The lecturer and the assistant can be contacted by email at email@example.com, or you can drop by our offices.
Lectures: Mon 12-14 Physicum room A315, Tue 12-14 Physicum room E205
The first lecture of Cosmology II is on Monday October 27.
Exercises: Wed 10-12 Physicum room A315
Note that the first exercise session of Cosmology II is already on October 29.
The exam of Cosmology II will be on Tuesday December 16 at 13.00-17.00 in Physicum room D114. (Exams begin sharp on the hour, not quarter past.)
Not showing up for the exam without such agreement counts as a failed attempt, so one has to retake the course. If the exam date is difficult, it is possible to take the exam later, but this must be agreed with the lecturer before the exam. The exam must be taken before the course is lectured again. The grade is based 25% on the exercises and 75% on the exam. (Exception: for students who have taken the course before, the grade is based only on the exam.) If it's agreed to take the exam later because of scheduling issues, the exercise points will be counted as usual. The exam may be retaken if one gets at least 25% of the total points for the course. For a retaken exam, the grade is based entirely on the exam, the exercise points are not counted.
Lecture notes will appear here as the lectures proceed. Reading
the lecture notes before attending the lectures is recommended.
The introductory lecture Powerpoint file is here. The simulations of large scale structure are from the Max Planck Institute for Astrophysics, here and here.
Chapter 1: Introduction
Chapter 2: Basics of general relativity
Chapter 3: The Friedmann-Robertson-Walker model
Chapter 4: Thermodynamics in an expanding universe
Chapter 5: Thermal history of the early universe
Chapter 6: Big bang nucleosynthesis
Chapter 7: Dark matter
Chapter 8: Inflation: background
Chapter 9: Linear perturbation theory
Chapter 10: Inflation: perturbations
Chapter 11: Perturbations after inflation
Chapter 12: Cosmic microwave background
Contents: The observable universe, homogeneous and isotropic models of the universe, thermal history of the universe, big bang nucleosynthesis, dark matter, inflation, cosmological perturbation theory, cosmic microwave background.
Textbook: Lecture notes.
Literature: E.W. Kolb, M.S. Turner: The Early Universe (Addison-Wesley 1990).
T. Padmanabhan: Structure formation in the universe (Cambridge University Press 1993).
M. Roos: Introduction to Cosmology, 3rd ed. (Wiley 2003).
L. Bergström and A. Goobar: Cosmology and Particle Astrophysics (Wiley 1999).
J.A. Peacock: Cosmological Physics (Cambridge University Press 1999).
A.R. Liddle and D.H. Lyth: Cosmological Inflation and Large-Scale Structure (Cambridge University Press 2000).
S. Dodelson: Modern Cosmology (Academic Press 2003).
V. Mukhanov: Physical Foundations of Cosmology (Cambridge University Press 2005).
S. Weinberg: Cosmology (Oxford University Press 2008).
R. Durrer: The Cosmic Microwave Background (Cambridge University Press 2008).
A.R. Liddle and D.H. Lyth: The Primordial Density Perturbation: Cosmology, Inflation and the Origin of Structure (Cambridge University Press 2009).
It's not necessary to buy any of these textbooks, the lecture notes are sufficient.
Unlike most theoretical physics courses, in Cosmology we will not derive a self-contained theory from basic principles, but we will instead apply known theories to the study of the universe.
In Cosmology I, we look at the universe in the simplest approximation, that of spatial homogeneity and isotropy, to get a basic picture of the composition and evolution of the universe. In Cosmology II, we look at the deviations from homogeneity and isotropy. We consider the origin of structures and the evolution of perturbations, with particular attention to the cosmic microwave background.
The assumed background includes mathematical methods, mechanics, special relativity, statistical physics and some quantum mechanics. Previous knowledge of general relativity is not required, as the results that are used will be reviewed (but not derived). For students who prefer not to have many results presented to them without proper derivation, it is advisable to first take a general relativity course. In Cosmology I we will use the Friedmann-Robertson-Walker models and some basic statistical physics without derivation and in Cosmology II we'll use general relativistic perturbation theory (and a little bit of quantum field theory in curved spacetime) in the same way.
In terms of course lectured at the university of Helsinki, recommended prerequisities are Matemaattiset apuneuvot I ja II, Analyyttinen mekaniikka, FYMM Ia, FYMM Ib, FYMM IIa and Statistinen fysiikka I. The statistical physics course is not completely necessary, but it will make Cosmology I easier to follow. On Cosmology I, we need only very little quantum mechanics, on Cosmology II we will need a little bit of it. The course Kvanttimekaniikka I is enough.