A new Chemo–Dynamical Smoothed Particle Hydrodynamic (CD-SPH) code is presented. The disk galaxy is described as a multi–fragmented gas and star system, embedded in a cold dark matter halo with a rigid potential field. The star formation (SF) process, SNII, SNIa and PN events, and the chemical enrichment of gas, have all been considered within the framework of the standard SPH model, which we u...

We present results from a Smoothed Particle Hydrodynamic (SPH) simulation of galaxy formation that exceeds the minimum resolution requirement suggested by Steinmetz & Muller (1993) of 3 × 10 SPH particles per galaxy. Using the multiple mass technique an effective resolution of a little over one billion particles is attained within a 48 Mpc cube. We find that even with an SPH mass resolution of ...

Context. One of the ways to determine the contribution of the dark halo to the gravitational potential of a galaxy is the study of noncircular (streaming) motions and the associated gas shocks in the bar region. These motions, determined by the potential in the inner parts, can break the disk-halo degeneracy. Here, two main fluid dynamical approaches have been chosen to model the non-circular m...

Modern cosmological observations allow us to study in great detail the evolution and history of the large scale structure hierarchy. The fundamental problem of accurate constraints on the cosmological parameters, within a given cosmological model, requires precise modelling of the observed structure. In this paper we briefly review the current most effective techniques of large scale structure ...

N-body/hydrodynamic numerical simulations of galaxy clusters including the interaction of the intra-cluster medium (ICM) with the galaxies are one of the outstanding challenges in computational astrophysics. We include metal enrichment processes like galactic winds and ram-pressure stripping. Galactic winds are calculated with an additional code which takes into account cosmic rays as well as m...

In this paper, we present the results of smoothed particle hydrodynamic (SPH) simulations of collisions between pre-main sequence stars and a variety of other kinds of stars. Simulations over a range of impact parameters and velocities were performed. We find that pre-main sequence stars tend to “wrap themselves” around their impactor. We discuss the probable evolutionary state of products of c...