Paper detail

The fundamentals on the non-black black holes

On the basis of general relativity and quantum statistics, it was shown (Neslušan L.: 2009, Phys. Rev. D 80, 024015, arxiv:0808.3484) that the equation of state (ES) of extremely hot Fermi-Dirac gas in the surface layer of an ultra-relativistic compact object converges to the same form as the relativistic equation of thermodynamical equilibrium (RETE), which is the condition of stability of the object. The description of energy state of a gas particle was completed with the term corresponding with the potential-type energy. The necessity of such the term is set by the demand of convergence of the relativistic particle-impulse distribution law to its Maxwell-Boltzmann form in the classical limit. The identity of the ES and RETE, both applied to the gas in the object's surface layer, becomes perfect, yielding the stable object, when the object's physical radius is identical to its gravitational radius. In this state, the internal energy of gas particles in a volume of the object's surface layer increases over all limits in the frame of the volume and this opens the question if the horizon of events actually is an insuperable barrier. It seems to be possible that some matter can be temporarily lifted above the surface or, so far, be ejected from the object and can emit a radiation detectable by a distant observer. In our contribution, we demonstrate a general validity of the functional form of the potential-type energy found in our previous work. The consistency of the RETE with its non-relativistic approximation can occur only for this functional form. We also point out some observational consequences of the approximate identity of ES and RETE before the object collapses, in the proper time, to its gravitational radius as well as the possible observational consequences of the infinitely high internal energy in the surface layer of already collapsed object. In general, we propagate the idea that a lot of phenomena observed at the stellar-sized or supermassive black holes (or not-yet black holes) can be not necessarily related to the structures in a vicinity of the black hole, e.g. to an accretion disk, but they can be linked directly to the behaviour of the central, ultra-compact object.