Self-similar solution for the flow behind an exponential shock wave in a rotational axisymmetric non-ideal gas with magnetic field

2019 ◽  
Vol 58 ◽  
pp. 280-293 ◽  
Author(s):  
G. Nath ◽  
P.K. Sahu ◽  
S. Chaurasia
Keyword(s):  
Magnetic Field ◽  
Shock Wave ◽  
Ideal Gas ◽  
Similar Solution ◽  
Self Similar Solution ◽  
Self Similar ◽  
Exponential Shock Wave

New Self Similar Solution of Spherical Radiative Gasdynamic Shock Wave With Increasing Density Under The Effect Of Axial And Azimuthal Magnetic Field

2015 ◽  
Vol 4 (2) ◽  
Author(s):  
Ajay Singh Yadav ◽  
Pravin Kumar Srivastava ◽  
Kishor Kumar Srivastava
Keyword(s):  
Magnetic Field ◽  
Shock Wave ◽  
Magnetic Fields ◽  
Initial Density ◽  
Radiation Energy ◽  
Azimuthal Magnetic Field ◽  
Self Similar Solution ◽  
Complete Study ◽  
Self Similar ◽  
Spherical Shock

In the present chapter we investigated the self similar flow behind a spherical shock wave propagating in a medium with increasing density, in the presence of magnetic fields. The medium is assumed to be non gravitational due to the heavy nucleus at origin. The medium ahead and behind the shock front are assumed to be inviscid. The initial density of gas is assumed to vary as some power of distance. It is assumed that gas is grey and opaque. The assumption of optically thick grey gas is physically consistant with the neglect of radiation pressure and radiation energy. Total energy of the flow field behind the spherical shock is assumed to be increasing with time, where the gas ahead of the shock is assumed to be at rest. The results of numerical calculations were shown in the form of graphs. A complete study was made for axial and azimuthal magnetic field. Also the effect of variation of initial density behind the shock, shock velocity and respective magnetic fields were investigated.

scholarly journals Magnetohydrodynamic Winds Driven by Line Force from the Standard Thin Disk around Supermassive Black Holes: II. A Possible Model for Ultra-fast Outflows in Radio-loud AGNs

2021 ◽  
Vol 922 (2) ◽  
pp. 262
Author(s):  
Xiao-Hong Yang
Keyword(s):  
Magnetic Field ◽  
Numerical Simulations ◽  
Inclination Angle ◽  
Initial Conditions ◽  
Disk Surface ◽  
Similar Solution ◽  
Driving Mechanism ◽  
Self Similar Solution ◽  
Line Force ◽  
Self Similar

Abstract In radio-loud active galactic nuclei (AGNs), ultra-fast outflows (UFOs) were detected at the inclination angle of ∼10°–70° away from jets. Except for the inclination angle of UFOs, the UFOs in radio-loud AGNs have similar properties to that in radio-quiet AGNs. The UFOs with such low inclination cannot be explained in the line-force mechanism. The magnetic-driving mechanism is suggested to explain the UFOs based on a self-similar solution with radiative transfer calculations. However, the energetics of self-similar solution need to be further confirmed based on numerical simulations. To understand the formation and acceleration of UFOs in radio-loud AGNs, this paper presents a model of the disk winds driven by both line force and magnetic field and implements numerical simulations. Initially, a magnetic field is set to 10 times stronger than the gas pressures at the disk surface. Simulation results imply that the disk winds driven by both line force and magnetic field could describe the properties of UFOs in radio-loud AGNs. Pure magnetohydrodynamics (MHDs) simulation is also implemented. When the initial conditions are the same, the hybrid models of magnetic fields and line force are more helpful to form UFOs than the pure MHD models. It is worth studying the case of a stronger magnetic field to confirm this result.

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