scholarly journals Orbital phase spectroscopy of four high mass X-ray binary pulsars to study the stellar wind of the companion

2009 ◽  
Vol 43 (6) ◽  
pp. 900-904 ◽  
Author(s):  
Sachindra Naik ◽  
U. Mukherjee ◽  
B. Paul ◽  
C.S. Choi
Keyword(s):  
Stellar Wind ◽  
High Mass ◽  
X Ray ◽  
Binary Pulsars ◽  
Orbital Phase

scholarly journals X-Ray Spectroscopy of the High-Mass X-Ray Binary 4U 1700-37

2004 ◽  
Vol 194 ◽  
pp. 213-213
Author(s):  
A. van der Meer ◽  
L. Kaper ◽  
T. Di Salvo ◽  
M. Méndez ◽  
M. van der Klis
Keyword(s):  
Binary System ◽  
Stellar Wind ◽  
High Mass ◽  
X Ray ◽  
Monitoring Campaign ◽  
Pile Up ◽  
First Results ◽  
Orbital Phase

We present the first results of a monitoring campaign of the high-mass X-ray binary system 4U 1700-37/HD 153919, carried out with XMM-Newton.We have observed the high-mass X-ray binary (HMXB) 4U 1700-37 with XMM-Newton at four orbital phases in February 2001. 4U 1700-37 is powered by the dense stellar wind of the O supergiant HD 153919. Numerous X-ray flares are observed with a typical duration, of the order of half an hour. We focus on three intervals in which the data are not affected by pile up: the eclipse, the eclipse egress and a low-flux part around orbital phase ϕ ~ 0.28.

scholarly journals On the origin of Supergiant Fast X-ray Transients

2018 ◽  
Vol 14 (S346) ◽  
pp. 193-196
Author(s):  
Swetlana Hubrig ◽  
Lara Sidoli ◽  
Konstantin A. Postnov ◽  
Markus Schöller ◽  
Alexander F. Kholtygin ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Neutron Star ◽  
Stellar Wind ◽  
Longitudinal Magnetic Field ◽  
High Mass ◽  
Large Telescope ◽  
X Ray ◽  
Very Large Telescope ◽  
Low X ◽  
X Ray Binaries

Abstract. A fraction of high-mass X-ray binaries are supergiant fast X-ray transients. These systems have on average low X-ray luminosities, but display short flares during which their X-ray luminosity rises by a few orders of magnitude. The leading model for the physics governing this X-ray behaviour suggests that the winds of the donor OB supergiants are magnetized. In agreement with this model, the first spectropolarimetric observations of the SFXT IGR J11215-5952 using the FORS 2 instrument at the Very Large Telescope indicate the presence of a kG longitudinal magnetic field. Based on these results, it seems possible that the key difference between supergiant fast X-ray transients and other high-mass X-ray binaries are the properties of the supergiant’s stellar wind and the physics of the wind’s interaction with the neutron star magnetosphere.

scholarly journals Color–color diagrams as tools for assessment of the variable absorption in high mass X-ray binaries

2020 ◽  
Vol 643 ◽  
pp. A109
Author(s):  
V. Grinberg ◽  
M. A. Nowak ◽  
N. Hell
Keyword(s):  
Stellar Wind ◽  
Binary Systems ◽  
Compact Object ◽  
Spectral Shape ◽  
High Mass ◽  
Line Of Sight ◽  
Current Generation ◽  
X Ray ◽  
Partial Covering ◽  
X Ray Binaries

High mass X-ray binaries hold the promise of allowing us to understand the structure of the winds of their supermassive companion stars by using the emission from the compact object as a backlight to evaluate the variable absorption in the structured stellar wind. The wind along the line of sight can change on timescales as short as minutes and below. However, such short timescales are not available for the direct measurement of absorption through X-ray spectroscopy with the current generation of X-ray telescopes. In this paper, we demonstrate the usability of color–color diagrams for assessing the variable absorption in wind accreting high mass X-ray binary systems. We employ partial covering models to describe the spectral shape of high mass X-ray binaries and assess the implication of different absorbers and their variability on the shape of color–color tracks. We show that in taking into account, the ionization of the absorber, and in particular accounting for the variation of ionization with absorption depth, is crucial to describe the observed behavior well.

scholarly journals Supergiant fast X-ray transients versus classical supergiant high mass X-ray binaries: Does the difference lie in the companion wind?

