Jets are ubiquitous in the Universe and are seen from a large number of astrophysical
objects including active galactic nuclei, gamma ray bursters, micro-quasars, proto-planetary …

When astrophysical jets were discovered one hundred years ago, the field of numerical
simulations did not yet exit. Since the arrival of programmable computers though, numerical …

Context. The planet-forming region of protoplanetary disks is cold, dense, and therefore
weakly ionized. For this reason, magnetohydrodynamic (MHD) turbulence is thought to be …

The global evolution and dispersal of protoplanetary disks (PPDs) are governed by disk
angular-momentum transport and mass-loss processes. Recent numerical studies suggest …

We perform three-dimensional, vertically-stratified, local shearing-box ideal MHD
simulations of the magnetorotational instability (MRI) that include a net vertical magnetic flux …

Planets appear to form in environments shaped by the gas flowing through protostellar disks
to the central young stars. The flows in turn are governed by orbital angular momentum …

Context. Astrophysical disks are likely embedded in an ambient vertical magnetic field
generated by its environment. This ambient field is known to drive magneto-rotational …

We present a study of X-ray ionization of MHD accretion-disk winds in an effort to constrain
the physics underlying the highly ionized ultra-fast outflows (UFOs) inferred by X-ray …

Context. The theory of jet emitting disks (JEDs) provides a mathematical framework for a self-
consistent treatment of steady-state accretion and ejection. A large-scale vertical magnetic …

Standard models of accretion discs study the transport of mass on a viscous time-scale but
do not consider the transport of magnetic flux. The evolution of a large-scale poloidal …