General Relativity for Cosmology (AMATH875/PHYS786)

Tadpole Galaxy

Term: Fall 2015
Course codes: AMATH875/PHYS786
Instructor: Achim Kempf
Prerequisites: A first course in General Relativity or consent of instructor
Time: Mondays and Fridays, 1:30 - 2:45 pm
Venue: Alice room, Perimeter Institute
Office hours: by arrangement
First lecture: Monday 14 September 2015, 1:30pm

Picture on the right: This Hubble image lets us see half way through the age of the universe. In the "foreground" is the tadpole galaxy.

Content

This is an advanced graduate course which develops the math and physics of general relativity from scratch up to the highest level. The going is sometimes steep but always careful. The purpose is to prepare students for studies in quantum gravity, relativistic quantum information, black hole physics and cosmology. (To this end, this course will be followed up in W16 by the course Quantum Field Theory for Cosmology.)

Coordinate-free Differential Geometry, Weyl versus Ricci curvature versus Torsion, Vielbein Formalism, Spin-connections, Form-valued Tensors, Spectral Geometry, some Cohomology.
Derivations of General Relativity including as a Gauge Theory, Diffeomorphism Invariance vs. Symmetries, Bianchi Identities vs. Local and Global Conservation Laws.
Penrose Diagrams for Black Holes and Cosmology, Types of Horizons, Energy Conditions and Singularity theorems, Properties and Classification of Exact Solutions.
Cosmology and Models of Cosmic Inflation

Lecture notes and video recordings

The lecture notes will be made available here:

Lecture 0: Assigned reading. A review of special relativity. Transition to general relativity.

Lecture 1: Overview. Differentiable manifolds.

Lecture 2: Algebra of function germs. Algebraic definition of tangent space.

Lecture 3: Physical and geometric definitions of tangent space. Tangent bundle and its sections.

Lecture 4: Algebra of differential forms. (Anti-) derivations. Exterior derivative. Cohomology. Categories.

Lecture 5: Inner derivation. Lie derivative on forms and on general tensors. Infinitesimal diffeomorphisms.

Lecture 6: Orientability and volume. Divergence. Integration. Stokes', Green's and Gauss' theorems. Metric.

Lecture 7: Hodge *. Hilbert Space Λ. Co-derivative. d'Alembertian. Klein Gordon and Maxwell equations.

Lecture 8: Affine connection. Absolute covariant derivative. Autoparallels and parallel transport.

Lecture 9: Torsion. Geodesics. Riemann normal coordinates. Curvature. Ricci identity. Bianchi identities.

Lecture 10: Levi-Civita connection. D. Moving frames. Tensor-valued p-forms. Cartan Structure equation.

Lecture 11: Riemannian structure. Spectra of Laplacians on p-forms. Infinitesimal spectral geometry.

Assigned viewing: Planck scale physics and spectral geometry

Lecture 12: Euler Lagrange equations. Klein Gordon, Electromagnetic & Dirac equations in curved spacetime.

Lecture 13: Energy momentum tensor. Killing vectors. T^ab_;b = 0. T^ab for scalar fields and perfect fluids.

Lecture 14: Static and stationary spacetimes. Weak and dominant energy conditions. Induced gravity action.

Lecture 15: General relativity in the tetrad formulation. GR as a gauge theory.

Lecture 16: Using the tetrad formalism to obtain cosmological solutions. Friedman equation.

Lecture 17: Cosmological epochs. Flatness and horizon problems. Inflation. Quantum origin of structure.

Lecture 18: Curvature in terms of light cones and conformal factor. Conformal equivalence. Penrose diagrams.

Lecture 19: Lie algebra of Killing vector fields. Segre classification. Weyl curvature. Petrov classification.

Lecture 20: Time orientability. Chronological and causal future and past. Stable vs. strong causality.

Lecture 21: Cauchy horizons. Incomplete geodesics. Singularities. Energy conditions. Geodesic congruences.

Lecture 22: Raychaudhury equation. Singularity theorems. Cosmological singularities. Apparent horizons.

Lecture 23: What replaces gravitational potential energy? ADM and SB momentum and angular momentum.

The video recordings of the lectures are here on the PIRSA.org site.

If you are not enrolled here at UW but are using the videos and/or lecture notes please drop me a line, I'd just like to know. Thanks!

Essay and project

The grades will be based on an essay and a project, in equal parts.

Deadline for submitting both essay and project, combined in one PDF file not exceeding 20 pages, is 10:00am on 20 December 2015.

Essay

The essay topic is taken from the first half of the course. The topic will be: "Mathematical methods to capture shape".

Your task is to review the various mathematical methods that are being used to describe the "shape" of a Riemannian or Lorentzian manifold. Remember, there are methods to describe the shape of a manifold by using the fact that a nontrivial shape implies violations of Pythagoras' law. Then there are methods using deficiency angles or causal dynamical triangulations (look it up), and methods that use the nontriviality of parallel transport or the affine connection, the tetrad fields that diagonalize the metric-tensor, the overtone spectrum and spectral geometry (for compact Riemannian manifolds), the Weyl and Ricci curvature decomposition, the causal structure plus a conformal function description, and there are probably many others. Try to cover several ideas and approaches and feel free to include new ideas if some come to mind. The point is to explain some of those approaches and how they do or may relate to each other in your own words - possibly with a discussion of the possible pros and cons of these methods, i.e., with a discussion of which approach might be useful for which purpose. Focus on the main ideas and concepts rather than getting lost in details. You can choose to write much more on one or two approaches than on others. But in any case your essay should contain an overview over and a discussion of a range of methods.

