Lovelock theory is the natural extension of General Relativity to higher di-mensions and can also be thought of as a toy model for ghost-free highercurvature gravity. These gravity theories capture some of the de ning fea-tures of higher curvature gravities, namely the existence of more than one(A)dS vacuum and an intricate dynamics, more general black hole solutionsand instabilities; while avoiding some of their problems. In particular, Love-lock gravities yield second order eld equations so that they can be consideredbeyond the perturbative regime and are free of higher derivative ghosts. Thisprovides an appealing arena to explore di erent gravitational and holographicaspects of higher curvature gravity.Most of the vacua of the theory support black holes that display inter-esting features. Besides, black holes with maximally symmetric horizons aresubject to a version of Birkho 's theorem and their solutions can be foundanalytically. Most e orts in the literature have been devoted however to oneparticular branch of solutions, often restricted to a speci c combination ofthe Lovelock couplings. The branch usually chosen for the analysis is the so-called EH-branch, as it actually reduces to the general relativistic solutionas we turn o the higher order couplings. In this thesis we have presentedsome tools that allow for the description of Lovelock black holes for arbitraryvalues of the whole set of couplings, dimensionality and order of the theory.Despite the fact of the solution being implicit, it is possible to extract mostrelevant information and discuss all possible cases in the general situation,analyze the number of horizons, the thermodynamic stability of the solution,phase transitions, etc. Furthermore, this approach has been generalized tothe case of charged and cosmological solutions, and also to the so calledquasi-topological gravities, that share the same functional form of the blackhole solutions with the Lovelock family while being lower dimensional.Our method is very useful to gain intuition about physical processes in-volving black holes. One can easily visualize the evolution of the position andnumber of horizons as the mass of the solution varies, this providing crucialinformation about, for instance, the possible appearance of naked singulari-ties or the violation of the third law of thermodynamics. We have seen thatthe rigid symmetry imposed on the solution naively allows such problematicbehavior which is avoided once the stability of the solution is taken into fullconsideration.