  A black hole can be regarded as a thermodynamic system described by a grand
canonical ensemble. In this paper, we study the Bekenstein-Hawking entropy of
higher-dimensional rotating black holes using the Euclidean path-integral
method of Gibbons and Hawking. We give a general proof demonstrating that
ignoring quantum corrections, the Bekenstein-Hawking entropy is equal to
one-fourth of its horizon area for general higher-dimensional rotating black
holes.
