Really focused stellar winds in X-ray binaries

Hadrava, Petr; Čechura, Jan

doi:10.1051/0004-6361/201016046

Cited by 25 publications

(28 citation statements)

References 28 publications

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“…For instance, recent simulations clearly show how the O-star wind can be strongly affected by the dynamics of the gas very near the BH (Hadrava &Čechura 2012;Yoon & Heinz 2014). Additional thermal heating, photoionization, bulk gas motions, clumping, and additonal turbulence likely present in a BH binary system may work to alter outflows.…”

Section: Summary and Future Prospects Formentioning

confidence: 99%

Shell-shocked: the interstellar medium near Cygnus X-1

Sell

Heinz

Richards

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We conduct a detailed case-study of the interstellar shell near the high-mass X-ray binary, Cygnus X-1. We present new WIYN optical spectroscopic and Chandra X-ray observations of this region, which we compare with detailed MAPPINGS III shock models, to investigate the outflow powering the shell. Our analysis places improved, physically motivated constraints on the nature of the shockwave and the interstellar medium (ISM) it is plowing through. We find that the shock is traveling at less than a few hundred km s −1 through a low-density ISM (< 5 cm −3 ). We calculate a robust, 3σ upper limit to the total, time-averaged power needed to drive the shockwave and inflate the bubble, < 2×10 38 erg s −1 . We then review possible origins of the shockwave. We find that a supernova origin to the shockwave is unlikely and that the black hole jet and/or O-star wind can both be central drivers of the shockwave. We conclude that the source of the Cygnus X-1 shockwave is far from solved.

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Section: Summary and Future Prospects Formentioning

confidence: 99%

Shell-shocked: the interstellar medium near Cygnus X-1

Sell

Heinz

Richards

et al. 2014

Monthly Notices of the Royal Astronomical Society

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“…The results presented here were obtained using the secondgeneration radiation-hydrodynamic model of the stellar wind in HMXBs (Hadrava &Čechura 2012). Simulations were conducted on a three-dimensional Cartesian coordinate grid corotating with the modelled components of a binary.…”

Section: Numerical Hydrodynamicsmentioning

confidence: 99%

Stellar wind in state transitions of high-mass X-ray binaries

Čechura

Hadrava

2015

A&A

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Aims. We have developed a new code for the three-dimensional time-dependent raditation hydrodynamic simulation of the stellar wind in interacting binaries to improve models of accretion in high-mass X-ray binaries and to quantitatively clarify the observed variability of these objects. We used the code to test the influence of various parameters on the structure and properties of circumstellar matter. Methods. Our code takes into account acceleration of the wind due to the Roche effective potential, Coriolis force, gas pressure, and (CAK-) radiative pressure in the lines and continuum of the supergiant radiation field that is modulated by its gravity darkening and by the photo-ionization caused by X-ray radiation from the compact companion. The parameters of Cygnus X-1 were used to test the properties of our model. Results. Both two-and three-dimensional numerical simulations show that the Coriolis force substantially influences the mass loss and consequently the accretion rate onto the compact companion. The gravitational field of the compact companion focuses the stellar wind, which leads to the formation of a curved cone-like gaseous tail behind the companion. The changes of X-ray photo-ionization of the wind material during X-ray spectral-state transitions significantly influence the wind structure and offer an explanation of the variability of Cygnus X-1 in optical observations (the Hα emission).

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“…HMXBs represent important laboratories to probe physical processes in extreme conditions of gravity and magnetic fields and to study a large number of fundamental astrophysical questions, such as star formation (Grimm et al 2003;Mineo et al 2012), masses of neutron stars and their equation of state (van der Meer et al 2007;Tomsick & Muterspaugh 2010;Manousakis et al 2012), wind physics (Negueruela 2010) and Finding charts with the identification of the secondary standard stars are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/574/A33 particle acceleration, including supersonic and relativistic fluid dynamics, emission mechanisms, and radiation reprocessing (Hadrava &Čechura 2012;Bosch-Ramon 2013).…”

Section: Introductionmentioning

confidence: 99%

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

Reig

Fabregat

2015

A&A

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We present photometric observations of the field around the optical counterparts of high-mass X-ray binaries. Our aim is to study the long-term photometric variability in correlation with their X-ray activity and derive a set of secondary standard stars that can be used for time series analysis. We find that the donors in Be/X-ray binaries exhibit larger amplitude changes in the magnitudes and colours than those hosting a supergiant companion. The amplitude of variability increases with wavelength in Be/X-ray binaries and remains fairly constant in supergiant systems. When time scales of years are considered, a good correlation between the X-ray and optical variability is observed. The X-rays cease when optical brightness decreases. These results reflect the fact that the circumstellar disk in Be/X-ray binaries is the main source of both optical and X-ray variability. We also derive the colour excess, E(B − V), selecting data at times when the contribution of the circumstellar disk was supposed to be at minimum, and we revisit the distance estimates.

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Really focused stellar winds in X-ray binaries

Cited by 25 publications

References 28 publications

Shell-shocked: the interstellar medium near Cygnus X-1

Shell-shocked: the interstellar medium near Cygnus X-1

Stellar wind in state transitions of high-mass X-ray binaries

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

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