2018 ◽  
Vol 610 ◽  
pp. A50 ◽  
Author(s):  
P. Pradhan ◽  
E. Bozzo ◽  
B. Paul
Keyword(s):  
Stellar Wind ◽  
Equivalent Width ◽  
High Mass ◽  
Stellar Winds ◽  
Data Set ◽  
Iron Line ◽  
X Ray ◽  
Eclipse Observations ◽  
The Difference ◽  
X Ray Binaries

We present a comparative study of stellar winds in classical supergiant high mass X-ray binaries (SgXBs) and supergiant fast X-ray transients (SFXTs) based on the analysis of publicly available out-of-eclipse observations performed with Suzaku and XMM-Newton. Our data set includes 55 observations of classical SgXBs and 21 observations of SFXTs. We found that classical SgXBs are characterized by a systematically higher absorption and luminosity compared to the SFXTs, confirming the results of previous works in the literature. Additionally, we show that the equivalent width of the fluorescence Kα iron line in the classical SgXBs is significantly larger than that of the SFXTs (outside X-ray eclipses). Based on our current understanding of the physics of accretion in these systems, we conclude that the most likely explanation of these differences is ascribed to the presence of mechanisms inhibiting accretion most of the time in SFXTs, thereby leading to a much less efficient photoionization of the stellar wind compared to classical SgXBs. We do not find evidence for the previously reported anticorrelation between the equivalent width of the fluorescence iron line and the luminosity of SgXBs.

scholarly journals SALT observations of the supernova remnant MCSNR J0127−7332 and its associated Be X-ray binary SXP 1062 in the SMC

2021 ◽  
Vol 503 (3) ◽  
pp. 3856-3866
Author(s):  
V V Gvaramadze ◽  
A Y Kniazev ◽  
J S Gallagher ◽  
L M Oskinova ◽  
Y-H Chu ◽  
...  
Keyword(s):  
Neutron Star ◽  
Emission Line ◽  
Supernova Remnant ◽  
Supernova Explosion ◽  
High Mass ◽  
Expansion Velocity ◽  
X Ray ◽  
Orbital Phase ◽  
Be Star ◽  
The Moment

ABSTRACT We report the results of optical spectroscopy of the Small Magellanic Cloud supernova remnant (SNR) MCSNR J0127−7332 and the mass donor Be star, 2dFS 3831, in its associated high-mass X-ray binary SXP 1062 carried out with the Southern African Large Telescope. Using high-resolution long-slit spectra, we measured the expansion velocity of the SNR shell of ${\approx} 140 \, {\rm \, km\, s^{-1}}$, indicating that MCSNR J0127−7332 is in the radiative phase. We found that the observed line ratios in the SNR spectrum can be understood if the local interstellar medium is ionized by 2dFS 3831 and/or OB stars around the SNR. We propose that MCSNR J0127−7332 is the result of supernova explosion within a bubble produced by the stellar wind of the supernova progenitor and that the bubble was surrounded by a massive shell at the moment of supernova explosion. We estimated the age of MCSNR J0127−7332 to be ${\lesssim} 10\, 000$ yr. We found that the spectrum of 2dFS 3831 changes with orbital phase. Namely, the equivalent width of the H α emission line decreased by ≈40 per cent in ≈130 d after periastron passage of the neutron star and then almost returned to its original value in the next ≈100 d. Also, the spectrum of 2dFS 3831 obtained closest to the periastron epoch (about 3 weeks after the periastron) shows a noticeable emission line of He ii λ4686, which disappeared in the next 2 weeks. We interpret these changes as a result of the temporary perturbation and heating of the disc as the neutron star passes through it.

