Luminosity dependence of the cyclotron line and evidence for the accretion regime transition in V 0332+53

Doroshenko, V.; Tsygankov, Sergey S.; Mushtukov, Alexander A.; Lutovinov, A.; Santangelo, A.; Suleimanov, V.; Poutanen, Juri

doi:10.1093/mnras/stw3236

Cited by 88 publications

(107 citation statements)

References 40 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Therefore, observational constraint of L * can be used to obtain independent estimates of the magnetic field. It is worth to note here that observational evidence of a transition through the critical luminosity was recently found in the classical XRP V 0332+53 (Doroshenko et al 2017).…”

Section: Critical and Maximal Luminositiesmentioning

confidence: 65%

SMC X-3: the closest ultraluminous X-ray source powered by a neutron star with non-dipole magnetic field

Tsygankov

Doroshenko

Lutovinov

et al. 2017

A&A

View full text Add to dashboard Cite

Aims. Magnetic field of accreting neutron stars determines their overall behavior including the maximum possible luminosity. Some models require an above-average magnetic field strength ( 10 13 G) in order to explain super-Eddington mass accretion rate in the recently discovered class of pulsating ultraluminous X-ray sources (ULX). The peak luminosity of SMC X-3 during its major outburst in 2016-2017 reached ∼ 2.5 × 10 39 erg s −1 comparable to that in ULXs thus making this source the nearest ULX-pulsar. Determination of the magnetic field of SMC X-3 is the main goal of this paper. Methods. SMC X-3 belongs to the class of transient X-ray pulsars with Be optical companions, and exhibited a giant outburst in July 2016 -March 2017. The source has been observed during the entire outburst with the Swift/XRT and Fermi/GBM telescopes, as well as the NuSTAR observatory. Collected data allowed us to estimate the magnetic field strength of the neutron star in SMC X-3 using several independent methods. Results. Spin evolution of the source during and between the outbursts and the luminosity of the transition to so-called propeller regime in the range of (0.3 − 7) × 10 35 erg s −1 imply relatively weak dipole field of (1 − 5) × 10 12 G. On the other hand, there is also evidence for much stronger field in the immediate vicinity of the neutron star surface. In particular, transition from super-to subcritical accretion regime associated with cease of the accretion column and very high peak luminosity favor an order of magnitude stronger field. This discrepancy makes SMC X-3 a good candidate to posses significant non-dipolar components of the field, and an intermediate source between classical X-ray pulsars and accreting magnetars which may constitute an appreciable fraction of ULX population.

show abstract

Section: Critical and Maximal Luminositiesmentioning

confidence: 65%

SMC X-3: the closest ultraluminous X-ray source powered by a neutron star with non-dipole magnetic field

Tsygankov

Doroshenko

Lutovinov

et al. 2017

A&A

View full text Add to dashboard Cite

show abstract

“…(Klochkov et al 2011;Sartore et al 2015), Vela X-1 (Fürst et al 2014), GX 304−1 , and Cep X-4 (Vybornov et al (2017). A possible additional source is V0332+53 at low luminosity towards the end of an outburst (Doroshenko et al 2016). At very high luminosity, this object is a good example of a negative E cyc -L correlation (Mowlavi et al 2006;Tsygankov et al 2010;Cusumano et al 2016;Doroshenko et al 2016).…”

Section: Introductionmentioning

confidence: 97%

“…At very high luminosity, this object is a good example of a negative E cyc -L correlation (Mowlavi et al 2006;Tsygankov et al 2010;Cusumano et al 2016;Doroshenko et al 2016). With regard to the long-term variation in E cyc , there are now three additional candidates: a decay in Vela X-1 (La ), a decay in V0332+53 during an outburst Doroshenko et al 2016), and a possible increase in 4U 1538−522 . In this Letter we present the results of new observations of Her X-1 in 2016 of the energy of the cyclotron resonance scattering feature in the pulse averaged X-ray spectrum of Her X-1: the CRSF energy has apparently stopped its 20-year decay and has started to increase again.…”

Section: Introductionmentioning

confidence: 99%

“…A possible additional source is V0332+53 at low luminosity towards the end of an outburst (Doroshenko et al 2016). At very high luminosity, this object is a good example of a negative E cyc -L correlation (Mowlavi et al 2006;Tsygankov et al 2010;Cusumano et al 2016;Doroshenko et al 2016). With regard to the long-term variation in E cyc , there are now three additional candidates: a decay in Vela X-1 (La ), a decay in V0332+53 during an outburst Doroshenko et al 2016), and a possible increase in 4U 1538−522 .…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Inversion of the decay of the cyclotron line energy in Hercules X-1

Staubert

Klochkov

Fürst

et al. 2017

A&A

View full text Add to dashboard Cite

Recent observations of Her X-1 with NuSTAR and INTEGRAL in 2016 have provided evidence that the 20-year decay of the cyclotron line energy found between 1996 and 2015 has ended and that an inversion with a new increase, possibly similar to the one observed around 1990-1993, has started. We consider this a strong motivation for further observations and for enhanced efforts to significantly improve our theoretical understanding of the accretion process in binary X-ray pulsars. We speculate about the physics behind the long-term decay and its inversion, a possible cyclic behavior, and correlations with other variable observables.

show abstract

“…Her X-1: Staubert et al (2007); GX 304-1: Yamamoto et al (2011); Cep X-4: Fürst et al (2015)) or negative (e.g. V 0332+53; Doroshenko et al (2017)). Long term variation of the energy of the cyclotron line has also been observed in two sources, namely Her X-1 (Ji et al 2019;Staubert et al 2017), and Vela X-1 (Fürst et al 2014;Ji et al 2019).…”

Section: Introductionmentioning

confidence: 99%

Possible detection of a new cyclotron feature in 4U 1700–37

Bala

Roy

Bhattacharya

2020

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We present a spectral and timing study of the High Mass X-ray Binary transient source 4U 1700-37 using NuSTAR and ASTROSAT/LAXPC. The source is observed in two different flux states. A combined spectral analysis of NuSTAR's FPMA and FPMB shows the possible hint of a cyclotron line feature at ∼16 keV. The line feature is consistently present in different continuum models with at least 3σ confidence level. We do not detect the presence of a previously reported 39 keV cyclotron line in the combined spectra. A ∼16 keV cyclotron feature would suggest that the compact object is a neutron star with a magnetic field strength ∼ 2.1×10 12 Gauss in the emission region. We also find the presence of a rare Ni Kα emission line around 7.6 keV in the NuSTAR spectrum. We searched the NuSTAR and ASTROSAT data for coherent or quasi-periodic oscillation signals but found no evidence in the frequency range 0.1 mHz to 10 3 Hz.

show abstract

Luminosity dependence of the cyclotron line and evidence for the accretion regime transition in V 0332+53

Cited by 88 publications

References 40 publications

SMC X-3: the closest ultraluminous X-ray source powered by a neutron star with non-dipole magnetic field

SMC X-3: the closest ultraluminous X-ray source powered by a neutron star with non-dipole magnetic field

Inversion of the decay of the cyclotron line energy in Hercules X-1

Possible detection of a new cyclotron feature in 4U 1700–37

Contact Info

Product

Resources

About