SEMANA 1

General Covariance

To start with, we recall the basic notions of the Special Theory of Relativity. We explain that Minkwoskian coordinates in flat space-time correspond to inertial observers. Then we continue with transformations to non-inertial reference systems in flat space-time. We show that non-inertial observers correspond to curved coordinate systems in flat space-time. In particular, we describe in grate details Rindler coordinates that correspond to eternally homogeneously accelerating observers. This shows that our Nature allows many different types of metrics, not necessarily coincident with the Euclidian or Minkwoskain ones. We explain what means general covariance. We end up this module with the derivation of the geodesic equation for a general metric from the least action principle. In this equation we define the Christoffel symbols.

7 videos

Vídeo: General covariance
Vídeo: Сonstant linear acceleration
Vídeo: Transition to the homogeneously accelerating reference frame (or system) in Minkowski space–time
Vídeo: Transition to the homogeneously accelerating reference frame in Minkowski space–time (part 2)
Vídeo: Geodesic equation
Vídeo: Christoffel symbols

Nota atribuída: Problems 1

SEMANA 2

Covariant differential and Riemann tensor

We start with the definition of what is tensor in a general curved space-time. Then we define what is connection, parallel transport and covariant differential. We show that for Riemannian manifolds connection coincides with the Christoffel symbols and geodesic equations acquire a clear geometric meaning. We end up with the definition of the Riemann tensor and the description of its properties. We explain how Riemann tensor allows to distinguish flat space-time in curved coordinates from curved space-times. For this module we provide complementary video to help students to recall properties of tensors in flat space-time.

9 videos

Vídeo: Covariant differentiation
Vídeo: Parallel transport
Vídeo: Covariant differentiation(part 2)
Vídeo: Locally Minkowskian Reference System (LMRS)
Vídeo: Curvature or Riemann tensor
Vídeo: Properties of Riemann tensor
Vídeo: Tensors in flat space-time(part 1)
Vídeo: Tensors in flat space-time(part 2)

Nota atribuída: Problems 2

SEMANA 3

Einstein-Hilbert action and Einstein equations

We start with the explanation of how one can define Einstein equations from fundamental principles. Such as general covariance, least action principle and the proper choice of dynamical variables. Namely, the role of the latter in the General Theory of Relativity is played by the metric tensor of space-time. Then we derive the Einstein equations from the least action principle applied to the Einstein-Hilbert action. Also we define the energy-momentum tensor for matter and show that it obeys a conservation law. We describe the basic generic properties of the Einstein equations. We end up this module with some examples of energy-momentum tensors for different sorts of matter fields or bodies and particles.To help understanding this module we provide complementary video with the explanation of the least action principle in the simplest case of the scalar field in flat two-dimensional space-time.

6 videos

Vídeo: Einstein equations
Vídeo: Matter energy–momentum (or stress-energy) tensor
Vídeo: Examples of matter actions
Vídeo: The least action (or minimal action) principle (part 1)
Vídeo: The least action principle (part 2)

Nota atribuída: Problems 3

SEMANA 4

Schwarzschild solution

With this module we start our study of the black hole type solutions. We explain how to solve the Einstein equations in the simplest settings. We find perhaps the most famous solution of these equations, which is referred to as the Schwarzschild black hole. We formulate the Birkhoff theorem. We end this module with the description of some properties of this Schwarzschild solution. We provide different types of coordinate systems for such a curved space-time.

5 videos

Vídeo: Schwarzschild solution(part 2)
Vídeo: Gravitational radius
Vídeo: Schwarzschild coordinates
Vídeo: Eddington–Finkelstein coordinates

Nota atribuída: Problems 4

SEMANA 5

Penrose-Carter diagrams

We start with the definition of the Penrose-Carter diagram for flat space-time. On this example we explain the uses of such diagrams. Then we continue with the definition of the Kruskal-Szekeres coordinates which cover the entire black hole space-time. With the use of these coordinates we define Penrose-Carter diagram for the Schwarzschild black hole. This diagram allows us to qualitatively understand the fundamental properties of the black hole.

4 videos

Vídeo: Kruskal–Szekeres coordinates
Vídeo: Penrose–Carter diagram for the Schwarzschild black hole
Vídeo: Penrose–Carter diagram for the Schwarzschild black hole (part 2)

Nota atribuída: Problems 5

SEMANA 6

Classical tests of General Theory of Relativity

We start with the definition of Killing vectors and integrals of motion, which allow one to provide conserving quantities for a particle motion in Schwarzschild space-time. We derive the explicit geodesic equation for this space-time. This equation provides a quantitative explanation of some basic properties of black holes. We use the geodesic equation to explain the precession of the Mercury perihelion and of the light deviation in curved space-time.

