Abstract
We explore the effect of large scale magnetic field on the formation of two-component jets in magnetohydrodynamic disk winds simulations. Our simulations show a one-component and two-component jets develop depending on the magnetic field distribution along the surface of the accretion disk. Magnetic field configurations with the least steep gradient along the disk lead to a well defined two-component jet with the self-similar (Blandford-Payne) configuration separating the two regimes. Our results have direct implications to jets models of AGN and GRBs if indeed two-component jets emanate directly from the accretion disk. Our findings imply that a three-component jets may exist in AGN jets if one takes into account a Blandford-Znajek component in the innermost, relativistic, regions.
Highlights
Astrophysical jets are commonly observed in many astrophysical settings involving a central object surrounded by an accretion disk (protostars, active galactic nuclei (AGNs), X-ray binaries, etc)
The role of the magnetic field has been demonstrated in numerical simulations (e.g. [8]) where it was shown that a universal scaling from YSO jets to AGN jets is feasible
The inner edge of the accretion disk surrounding this black hole is at 10rg with rg = 2GM/c2 being the Schwartzschild radius, G is the gravitational constant, M is the mass of the black hole and c is the speed of light
Summary
Astrophysical jets are commonly observed in many astrophysical settings involving a central object surrounded by an accretion disk (protostars, active galactic nuclei (AGNs), X-ray binaries, etc). These jets all have in common the accretion disk threaded by large-scale poloidal field lines. These jets are believed to result from the centrifugal acceleration of disc material by the magnetic field ([1]) which acts as the collimating agent. We highlight and focus on two-component jet solutions found in our simulations, which may be needed to reconcile the unification scheme of BL Lacs and FR I radio galaxies
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