A star that collapses gravitationally can reach a further stage of its life , where quantum-gravitational pressure counteracts weight .
The duration of this stage is very short in the star proper time , yielding a bounce , but extremely long seen from the outside , because of the huge gravitational time dilation .
Since the onset of quantum-gravitational effects is governed by energy density —not by size— the star can be much larger than planckian in this phase .
The object emerging at the end of the Hawking evaporation of a black hole can then be larger than planckian by a factor ( m / m _ { \scriptscriptstyle P } ) ^ { n } , where m is the mass fallen into the hole , m _ { \scriptscriptstyle P } is the Planck mass , and n is positive .
We consider arguments for n = 1 / 3 and for n = 1 .
There is no causality violation or faster-than-light propagation .
The existence of these objects alleviates the black-hole information paradox .
More interestingly , these objects could have astrophysical and cosmological interest : they produce a detectable signal , of quantum gravitational origin , around the 10 ^ { -14 } cm wavelength .