5 videos

Vídeo: Test particle motion on Schwarzschild black hole background
Vídeo: Test particle motion on Schwarzschild black hole background(part 2)
Vídeo: Mercury perihelion precession
Vídeo: Light ray deviation in the vicinity of the Sun

Nota atribuída: Problems 6

SEMANA 7

Interior solution and Kerr's solution

We start with the definition of the so called perfect fluid energy-momentum tensor and with the description of its properties. We use this tensor to derive the so called interior solution of the Einstein equations, which provides a simple model of a star in the General Theory of Relativity. Then we continue with a brief description of the Kerr solution, which corresponds to the rotating black hole. We end up this module with a brief description of the Cosmic Censorship hypothesis and of the black hole No Hair Theorem.

4 videos

Nota atribuída: Problems 7

SEMANA 8

Collapse into black hole

We start with the derivation of the Oppenheimer-Snyder solution of the Einstein equations, which describes the collapse of a star into black hole. We derive the Penrose-Carter diagram for this solution. We end up this module with a brief description of the origin of the Hawking radiation and of the basic properties of the black hole formation.

4 videos

Vídeo: Penrose–Carter diagram for the Oppenheimer– Snyder collapsing solution
Vídeo: Hints on Hawking radiation
Vídeo: Black hole horizon creation

Nota atribuída: Problems 8

SEMANA 9

Gravitational waves

With this module we start our study of gravitational waves. We explain the important difference between energy-momentum conservation laws in the absence and in the presence of the dynamical gravity. We define the gravitational energy-momentum pseudo-tensor. Then we continue with the linearized approximation to the Einstein equations which allows us to clarify the meaning of the pseudo-tensor. We end up this module with the derivation of the free monochromatic gravitational waves and of their energy-momentum pseudo-tensor. These waves are solutions of the Einstein equations in the linearized approximation.

3 videos

Vídeo: Weak field approximation
Vídeo: Free gravitational waves

Nota atribuída: Problems 9

SEMANA 10

Gravitational radiation

In this module we show how moving massive bodies create gravitational waves in the linearized approximation. Then we continue with the derivation of the exact shock gravitational wave solutions of the Einstein equations. We describe their properties. To help to understand this module we provide two complementary videos. One with the explanations how to perform the averaging over directions in space. And the other video is with the derivation of the retarded Green function.

6 videos

Vídeo: Intensity of the radiation
Vídeo: Shock gravitational wave or Penrose parallel plane wave
Vídeo: Properties of the Penrose parallel plane wave
Vídeo: Green functions
Vídeo: Averages

Nota atribuída: Problems 10

SEMANA 11

Friedman-Robertson-Walker cosmology

With this module we start our discussion of the cosmological solutions. We define constant curvature three-dimensional homogeneous spaces. Then we derive Friedman-Robertson-Walker cosmological solutions of the Einstein equations. We describe their properties. We end up this module with the derivation of the vacuum homogeneous but anisotropic cosmological Kasner solution.

4 videos

Vídeo: Friedmann–Robertson–Walker metric
Vídeo: Homogeneous isotropic cosmological solutions
Vídeo: Anisotropic Kasner cosmological solution

Nota atribuída: Problems 11

SEMANA 12

Cosmological solutions with non-zero cosmological constant

In this module we derive constant curvature de Sitter and anti de Sitter solutions of the Einstein equations with non-zero cosmological constant. We describe the geometric and causal properties of such space-times and provide their Penrose-Carter diagrams. We provide coordinate systems which cover various patches of these space-times.

9 videos

Vídeo: Geometry of the de Sitter space–time
Vídeo: Metric of the de Sitter space–time
Vídeo: Penrose–Carter diagram for the de Sitter space–time
Vídeo: Poincare' patches for the de Sitter space–time
Vídeo: Geometry of the anti–de Sitter space–time
Vídeo: Metric of the anti–de Sitter space–time
Vídeo: Penrose–Carter diagram of the anti–de Sitter space–time
Vídeo: Poincare' patch of the anti–de Sitter space–time

Nota atribuída: Problems 12

Nível	Avançado
Compromisso	12 weeks of study, 4-6 hours per week
Idioma	English
Como ser aprovado	Seja aprovado em todas as tarefas para concluir o curso.
Classificação do usuário	4.6 estrelas Classificação média do usuário 4.6Veja o que os aprendizes disseram

Introduction into General Theory of Relativity

Introduction into General Theory of Relativity