3D MHD simulations of subsurface convection in OB stars

3D MHD simulations of subsurface convection in OB stars

During their main sequence evolution, massive stars can develop convective regions very close to their surface. These regions are caused by an opacity peak associated with iron ionization. Cantiello et al. (2009) found a possible connection between the presence of subphotospheric convective motions and small scale stochastic velocities in the photosphere of early-type stars. This supports a phy...

3D Anelastic Simulations of Convection in Massive Stars

After briefly describing the anelastic approximation and Glatzmaier’s code, we present results from our preliminary studies of core convection during the hydrogen burning phase of a 15M⊙ star, as well as our most recent results concerning convection in the oxygen shell of a 25M⊙ star.

3D MHD Simulations of Laboratory Plasma Jets

Jets and outflows are thought to be an integral part of accretion phenomena and are associated with a large variety of objects. In these systems, the interaction of magnetic fields with an accretion disk and/or a magnetized central object is thought to be responsible for the acceleration and collimation of plasma into jets and wider angle flows. In this paper we present three-dimensional MHD si...

Unstable Disk Accretion to Magnetized Stars: First Global 3d Mhd Simulations

We report the first global three-dimensional (3D) MHD simulations of disk accretion onto a rotating magnetized star through the Rayleigh-Taylor instability. In this regime, the accreting matter typically forms 2 to 7 vertically elongated “tongues” which penetrate deep into the magnetosphere, until they are stopped by the strong field. Subsequently, the matter is channeled along the field lines ...

3D MHD Simulations of Radio Galaxies Including Nonthermal Electron Transport