Wolfram Schmidt

Black hole formation in the early Universe

Supermassive black holes with up to a

The characteristic black hole mass resulting from direct collapse in the early Universe

\rm 10^{9}~M_{\odot}

Algorithmic comparisons of decaying, isothermal, supersonic turbulence

dwell in the centers of present-day galaxies, and their presence has been confirmed at z

High resolution studies of massive primordial haloes

\geq

Three-dimensional simulations of globule and pillar formation around HII regions: turbulence and shock curvature

6. Their formation at such early epochs is still an enigma. Different pathways have been suggested to assemble supermassive black holes in the first billion years after the Big Bang. Direct collapse has emerged as a highly plausible scenario to form black holes as it provides seed masses of

Turbulence production and turbulent pressure support in the intergalactic medium

\rm 10^{5}-10^{6}~M_{\odot}

ADAPTIVELY REFINED LARGE EDDY SIMULATIONS OF A GALAXY CLUSTER: TURBULENCE MODELING AND THE PHYSICS OF THE INTRACLUSTER MEDIUM

. Gravitational collapse in atomic cooling haloes with virial temperatures T

The small-scale dynamo and the amplification of magnetic fields in massive primordial haloes

_{vir} \geq 10^{4}

A fluid-dynamical subgrid scale model for highly compressible astrophysical turbulence

~K may lead to the formation of massive seed black holes in the presence of an intense background UV flux. Turbulence plays a central role in regulating accretion and transporting angular momentum. We present here the highest resolution cosmological large-eddy simulations to date which track the evolution of high-density regions on scales of

The structure of the thermally bistable and turbulent atomic gas in the local interstellar medium

0.25