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First we consider CRNBH metric which is obtained by solving Einstein-Maxwellmetric equation for a point electric charge $e$ inside of a spherical staticbody with mass $M$. It has 2 interior and exterior horizons. UsingBekenestein-Hawking entropy theorem we calculate interior and exterior entropy,temperature, Gibbs free energy and heat capacity at constant electric charge.We calculate first derivative of the Gibbs free energy with respect totemperature which become a singular function having a singularity at criticalpoint with corresponding temperature $T_c=\frac{1}{24\pi \sqrt{3}|e|}.$ Hencewe clime first order phase transition is happened there. Temperature same asGibbs free energy takes absolutely positive (negative) values on the exterior(interior) horizon. The Gibbs free energy takes two different positive valuessynchronously for $0<T<T_c$ but not for negative values which means the systemis made from two subsystem. For negative temperatures entropy reaches to zerovalue at $T\to-\infty$ and so takes Bose-Einstein condensation single state.Entropy increases monotonically in case $0<T<T_c$. Regarding results of thework presented at Ref. \citep{Bob01} we calculate again the mentionedthermodynamical variables for remnant stable final state of evaporating QRNBHand obtained results same as one in case of the CRNBH. Finally, we solve massloss equation of QRNBH against advance Eddington-Finkelstein time coordinateand derive luminosity function. We obtain switching off of QRNBH evaporationbefore than the mass completely vanishes. It reaches to a could Lukewarm typeof RN black hole which its final remnant mass is $m_{final}=|e|$ in geometricalunits. Its temperature and luminosity vanish but not in Schwarzschild case ofevaporation. Our calculations can be takes some acceptable statements aboutinformation loss paradox .

Classical and Quantum Reissner-Nordstr\"om Black Hole Thermodynamics and first order Phase Transition