Regular Black Hole Remnants

The Einstein equations admit the class of regular solutions asymptotically de Sitter at the origin (Lambda delta(i)(k) as r -> 0) and at infinity (lambda delta(i)(k) as r -> infinity). In a certain range of mass M they describe a regular cosmological black holes with three horizons, a cosmological horizon r(c), a black hole horizon r(b) < r(c) and an internal horizon r(a) < r(b). Generic asymptotic behavior of a metric function defines generic dynamics of evaporation: It involves a phase transition where a specific heat is broken and changes its sign. Thermodynamical preference for a final product of the Hawking evaporation is a thermodynamically stable double- horizon (r(a) = r(b)) remnant with the positive specific heat.