A black hole can be rightfully thought as the most extreme manifestation of gravity – and thus of curvature! Besides being a unique source of puzzles and paradoxes for scientists, they have also been the inspiration for endless and breathtaking adventures in science-fiction novels and movies. This chapter will, therefore, explain the concept of black hole by making use of two different mechanical equivalents that have many points in common with black holes. In this way, it will become clear what is an event horizon and why it represents a one-way membrane, which can be entered, but from within which nothing can exit, not even light. Similarly, we will introduce the concept of spacetime singularity and explain why this is a problem that worries us physicists most, and for which we have not found any satisfactory solution yet. We will see that black holes are beautiful manifestations of nature and are not more monstrous than an erupting volcano.

The simplest curved spacetimes of general relativity are the ones with the most symmetry, and the most useful of these is the geometry of empty space outside a spherically symmetric source of curvature – for example, a spherical star. This is called the Schwarzschild geometry. To an excellent approximation, this is the curved spacetime outside the Sun and therefore leads to the predictions of Einstein’s theory most accessible to experimental test. In this chapter, we explore the geometry of Schwarzschild’s solution, assuming it’s given. We will concentrate on predicting the orbits of test particles and light rays in the curved spacetime of a spherical star that exhibit some of the famous effects of general relativity – the gravitational redshift, the precession of the perihelion of a planet, the gravitational bending of light, and the time delay of light.

This chapter introduces compact objects, white dwarfs, neutron stars, and black holes. The properties of compact objects are summarized as the typical radius, mass, and compactness. These compact objects are the final end point in stellar evolution. The stellar evolution in terms of the mass of the star is outlined, focusing on the burning stages and the final collapse of the star, either as a white dwarf or in a core-collapse supernova. Historical notes are given for the discovery of white dwarfs and neutron stars.