Formation of Galaxies and of the Structure at Large Scale in the Universe

Aims

Galaxies are the fundamental components of the structures observed in the universe. Understanding how they formed, from cosmological initial conditions, and which processes were responsible for their evolution until they become the objects we observe nowadays, is a fascinating key question in Astronomy. The enormous amounts of observational data that will become available once the different observational projects are operative, will imply a considerable advancement in our understanding of the physical processes involved in the formation and evolution of galaxies. However, this advancement will only be made possible, if, at the same time, theoretical models to unify data interpretation are developed.

The objetive of this course is to offer a study of galaxy formation and evolution in a cosmological context, and, at the same time, of the structures they form. Particular attention will be paid to comparisons with observational data, both from the local and deep universe. Thanks to the very important developments of computer technology and numerical techniques in the last years, it is now possible to carry out this study from first physical principles through a numerical approach, i.e., the so-called numerical simulations.

In this course, different theoretical tools will be introduced, focusing on the method of numerical simulations. The simulation results will be compared to observational data. The student will have the opportunity to run and analyze some simulations in the practical lessons.

Programme

A. The Cosmological Model at Large Scales: Formation and Evolution of the Structure in the Universe (G. Yepes)

1. Summary of the observational situation
2. The cosmological model
• The Friedmann-Robertson-Walker metric
• The thermal history of the Universe
• The cosmological parameters and their determination
• Dark matter, its nature and consequences
3. The hierarchical scenario for structure formation
   • The evolution of the fluctuation field in the linear phase
   • Statistics of the fluctuation field: the spectrum and the correlation function
   • Determination of the spectrum parameters
4. Numerical simulations in Cosmology
• Collisionless matter: the N-body problem
• Methods of resolution: particle-particle, tree, grids
• Baryonic matter: the hydrodynamic problem
• Initial and boundary conditions
5. Large-scale structure formation and evolution according to numerical simulations
   • The correlation fuction and other statistical descriptors
   • Galaxy clusters
      

B. The Cosmological Model at Scales of ~500 kpc: Galaxy Formation and Evolution (R. Dominguez-Tenreiro)

1. Observational keys: local galaxies and high redshift galaxies or protogalaxies
2. Dynamical processes as keys to galaxy formation and evolution I
• The adhesion model for the nonlinear description of gravitational instability
• Spherical model for the nonlinear collapse
• Other models for the nonlinear collapse
3. Dynamical processes as keys to galaxy formation and evolution II
• Equilibrium of collisionless systems: spheroids and disks
• Coalescences and mergers
• Interactions
• Halo formation and statistics: the Press-Schechter model
4. The role of hydrodynamic processes in galaxy formation and evolution
   • Shock waves Gas cooling and heating.
   • Multiphase medium
   • Processes of gas accumulation before the formation of stars
5. The formation of stars and its consequences
   • Why do stars form?: observations, models, theories and results of numerical simulations
   • Star formation and its connections with dynamical and thermohydrodynamical processes
   • Energetic consequences of star formation
   • Star formation and chemical evolution
   • Observational consequences of star formation
6. Galaxy formation and evolution according to numerical simulations
   • Scenarios for elliptical formation and evolution
   • Scenarios for the formation and evolution of disks of spiral galaxies
   • Scenarios for the formation and evolution of bulges of spiral galaxies
   • Scenarios for the formation and evolution of peculiar and dwarf galaxies
   • The evolutive sequence: scenarios for the interpretation of observations of objects at high redshift
7. Future developments on galaxy formation and evolution: are we in the decade of definitive advancement?

1. Computer Simulations Using Particles R. W. Hockney and J. W. Eastwood, Adam Hilger, 1988
2. GALACTIC ASTRONOMY James Binney and Michael Merrifield, Princeton Series in Astrophysics, 1998
3. GALACTIC DYNAMICS James Binney and Scott Tremaine, Princeton Series in Astrophysics, 1987
4. GALAXY FORMATION Malcolm. S. Longair. Springer-Verlag, 1999.
5. COSMOLOGICAL PHYSICS. John A. Peacock. Cambridge University Press. 1999.
6. COSMOLOGY: THE ORIGIN AND EVOLUTION OF COSMIC STRUCTURE.. P. Coles y F. Lucchin. Wiley Interscience. 1995.
7. COSMOLOGY. M. Rowan-Robinson. Clarendon Press. Oxford (1996).
8. STRUCTURE FORMATION IN THE UNIVERSE. T. Padmamanabhan Cambridge Univ Press. 1993
9. PRINCIPLES OF PHYSICAL COSMOLOGY P.J.E. Peebles. Princeton Univ Press. 1993
10. GRAVITATION AND COSMOLOGY. S. Weinberg. John Wiley and Son. 1972
11. THE LARGE-SCALE STRUCTURE OF THE UNIVERSE. P.J.E. Peebles. Princeton Univ Press. 1980
12. STATISTICS OF THE GALAXY DISTRIBUTION Vicent. J. Martinez and Enn Saar, Chapman and Hall/CRC, 2002