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The photometric evolution of galaxies in a hierarchically clustering universe is investigated. The study is based on high resolution numerical simulations which include the effects of gas dynamics, shock heating, radiative cooling and a heuristic star formation scheme. The outcome of the simulations is convolved with photometric models which enables us to predict the appearance of galaxies in the broad band colors U, B, V, R, I and K. We demonstrate the effect of the mutual interplay of the hierarchical build-up of galaxies, photometric evolution, k-correction, and intervening absorption on the appearance of forming disk galaxies at redshift one to three. We also discuss to what extend the numerical resolution of current computer simulations is sufficient to make quantitative predictions on surface density profiles and color gradients.
I discuss the chemical and spectrophotometric evolution of galaxies over cosmological timescales and present a first attempt to treat both aspects in a chemically consistent way. In our evolutionary synthesis approach, we account for the increasing m
We studied the evolution of the gas kinematics of galaxies by performing hydrodynamical simulations in a cosmological scenario. We paid special attention to the origin of the scatter of the Tully-Fisher relation and the features which could be associ
Symmetric Teleparallel Gravity is an exceptional theory of gravity that is consistent with the vanishing affine connection. This theory is an alternative and a simpler geometrical formulation of general relativity, where the non-metricity $Q$ drives
The problem of chemo-photometric evolution of late-type galaxies is dealt with relying on prime physical arguments of energetic self-consistency between chemical enhancement of galaxy mass, through nuclear processing inside stars, and luminosity evol
We perform a suite of cosmological hydrodynamical simulations of disc galaxies, with zoomed-in initial conditions leading to the formation of a halo of mass $M_{rm halo, , DM} simeq 2 cdot 10^{12}$ M$_{odot}$ at redshift $z=0$. These simulations aim