Physics and evolution of constant opening angle jets using a quasi-one-dimensional magnetohydrodynamic model

Details Physics and evolution of constant opening angle jets using a quasi-one-dimensional magnetohydrodynamic model Physics and evolution of constant opening angle jets using a quasi-one-dimensional magnetohydrodynamic model

Apr 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...424..645k&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 424, no. 2, p. 645-665

Computer Science

Numerical Analysis

Active Galactic Nuclei, Astronomical Models, Black Holes (Astronomy), Jet Flow, Magnetic Field Configurations, Magnetohydrodynamic Flow, Neutron Stars, Protostars, Flow Velocity, Gas Pressure, Gravitation, Magnetic Flux, Numerical Analysis, Polytropic Processes, Rotation

Scientific paper

We discuss the significance of the assumptions of infinite conductivity and time independence in the context of an ideal MHD model for constant opening angle jets. The model is developed by projecting the MHD equations onto the jet axis. We find that for initially sub-Alfvenic flows (i.e., flows emanating from active galactic nuclei and neutron stars) wind-type solutions exist only when the field lines at the origin are wound up in a direction opposite to the direction of rotation of the compact source. We discuss the possibility that the time evolution of these outflows may be a cycle between breeze- and wind-type solutions as a result of continuous changes in the boundary conditions at the origin due to accretion. We propose that such cycles may explain the apparent one-sideness of some jets, especially the ones for which we cannot use arguments of relativistic beaming. We examine the dependence of the wind-type solutions on the following parameters describing the outflow at the origin: the degree of winding of the field lines, the value of the gas pressure, the polytropic index, the strength of the magnetic field, the value of the rotational velocity, the gravitational potential of the compact object, and the injection velocity. We compare results with results obtained previously, and discuss briefly the qualitative features and physical interpretation of the solutions for outflows emanating from neutron stars and protostars.

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