Project

The project topic is chosen from the second half of the course (in particular the upcoming lectures 15, 16, 17): "Numerical explorations of the dynamics of FRW cosmologies".
Your task is:

Briefly explain the origin of the three coupled equations that determine the time evolution of the scale factor, the energy density and the pressure in spatially flat FRW cosmological models.
Main task: Study the past and future evolution of the night sky. Namely, explore the behavior of the flat FRW solutions numerically, i.e., numerically simulate the time evolution of the universe under different conditions. Here is a suggestion for how you may want to structure your explorations (you are free to structure your explorations differently):
- For practice, and as a consistency check, I would suggest to first try to recover numerically the behavior in each cosmological epoch that we solve for analytically in class. Namely, make an assumption for a fixed value of the equation of state parameter, separately for the epochs (e.g., of radiation, dust and cosmological constant domination) that follow each other as the universe gets more and more diluted. Then solve the dynamical equations and plot the results for each epoch and compare with the analytically predicted behavior.
- Then, make the equation of state parameter w vary in a prescribed way. To this end, assume that w is a given function w(rho) of the energy density, that you choose so that w(rho) runs successively between the values for radiation, dust and vacuum energy dominance as the universe gets diluted, i.e., as rho drops. Notice that w(rho) should not drop uniformly but should drop so as to reflect the presence of more or less clearly defined epochs connected by transitional periods.
- One question you may want to explore whether the behavior of the dynamics is sensitive to how slowly or how abruptly w changes. For example, w may changes very quickly at a time when the matter in the universe undergoes a phase transition.
- Here is another question you may want to address: No known form of matter, or of vacuum energy, or combination thereof, would lead to a value of w < -1. However, several experiments, including recent experimental data. "Leading dark energy theory incompatible with new measurement" on Scientific American indicate that the evolution of the universe is currently such that w is smaller -1, namely approximately -1.19. Explore numerically and/or analytically what the long term fate of the universe will be according to general relativity, if indeed w is and will stay at that value.
- Another question that you may want to explore numerically and/or analytically is the question of whether there are choices of w(rho) such that a shrinking FRW universe would not collapse completely, i.e., so that the scale factor would get smaller only down to a finite smallest value and then grow again (a so-called bounce).

Don't forget to state all your sources clearly, also for the project. This also includes the software that you use. If you use a specialized software package for GR, mention this. In this case the expectations are somewhat higher of course.

General advice on what is expected in the essay

Format: title and abstract page/motivation/main parts/summary (or conclusions)/bibliography.
Bibliography: Again, list all of your sources explicitly. Of course you can use Wikipedia but you should not cite it - because it can change from day to day and because as it not (yet) reliable enough to meet scientific standards. Instead, cite books and papers that you may have found via Wikipedia. Also, it is good style to list items in the bibliography in that sequence in which they are first referred to in the text.
At most about 10 pages.
An essay should be a review of existing literature on a given topic. The sources can be textbooks, lecture notes or review articles or original articles or some of each. All and everything that is used needs to be cited. Most articles are now available online and for example "Google Scholar" can get you there quickly. Try for example searching for a few key words along with the words "review" or "introduction". Most electronic journals require a subscription, which the university library usually has. For the license to be recognized you may need to browse either from a university computer (the domain is what counts) or you log into the library website from home and go to an electronic journal through the library's electronic journal search engine.
In the essay, your task is to show that you have understood and critically reflected upon the material by making it your own. You make it your own by coming up with an original way for presenting the material that you are bringing together. Try to give it your own angle or spin. Wherever possible, try to put things into a larger context. Sometimes (hopefully very rarely) it may be necessary to stick quite closely to a source, e.g., when a calculation is to be presented and the source does it in a way that is just hard to improve upon. In this case, you can make it your own for example by filling in a few steps in the calculation that the author omitted. In this case, it is important that you point out at that place that you do so. Filling in steps obviously proves that you understood that calculation.
A good essay describes. An excellent essay explains.
No original research is expected. But, you are encouraged to make educated speculations about what interesting things could be done in this area. You have been a regurgitating undergraduate for a long time. This is an opportunity to show that you still have some creativity left in you! Don't worry, you are not expected to solve the problem of quantum gravity here. Just show that you are thinking for yourself.

General advice on what is expected in the project

Format: introduction/motivation/methods/results/discussion/references.
Make sure you list your sources and the technology (software in particular) that you may be using.
At most about 10 pages.

Literature

We will be using mainly material from the following three texts:

N. Straumann, General Relativity with Applications to Astrophysics, Springer (2004)
J. Stewart, Advanced General Relativity, Cambridge (1991)
S. Hawking, G.F.R. Ellis, The Large Scale Structure of Space-Time, Cambridge (1973)

Note: These three texts are available at the Davis Library.

Recommended general references are also:

Scott Dodelson, Modern Cosmology, Academic Press, San Diego, (2003)
A.R. Liddle, D.H. Lyth, Cosmological Inflation and Large-Scale Structure, CUP (2000)
G.F.R. Ellis and J. Wainwright, Dynamical Systems in Cosmology, CUP (1997)
R. M. Wald, General Relativity, University of Chicago Press (1984)
H. Stephani, General Relativity, Cambridge University Press (CUP) (1982)

We will cover Sakharov's "induced gravity" argument. Read the original (very short) paper here:

Here are links to general online reviews:

You may also wish to have a look at these free only resources: A collection of links