Upper bound on entropy.
Abstract
The upper bound proposed by Bekenstein (1982) for the entropy S of a system (such as a black hole) with energy E and 'length scale' R, S less than or equal to 2(pi)(ER) is examined theoretically. A somewhat more stringent limit, S less than or equal to 0.575(ER), is derived and shown to be independent of blackhole thermodynamic arguments. It is pointed out that Bekenstein's (1981 and 1982) arguments are valid only in the semiclassical approximation and assume both the existence of black holes and the applicability of semiclassical thermodynamics with them.
 Publication:

Nuovo Cimento Lettere
 Pub Date:
 December 1984
 Bibcode:
 1984NCimL..41..493K
 Keywords:

 Astrophysics;
 Black Holes (Astronomy);
 Entropy;
 Stellar Evolution;
 Black Body Radiation;
 Maxima;
 Astrophysics