Alexander E. Dudorov

Two-dimensional adaptive code for simulation of astrophysical magnetohydrodynamic flows

Integrated adaptive mesh for simulations of two-dimensional (2D) self-gravitating, axially symmetric magnetohydrodynamic (MHD) flows in spherical coordinates is constructed and a new adaptive numer...

Theory of fossil magnetic field

Theory of fossil magnetic field is based on the observations, analytical estimations and numerical simulations of magnetic flux evolution during star formation in the magnetized cores of molecular clouds. Basic goals, main features of the theory and manifestations of MHD effects in young stellar objects are discussed.

Numerical Simulations of the Astrophysical MHD Flows

Magnetic fields can play an important role in many astrophysical problems. At the present time, sufficient observational data have been gathered about the magnetic field of the interstellar medium, molecular clouds, star formation regions, Bok globules, and young stellar objects (Heiles et all, 1993; Dudorov, 1995; Vallee, 1997). This shows that star formation takes place in rotating magnetized interstellar clouds.

MHD-Collapse of protostellar clouds

Abstract The subject of this paper is the numerical simulation of two-dimensional gravitational MHD collapse of protostellar clouds. A new numerical method was constructed to solve the equations of a two-component mixture including the effects of ambipolar diffusion, non-stationary ionization, and heating (cooling). The method was implemented in a two-dimensional code that simulates the MHD-collapse on a Eulerian cylindrical grid. The code uses the explicit monotonic Osher scheme which gives a third-order accurate approximation in space and a second-order approximation in time. The method was tested on several problems, one of which, isothermal gravitational collapse of a rotating protostellar cloud, is discussed in some detail.

Dynamics of magnetic flux tubes and IR-variability of young stellar objects

We simulate the dynamics of slender magnetic flux tubes (MFTs) in the accretion disks of T Tauri stars. The dynamical equations of our model take into account the aerodynamic and turbulent drag forces, and the radiative heat exchange between the MFT and ambient gas. The structure of the disk is calculated with the help of our MHD model of the accretion disks. We consider the MFTs formed at the distances

Magnetic field buoyancy in accretion disks of young stars

0.027-0.8

Hierarchical structure of the interstellar molecular clouds and star formation

au from the star with various initial radii and plasma betas

Angular momentum evolution of protostellar clouds

\beta_0

Protostar formation in magnetized rotating molecular cloud cores

. The simulations show that the MFT with weak magnetic field (

Thermal instability in magnetized interstellar clouds

\beta_0=10