  In this work, generalizing our previous results, we determine in an original
and the simplest way three most important thermodynamical characteristics
(Bekenstein-Hawking entropy, Bekenstein quantization of the entropy or (outer)
horizon surface area and Hawking temperature) of Schwarzschild, Kerr and
Reissner-Nordstrom black hole. We start physically by assumption that
circumference of black hole (outer) horizon holds the natural (integer) number
of corresponding reduced Compton's wave length and use mathematically only
simple algebraic equations. (It is conceptually similar to Bohr's quantization
postulate in Bohr's atomic model interpreted by de Broglie relation.)
