T Naab

Learn More
We present a numerical code for simulating the evolution of astrophysical systems using particles to represent the underlying fluid flow. The code is written in Fortran 95 and is designed to be extremely versatile, flexible and extensible, with modular options that can be selected either at the time the code is compiled or at run time through a text input(More)
We continue our presentation of VINE. In this paper, we begin with a description of relevant architectural properties of the serial and shared memory parallel computers on which VINE is intended to run, and describe their influences on the design of the code itself. We continue with a detailed description of a number of optimizations made to the layout of(More)
  • H Kotarba, Lesch, K Dolag, T Naab, P H Johansson, F A Stasyszyn
  • 2008
We present a set of global, self-consistent N-body/SPH simulations of the dynamic evolution of galactic discs with gas and including magnetic fields. We have implemented a description to follow the evolution of magnetic fields with the ideal induction equation in the SPH part of the Vine code. Results from a direct implementation of the field equations are(More)
We test the formation of low–luminosity elliptical galaxies through collisionless mergers of unequal–mass disk galaxies. The kinematic properties of a small survey of simulated merger end–products with initial disk mass ratios of 3:1 is compared to a sample of seven low–luminosity galaxies observed by Rix et al. that were chosen photometri-cally to be "(More)
Stars form from cold molecular interstellar gas. As this is relatively rare in the local Universe, galaxies like the Milky Way form only a few new stars per year. Typical massive galaxies in the distant Universe formed stars an order of magnitude more rapidly. Unless star formation was significantly more efficient, this difference suggests that young(More)
We present a three-dimensional, fully parallelized, efficient implementation of ionizing UV radiation for smoothed particle hydrodynamics (SPH) including self-gravity. Our method is based on the SPH/tree code VINE. We therefore call it iVINE (for Ioniza-tion + VINE). This approach allows detailed high-resolution studies of the effects of ionizing radiation(More)
  • F Renaud, C M Boily, J.-J Fleck, T Naab, Ch Theis
  • 2008
Gravitational tides are widely understood to strip and destroy galactic substructures. In the course of a galaxy merger, however, transient totally compressive tides may develop and prevent star forming regions from dissolving, after they condensed to form clusters of stars. We study the statistics of such compressive modes in an N-body model of the galaxy(More)
  • S J Karl, T Naab, P H Johansson, Ch Theis, C M Boily
  • 2008
The dates of receipt and acceptance should be inserted later Key words galaxies: evolution – galaxies: interaction – galaxies: individual (NGC 4038, NGC 4039) – methods: numerical In the framework of hierarchical structure formation ellipticals can form from merging of smaller disk galaxies. The nearby interacting 'Antennae' galaxy pair (NGC 4038/39) is one(More)
We present results from our Very Large Telescope large program to study the dynamical evolution of local Ultraluminous Infrared Galaxies (ULIRGs) and QSOs. This paper is the second in a series presenting the stellar kinematics of 54 ULIRGs, derived from high resolution, long-slit Hand K-band spectroscopy. The data presented here, including observations of(More)
Recent observations with the Spitzer Space Telescope show clear evidence that star formation takes place in the surrounding of young massive O-type stars, which are shaping their environment due to their powerful radiation and stellar winds. In this work we investigate the effect of ionising radiation of massive stars on the ambient interstellar medium(More)