A new quantum black hole phenomenology with A.Barrau, B. Bolliet, H. Haggard, C. Rovelli, C. Weimer Hawking Radiation Conference Stockholm - September 25 th, 2015
Penrose diagram Vidotto, Rovelli 1401.6562 singularity J + horizon r = 0 J -
J + Penrose diagram Vidotto, Rovelli 1401.6562 quantum region trapping horizon surface r = 0 J -
!+!- III J + II Penrose diagram anti-trapping surface quantum region t t = 0 trapping horizon surface Vidotto, Rovelli 1401.6562 - Neglect Hawking radiation in the first approximation - Energy conservation at infinity elastic bounce - GR is time reversal invariant! time-symmetric process: white hole r r = 0 0 I J - Black hole white hole quantum tunneling Haggard, Rovelli 1407.0989 Consider a collapsing quantum light-like shell that bounces and re-expands Hájíček, Kiefer 0107102
Time dilatation internal m 1ms external & m 2 10 9 years r = 0 A black hole is a short cut to the future
How long is the bounce from outside? Upper limit: Vidotto, Rovelli 1401.6562 Firewall argument (Almheiri, Marolf, Polchinski, Sully): something unusual must happen before the Page time (~ 1/2 evaporation time) the hole lifetime must be shorter or of the order of ~ m 3 Lower limit: Haggard, Rovelli 1407.0989 For something quantum to happens, semiclassical approximation must fail. Typically in quantum gravity: high curvature Curvature ~ (LP) -2 Small! effects can pile up: small probability per time unit gives a probable effect on a long time! Typically in quantum tunneling: Curvature (time) ~ (LP) -1 the hole lifetime must be longer or of the order of ~ m 2
Planck Stars Primordial Black Hole Explosion exploding now: r th m m(t) = t=th 4k 1.2 1023 kg R = 2Gm c 2.02 cm {!! LOW ENERGY: size of the source wavelength predicted &.02 cm HIGH ENERGY: energy of the particle liberated fast process ( few milliseconds? ) Tev the source disappears with the burst very compact object: big flux E = mc 2 1.7 10 47 erg Barrau, Rovelli, Vidotto 1409.4031
Exponential decay: m 2 is favorite exploding now: m = r th 4k 1.2 1023 kg R = 2Gm c 2.02 cm {!! LOW ENERGY: size of the source wavelength predicted &.02 cm HIGH ENERGY: energy of the particle liberated fast process ( few milliseconds? ) Tev the source disappears with the burst very compact object: big flux E = mc 2 1.7 10 47 erg Barrau, Rovelli, Vidotto 1409.4031
Maximal distance Barrau, Bolliet, Vidotto, Weimer 1507.1198 shorter lifetime smaller wavelength Low energy channel High energy channel 10 28 10 24 10 26 Hubble radius 10 22 Galactic scale R [m] 10 24 10 22 10 20 Galactic scale R [m] 10 20 10 18 10 16 Hadron decay Direct emission k 1 10 4 E [ev] 2.7 10 8 10 12 10 16 10 20 2.7 10 2 2.7 10 4 2.7 10 6 2.7 10 8 k 1 10 4 10 8 10 12 10 16 10 20 E [ev] 3.6 10 13 3.6 10 14 3.6 10 15 3.6 10 16 3.6 10 17 detection of arbitrarily far signals better single-event detection PBH: mass - temperature relation different scaling! Quantum Gravity Phenomenology!
The smoking gun: distance/energy relation obs 2Gm c 2 (1 + z) v u t H 0 1 6 k 1/2 sinh 1 " M 1/2 (z + 1) 3/2 # distant signals originated in younger and smaller sources l distance 1/wave length taking into account the redshift the resulting function is very slowly varying Barrau, Rovelli, Vidotto 1409.4031 2 4 6 8 10 z
Integrated emission Barrau, Bolliet, Vidotto, Weimer 1507.1198 m 3 Low energy channel High energy channel k=10 22 direct decayed k=10 22 direct+decayed enlarged dn mes dedtds characteristic shape: distorted black body depends on how much DM are PBL Quantum Gravity Phenomenology!
Integrated emission Barrau, Bolliet, Vidotto, Weimer 1507.1198 m 2 Low energy channel k=0.05 High energy channel direct decayed k=0.05 direct+decayed enlarged dn mes dedtds characteristic shape: distorted black body depends on how much DM are PBL Quantum Gravity Phenomenology!
Short Gamma Ray Burst the white hole should eject particles at the same temperature as the particles that felt in the black hole limited horizon due to absorption 100 million light-years / z=0.01 known GRB have energy Tev telescopes spanning large surfaces needed (CTA?) Barrau, Rovelli, Vidotto 1409.4031 obs / (1 + z) sinh 1 " M 1 #! 1 4 2 3 (z + 1) 2
Fast Radio Burst Thornton et al. 1307.1628 Spitler et al. 1404.2934 E. Petroff et al. 1412.0342 Short Observed width milliseconds No Long GRB associated No Afterglow Punctual No repetition Enormous flux density Energy 10 38 erg Likely Extragalactic Dispersion Measure: z 0.5 10 4 event/day A pretty common object? Circular polarization Intrinsic
Fast Radio Burst Barrau, Rovelli, Vidotto 1409.4031 Short " 20 cm Observed width milliseconds size of the source fast process predicted &.02 cm No Long GRB associated No Afterglow Punctual No repetition Enormous flux density Energy 10 38 erg Likely Extragalactic Dispersion Measure: z 0.5 10 4 event/day A pretty common object? Circular polarization Intrinsic Very short GRB? gravitational waves? the source disappears with the burst very compact object 10 47 erg peculiar distance/energy relation Are they bouncing Black Holes?
Summary 1. QUANTUM BLACK HOLE can be singularity free and they can tunnel into a white hole Vidotto, Rovelli 1401.6562 Haggard, Rovelli 1407.0989 * repulsive force @ Planck density 2. PHENOMENOLOGY depends on mass and bounce time * new experimental window for quantum gravity { fast radio burst short GRB Barrau, Rovelli, Vidotto 1409.4031 3. PRIMORDIAL BLACK HOLES { new features diffuse emission Barrau, Bolliet, Vidotto, Weimer 1507.1198