The authors assume an initial protogalaxy to consist of a few independently moving clouds. As driving process of its early evolution they have the collisions of clouds. This process dissipates energy, but slowly enough such that the evolution can be considered as quasi-static. The retarding process is star formation which the authors model with a phenomenological formula depending on the density and the random velocities of the clouds. Star formation diminishes the substrate of the driving process and therefore may bring the evolution to a "halt" if there is not new delivery. If this condition does not act, then a further "halt" occurs if the energetically deepest state permitted under conservation of angular momentum is arrived at. The aut...
We use our model for the formation and evolution of galaxies within a two-phase galaxy formation sce...
We present a phenomenological model for understanding the origins and evolution of galaxy morphologi...
Context.Modelling the gaseous component of the interstellar medium (ISM) by Smoothed Particles Hydro...
Numerical experiments concerning the dynamics of a distribution of interacting gas clouds in a proto...
We reanalyze the formation and evolution of galaxies in the hierarchical clustering scenario. Using ...
The formation and evolution of galaxies is studied using two alternative modelling techniques within...
We present a theoretical model embedding the essential physics of early galaxy for-mation based on t...
A semi-analytic model is proposed that couples the Press-Schechter formalism for the number of galax...
Many models exist in the literature of either star formation or galactic structure, but the former c...
We model star formation in a wide range of isolated disk galaxies composed of a dark matter halo and...
We construct a simple prescription based on hydrodynamical simulations to predict the effective radi...
In this thesis, we explore the use of semi-analytic galaxy formation models and related techniques a...
We use our model for the formation and evolution of galaxies within a two-phase galaxy formation sce...
ABSTRACT In recent years, simple models of galaxy formation have been shown to provid...
We invistigate different aspects of galaxy formation like star formation histories, galaxy interacti...
We use our model for the formation and evolution of galaxies within a two-phase galaxy formation sce...
We present a phenomenological model for understanding the origins and evolution of galaxy morphologi...
Context.Modelling the gaseous component of the interstellar medium (ISM) by Smoothed Particles Hydro...
Numerical experiments concerning the dynamics of a distribution of interacting gas clouds in a proto...
We reanalyze the formation and evolution of galaxies in the hierarchical clustering scenario. Using ...
The formation and evolution of galaxies is studied using two alternative modelling techniques within...
We present a theoretical model embedding the essential physics of early galaxy for-mation based on t...
A semi-analytic model is proposed that couples the Press-Schechter formalism for the number of galax...
Many models exist in the literature of either star formation or galactic structure, but the former c...
We model star formation in a wide range of isolated disk galaxies composed of a dark matter halo and...
We construct a simple prescription based on hydrodynamical simulations to predict the effective radi...
In this thesis, we explore the use of semi-analytic galaxy formation models and related techniques a...
We use our model for the formation and evolution of galaxies within a two-phase galaxy formation sce...
ABSTRACT In recent years, simple models of galaxy formation have been shown to provid...
We invistigate different aspects of galaxy formation like star formation histories, galaxy interacti...
We use our model for the formation and evolution of galaxies within a two-phase galaxy formation sce...
We present a phenomenological model for understanding the origins and evolution of galaxy morphologi...
Context.Modelling the gaseous component of the interstellar medium (ISM) by Smoothed Particles Hydro...