The Acceleration Mechanism of Resistive MHD Jets Launched from Accretion Disks

Details The Acceleration Mechanism of Resistive MHD Jets Launched from Accretion Disks The Acceleration Mechanism of Resistive MHD Jets Launched from Accretion Disks

2004-11-26

arxiv.org/abs/astro-ph/0411712v1

Astrophys.J. 621 (2005) 921-931

Astronomy and Astrophysics

Astrophysics

15 pages, 15 figures, 1 table, accepted for publication in ApJ

Scientific paper

10.1086/427720

We analyzed the results of non-linear resistive magnetohydrodynamical (MHD) simulations of jet formation to study the acceleration mechanism of axisymmetric, resistive MHD jets. The initial state is a constant angular momentum, polytropic torus threaded by weak uniform vertical magnetic fields. The time evolution of the torus is simulated by applying the CIP-MOCCT scheme extended for resistive MHD equations. We carried out simulations up to 50 rotation period at the innermost radius of the disk created by accretion from the torus. The acceleration forces and the characteristics of resistive jets were studied by computing forces acting on Lagrangian test particles. Since the angle between the rotation axis of the disk and magnetic field lines is smaller in resistive models than in ideal MHD models, magnetocentrifugal acceleration is smaller. The effective potential along a magnetic field line has maximum around $z \sim 0.5r_0$ in resistive models, where $r_0$ is the radius where the density of the initial torus is maximum. Jets are launched after the disk material is lifted to this height by pressure gradient force. Even in this case, the main acceleration force around the slow magnetosonic point is the magnetocentrifugal force. The power of the resistive MHD jet is comparable to the mechanical energy liberated in the disk by mass accretion. Joule heating is not essential for the formation of jets.

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