J0243.6+6124

Eijnden

Degenaar

Schulz

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Accretion at super-Eddington rates is expected to be accompanied by strong outflows. Such outflows are observed in Galactic X-ray binaries and extragalactic Ultra-luminous X-ray sources (ULXs). However, due to their large source distances, ULX outflows are challenging to detect and study in detail. Galactic neutron stars accreting from a Be-star companion at super-Eddington rates show many similarities to ULX pulsars, and therefore offer an alternative approach to study outflows in this accretion regime. Here, we present Chandra high-resolution spectroscopy of such a super-Eddington accreting neutron star, Swift J0243.6+6124, to search for wind outflow signatures during the peak of its 2017/2018 giant outburst. We detect narrow emission features at rest from Ne, Mg, S, Si, and Fe. In addition, we detect a collection of absorption features which can be identified in two ways: either as all Fe transitions at rest (with a possible contribution from Mg), or a combination of three blue-shifted Ne and Mg lines at ∼ 0.22c, while the remaining lines are at rest. The second scenario would imply an outflow with a velocity similar to those seen in ULXs, including the ULX pulsar NGC 300 ULX-1. This result would also imply that Swift J0243.6+6124 launches both a jet, detected in radio and reported previously, and an ultra-fast wind outflow simultaneously at super-Eddington accretion rates.

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An evolving jet from a strongly magnetized accreting X-ray pulsar

Cited by 74 publications

References 50 publications

Insight-HXMT Observations of Swift J0243.6+6124 during Its 2017–2018 Outburst

Insight-HXMT Observations of Swift J0243.6+6124 during Its 2017–2018 Outburst

An Evolving Broad Iron Line from the First Galactic Ultraluminous X-Ray Pulsar Swift J0243.6+6124

Chandra reveals a possible ultrafast outflow in the super-Eddington Be/X-ray binary Swift J0243.6+6124

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