Parameter Study in Disk Jet Systems

In the present work we discuss how the strength of magnetic fields determines the characteristics of solutions in models where the collimated outflow and the accretion disk are treated consistently. We perform a complete analysis of the range of magnetic field by non-relativistic 2.5 dimension numerical simulations using the PLUTO code. The main results are that magnetic fields around equipartition with plasma pressure allow steady super-fast-magnetosonic collimated jet solutions; magnetic fields below equipartition correspond to intermittent collimated outflows, while magnetic fields above equipartition lead to sub-alfvenic winds. These results allow to conclude that the configuration proposed by Blandford and Payne to interpret supersonic jets is viable both for equipartition and weaker magnetic fields.