Editing Gravitational singularity (section)

== Entropy==
{{further|Black hole|Hawking radiation|Entropy}}
Before [[Stephen Hawking]] came up with the concept of [[Hawking radiation]], the question of black holes having entropy had been avoided. However, this concept demonstrates that black holes radiate energy, which conserves entropy and solves the incompatibility problems with the [[second law of thermodynamics]]. Entropy, however, implies heat and therefore temperature. The loss of energy also implies that black holes do not last forever, but rather evaporate or decay slowly. Black hole temperature is [[Hawking radiation#Emission process|inversely related to mass]].<ref name="LoPresto2003">{{cite journal|last1= LoPresto|first1=M. C.|s2cid=122758428|title= Some Simple Black Hole Thermodynamics|journal= The Physics Teacher|volume= 41|issue=5|year= 2003|pages= 299–301|doi= 10.1119/1.1571268|bibcode=2003PhTea..41..299L}}</ref> All known black hole candidates are so large that their temperature is far below that of the cosmic background radiation, which means they will gain energy on net by absorbing this radiation. They cannot begin to lose energy on net until the background temperature falls below their own temperature. This will occur at a [[cosmological redshift]] of more than one million, rather than the thousand or so since the background radiation formed.{{citation needed|date=October 2018}}