scholarly journals Spectroscopy of the Stellar Wind in the Cygnus X-1 System

10.14311/1332 ◽  
2011 ◽  
Vol 51 (1) ◽  
Author(s):  
I. Miškovičová ◽  
M. Hanke ◽  
J. Wilms ◽  
M. A. Nowak ◽  
K. Pottschmidt ◽  
...  
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Binary System ◽  
Stellar Wind ◽  
Roche Lobe ◽  
High Mass ◽  
Lagrange Point ◽  
Companion Star ◽  
X Ray ◽  
Accretion Flow

The X-ray luminosity of black holes is produced through the accretion of material from their companion stars. Depending on the mass of the donor star, accretion of the material falling onto the black hole through the inner Lagrange point of the system or accretion by the strong stellar wind can occur. Cygnus X-1 is a high mass X-ray binary system, where the black hole is powered by accretion of the stellar wind of its supergiant companion star HDE226868. As the companion is close to filling its Roche lobe, the wind is not symmetric, but strongly focused towards the black hole. Chandra-HETGS observations allow for an investigation of this focused stellar wind, which is essential to understand the physics of the accretion flow. We compare observations at the distinct orbital phases of 0.0, 0.2, 0.5 and 0.75. These correspond to different lines of sight towards the source, allowing us to probe the structure and the dynamics of the wind.

scholarly journals Investigating a unique partial eclipse in the high-mass X-ray binary IGR J16393−4643 with Swift-XRT

2019 ◽  
Vol 491 (1) ◽  
pp. 1491-1497 ◽  
Author(s):  
Sanhita Kabiraj ◽  
Nazma Islam ◽  
Biswajit Paul
Keyword(s):  
Inclination Angle ◽  
High Mass ◽  
Spectral Parameters ◽  
X Ray ◽  
Low Intensity ◽  
Orbital Phase

ABSTRACT The orbital profile of the high-mass X-ray binary IGR J16393−4643 shows a dip in its X-ray intensity, which was previously interpreted as an eclipse. Unlike most eclipsing HMXBs, where the X-ray eclipses are about two orders of magnitude fainter compared to the out-of-eclipse emission, this particular eclipse-like feature is narrow and partial, casting doubt if it is indeed an eclipse. To further investigate the nature of this low-intensity orbital phase, we use a large number of observations with Swift-XRT, covering the entire orbital phase. The soft X-ray observations also show this low-intensity phase, which is about 30 % of the intensity during rest of the orbit. We also carried out orbital-phase-resolved spectroscopy to compare the change in the spectral parameters inside and outside of this low-intensity state. The results indicate that this low-intensity state might not be an eclipse, as previously thought but absorption in the stellar corona. We have also provided the inclination angle of the binary for grazing eclipse caused by the stellar corona.

scholarly journals Stellar winds in high-mass X-ray binaries

1995 ◽  
Vol 163 ◽  
pp. 271-279
Author(s):  
Lex Kaper
Keyword(s):  
Stellar Wind ◽  
Large Scale ◽  
Binary Systems ◽  
Compact Object ◽  
High Mass ◽  
X Rays ◽  
Ionization Zone ◽  
X Ray ◽  
Massive Binary Systems ◽  
X Ray Binaries

High-mass X-ray binaries (HMXBs) represent an important stage in the evolution of massive binary systems. The compact object (in most cases an X-ray pulsar) not only provides information on the orbital and stellar parameters, but also probes the stellar wind of the massive companion, an OB supergiant or Be star. The X-ray luminosity directly depends on the density and the velocity of the wind at the orbit of the X-ray source. Important constraints on the stellar-wind structure can be set by studying the orbital modulation of UV P-Cygni profiles. In this paper different aspects of the interactive wind-accretion process are highlighted, such as the highly variable X-ray luminosity, the influence of the X-rays on the radiative acceleration of the wind inside the ionization zone, and the large-scale structures that trail the X-ray source in its orbit.

Sign in / Sign up

Export Citation Format

Share Document