Strong outburst activity of the X-ray pulsar X Persei during 2001-2011

Lutovinov, A.; Tsygankov, Sergey S.; Chernyakova, M.

doi:10.1111/j.1365-2966.2012.21036.x

Cited by 61 publications

(58 citation statements)

References 37 publications

(84 reference statements)

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“…In the X Persei spectrum there is also a strong absorption feature near the energy of ≃ 30 keV. It was discovered by Coburn et al (2001) based on the RXTE data and interpreted as a cyclotron resonance scattering feature, that allowed to estimate a magnetic field on the neutron star surface B N S ≃ (2.4 − 2.9) × 10 12 G, (Lutovinov et al, 2012a). This line was found to be significantly broader than is typically observed in X-ray pulsars (Coburn et al, 2002), that allowed other authors interpreted it as an artificial deficit of photons in the region where the different spectral components overlap Doroshenko et al, 2012b).…”

Section: Discussionmentioning

confidence: 99%

“…Delgado-Martí et al (2001) succeeded in determining orbital parameters for X Persei and showed that it is in a moderately eccentric orbit (e ≃ 0.11) with a very long P orb ≃ 250 days orbital period. Deep observations performed with the INTEGRAL observatory allowed to detect the hard X-ray emission from X Persei up to ≃ 160 keV (Doroshenko et al, 2012b;Lutovinov et al, 2012a), that is non-typical for X-ray pulsars. In the X Persei spectrum there is also a strong absorption feature near the energy of ≃ 30 keV.…”

Section: Discussionmentioning

confidence: 99%

“…A distance to the source is estimated by different authors in the range of 700 to 1300 pc, but more often the value of 950 ± 200 pc is used (Telting et al, 1998). Adopting this distance the source peak luminosity L X ≃ 2 × 10 35 erg s 2010 (Lutovinov et al, 2012a). Delgado-Martí et al (2001) succeeded in determining orbital parameters for X Persei and showed that it is in a moderately eccentric orbit (e ≃ 0.11) with a very long P orb ≃ 250 days orbital period.…”

Section: Discussionmentioning

confidence: 99%

“…INTEGRAL detected very hard spectra in some of these systems. In particular, X Persei and RX J0440.9+4431 were detected significantly up to ∼ 160 keV (Doroshenko et al, 2012b;Lutovinov et al, 2012a) and ∼ 120 keV , respectively. Broadband spectra of both sources are shown in Fig.…”

Section: Be Systems X-ray Pulsars and Properties Of Cyclotron Absorpmentioning

confidence: 99%

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High-mass X-ray binaries in the Milky Way

Walter

Lutovinov

Bozzo

et al. 2015

Astron Astrophys Rev

230

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%

Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Section: Be Systems X-ray Pulsars and Properties Of Cyclotron Absorpmentioning

confidence: 99%

See 2 more Smart Citations

High-mass X-ray binaries in the Milky Way

Walter

Lutovinov

Bozzo

et al. 2015

Astron Astrophys Rev

230

234

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“…X Per does not show the typical Type I or II X-ray outbursts, but shows extended periods of low and high X-ray activity. The lack of a correlation A122, page 13 of 31 between optical and X-ray flux in X Per has been reported before (Lutovinov et al 2012;Li et al 2014).…”

Section: Circumstellar Disk and X-ray Variabilitymentioning

confidence: 99%

Long-term optical variability of high-mass X-ray binaries

Reig

Nersesian

Zezas

et al. 2016

A&A

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Context. High-mass X-ray binaries are bright X-ray sources. The high-energy emission is caused by the accretion of matter from the massive companion onto a neutron star. The accreting material comes from either the strong stellar wind in binaries with supergiant companions or the cirscumstellar disk in Be/X-ray binaries. In either case, the Hα line stands out as the main source of information about the state of the accreting material. Aims. We present the results of our monitoring program to study the long-term variability of the Hα line in high-mass X-ray binaries. Our aim is to characterise the optical variability timescales and study the interaction between the neutron star and the accreting material. Methods. We fitted the Hα line with Gaussian profiles and obtained the line parameters and equivalent width. The peak separation in split profiles was used to determine the disk velocity law and estimate the disk radius. The relative intensity of the two peaks (V/R ratio) allowed us to investigate the distribution of gas particles in the disk. The equivalent width was used to characterise the degree of variability of the systems. We also studied the variability of the Hα line in correlation with the X-ray activity. Results. Our results can be summarised as follows: i) we find that Be/X-ray binaries with narrow orbits are more variable than systems with long orbital periods; ii) we show that a Keplerian distribution of gas particles provides a good description of the disks in Be/X-ray binaries, as it does in classical Be stars; iii) a decrease in the Hα equivalent width is generally observed after major X-ray outbursts; iv) we confirm that the Hα equivalent width correlates with disk radius; v) while systems with supergiant companions display multistructured profiles, most of the Be/X-ray binaries show, at some epoch, double-peak asymmetric profiles, which indicates that density inhomogeneities is a common property in the disk of Be/X-ray binaries; vi) the profile variability (V/R ratio) timescales are shorter and the Hα equivalent widths are smaller in Be/X-ray binaries than in isolated Be stars; and vii) we provide new evidence that the disk in Be/X-ray binaries is, on average, denser than in classical Be stars. Conclusions. We carried out the most complete optical spectroscopic study of the global properties of high-mass X-ray binaries with the analysis of more than 1100 spectra from 20 sources. Our results provide further evidence for the truncation of the disk in Be/X-ray binaries. We conclude that the interaction between the compact object and the Be-type star works in two directions: the massive companion provides the source of matter for accretion, affecting the surroundings of the compact object, and the continuous revolution of the neutron star around the optical counterpart also produces the truncation of the Be star's equatorial disk.

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Disability Education at Lady Irwin College, University of Delhi

Sharma

2020

Disability Studies in India

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In this article, we introduce and study Riesz bases in a separable quaternionic Hilbert spaces. Some results on Riesz bases in a separable quaternionic Hilbert spaces are proved. It is also proved that a Riesz basis in a separable quaternionic Hilbert space a frame for the quaternionic Hilbert space. Riesz sequences are defined and equivalence of a Riesz basis and a complete Riesz sequence in a separable quaternionic Hilbert space is proved. 2010 Mathematics Subject Classification. 42C15, 42A38.

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Strong outburst activity of the X-ray pulsar X Persei during 2001-2011

Cited by 61 publications

References 37 publications

High-mass X-ray binaries in the Milky Way

High-mass X-ray binaries in the Milky Way

Long-term optical variability of high-mass X-ray binaries

Disability Education at Lady Irwin College, University of Delhi

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