We develop a Monte Carlo technique based on L.B. Lucy's indivisible photon packets method to calculate X‐ray continuum spectra of Comptonized thermal plasma in arbitrary geometry and apply it to describe the broad‐band X‐ray continuum of the galactic superaccreting microquasar SS433 observed by INTEGRAL. A physical model of the X‐ray emitting region is proposed that includes thermal emission from the accretion disc, jets and hot corona where the photons of different origin are Comptonized. From comparison with INTEGRAL observations, we estimate physical parameters of the complex X‐ray emitting region in SS433 and present model spectra for different viewing angles of the object.
We develop a Monte-Carlo technique based on L.B. Lucy's indivisible photon packets method to calculate X-ray continuum spectra of comptonized thermal plasma in arbitrary geometry and apply it to describe the broadband X-ray continuum of the galactic superaccreting microquasar SS433 observed by INTEGRAL. A physical model of the X-ray emitting region is proposed that includes thermal emission from the accretion disk, jets and hot corona where the photons of different origin are comptonized. From comparison with INTEGRAL observations, we estimate physical parameters of the complex X-ray emitting region in SS433 and present model spectra for different viewing angles of the object.
We investigate the dynamics of a jet collimated by magnetotorsional oscillations. The problem is reduced to an ordinary differential equation containing a singularity and depending on a parameter. We find a parameter range for which this system has stable periodic solutions and study the bifurcations of these solutions. We use Poincaré sections to demonstrate the existence of domains of regular and chaotic motions. We investigate the transition from periodic to chaotic solutions through a sequence of period doublings.Key words: chaos -magnetic fields -MHD -ISM: jets and outflows -ISM: kinematics and dynamics -galaxies: jets. I N T RO D U C T I O NMany quasars and active galactic nuclei are connected with long thin collimated outbursts -jets. When observed with a high angular resolution, these jets show a structure with bright knots separated by relatively dark regions. The mechanism of collimation of such jets is still not clear. Magnetic collimation of jets was first considered by Bisnovatyi-Kogan, Komberg & Fridman (1969). In the paper of Bisnovatyi-Kogan (2007) magnetic collimation resulting from the torsional oscillations of a cylinder with an elongated magnetic field and the periodically distributed initial rotation around the cylinder axis were considered (Fig. 1). The stabilizing azimuthal magnetic field is created here by torsional oscillations. An approximate simplified model was developed, and an ordinary differential equation was derived describing the process of dynamic stabilization. The interval of parameters, for jet stabilization to occur, was estimated qualitatively.The ordinary differential equation under consideration is a nonlinear non-autonomous time-periodic second-order equation with a singularity on the right-hand side. The equation contains a dimensionless parameter D, which summarizes the information about the magnetic field, amplitude and frequency of oscillations, the radius of the jet, its spatial period along the jet axis, and the sound speed in the jet matter. Here we investigate analytically and numerically the structure of the phase space of this equation, which has very peculiar characteristics and contains chaotic solutions as well as quasi-periodic and periodic regular solutions.
Thermal balance of the jet in the source SS433 is considered with account of radiative and adiabatic cooling, and different heating mechanisms. We consider jet heating by the inverse Compton effect of coronal hard X-ray quanta on jet electrons, the influence of shock wave propagation along the jet, and jet kinetic energy transformation into heat via Coulomb collisions of jet and corona protons. The most important heating mechanism for the source SS433 turns out to be Coulomb collisions of jet particles with the surrounding medium.
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