  We present an overall picture of the advances in the description of black
hole physics from the perspective of loop quantum gravity. After an
introduction that discusses the main conceptual issues we present some details
about the classical and quantum geometry of isolated horizons and their quantum
geometry and then use this scheme to give a natural definition of the entropy
of black holes. The entropy computations can be neatly expressed in the form of
combinatorial problems solvable with the help of methods based on number theory
and the use of generating functions. The recovery of the Bekenstein-Hawking law
and corrections to it is explained in some detail. After this, due attention is
paid to the discussion of semiclassical issues. An important point in this
respect is the proper interpretation of the horizon area as the energy that
should appear in the statistical-mechanical treatment of the black hole model
presented here. The chapter ends with a comparison between the microscopic and
semiclassical approaches to the computation of the entropy and discusses a
number of issues regarding the relation between entanglement and statistical
entropy and the possibility of comparing the subdominant (logarithmic)
corrections to the entropy obtained with the help of the Euclidean path
integral with the ones obtained in the present framework.
