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DO EVAPORATING BLACK HOLES FORM PHOTOSPHERES AND/OR CHROMOSPHERES? Jane H MacGibbon, B.J. Carr and Don N. Page MacGibbon Carr & Page PRD 78, 064043 (2008); Page Carr & MacGibbon PRD 78, 064044 (2008) JANE H MACGIBBON UNIVERSITY OF NORTH FLORIDA MacGibbon, Carr & Page "Black Hole Chromospheres/Photospheres" MG12 Paris July 12 - 18 2009 MOTIVATION Heckler Model A.F.Heckler PRD 55, 480 (1997); A.F.Heckler PRL 78, 3430 (1997) • QED/QCD bremsstrahlung and pair-production interactions between Hawking-radiated particles form photosphere/chromosphere Other Photosphere/Chromosphere Models • Belyanin et al • Bugaev et al • D. Cline and Hong • Kapusta and Daghigh MacGibbon, Carr & Page "Black Hole Chromospheres/Photospheres" MG12 Paris July 12 - 18 2009 BLACK HOLE THERMODYNAMICS HAWKING TEMPERATURE: M BH c 1.06 13 GeV 8 GM BH 10 g 3 kTBH Solar Mass BH TBH ~ 10 -7 K MBH ~ 10 25 g TBH ~ 3 K CMB HAWKING RADIATION FLUX: d NS snl dt dE n,l 2 2 2s E n e 1 exp / 2 c MacGibbon, Carr & Page "Black Hole Chromospheres/Photospheres" MG12 Paris July 12 - 18 2009 1 HAWKING RADIATION Sources: Page, Elster, Simkins STANDARD PICTURE BH should directly Hawking evaporate those particles which appear non-composite compared to wavelength of the radiated energy (or equivalently BH size) at given TBH As TBH increases: BH directly emits photons + gravitons + neutrinoes + electrons + muons + pions Once TBH >>ΛQCD: BH directly emits quarks and gluons (not direct pions) which shower and hadronize into astrophysically stable γ , ν, p, pbar, e-, e+ MacGibbon, Carr & Page "Black Hole Chromospheres/Photospheres" MG12 Paris July 12 - 18 2009 HAWKING RADIATION Source: MacGibbon and Webber (1990) TOTAL BLACK HOLE EMISSION dM BH 2 25 1 5 x 10 M / g f M g s MASS LOSS RATE: BH BH dt 1 - 27 3 6 . 24 x10 M f M s BLACK HOLE LIFETIME: evap i i Mass of PBH whose lifetime equals age of Universe (MacGibbon, Carr & Page 2008): M 5.00 0.04 10 gm 14 MacGibbon, Carr & Page "Black Hole Chromospheres/Photospheres" MG12 Paris July 12 - 18 2009 HECKLER MODEL Number Density at radius r from BH of e- directly Hawking radiated by BH n r 104 where k G c 1 0 M BH r 2 Two-body QED bremsstrahlung cross-section in BH center-of-mass frame 8 3 2E brem Plasma mass correction me 2 ln m 'e me m pm 2 Total Number of Scatterings N R rmax R rmin rBH me 2 for e e e e where m pm 2 4 n r N r 1 dr 3 where r n r brem vrel and n r r 2 Eav n0 r QED Photosphere above TBH ~ 45 GeV. Similarly QCD brem 8 s 3 2 E ln 2 mq mq Chromosphere above TBH ~ ΛQCD IS THE HECKLER MODEL CORRECT? QED 3-vertex Bremsstrahlung IS THE HECKLER MODEL CORRECT? √ Two-body bremsstrahlung cross-section brem d brem 1 8 3 2 E d 2 ln E0 d me me E Average momentum exchanged is ~ me in centerof-momentum (CM) frame particles must be within ~ 1/ me of each other to interact Average angle between final on-shell electron and outgoing photon in CM frame is φav~ me / 2E Average energy of final on-shell electron and outgoing photon in CM frame is Ee~ ω ~ E / 2 MacGibbon, Carr & Page "Black Hole Chromospheres/Photospheres" MG12 Paris July 12 - 18 2009 IS THE HECKLER MODEL CORRECT? √ Heckler assumes, even after photosphere / chromosphere develops, that most particles are moving radially out from BH For random walk, particle emitted by TBH ~ 1-10 2 7 GeV BH would have to undergo N 10 av scatterings to deviate O 0.1 1 from the radial MacGibbon, Carr & Page "Black Hole Chromospheres/Photospheres" MG12 Paris July 12 - 18 2009 IS THE HECKLER MODEL CORRECT? √ BH is center-of-momentum frame for most pairs of emitted charged particles BUT two particles moving in similar direction will not interact near BH (because their center-ofmomentum frame is highly Lorentz-boosted) ‘Exclusion cone’ around emitted particle once particle is a distance d from BH the transverse distance to nearest particle for interaction is xT ~ d particles must be within ~1/me of BH to interact MacGibbon, Carr & Page "Black Hole Chromospheres/Photospheres" MG12 Paris July 12 - 18 2009 IS THE HECKLER MODEL CORRECT? MacGibbon, Carr & Page "Black Hole Chromospheres/Photospheres" MG12 Paris July 12 - 18 2009 IS THE HECKLER MODEL CORRECT? For radial emission r n r bremvrel is not correct must be replaced by radial description 1 particles are Hawking emitted near BH so particles do not travelling in from minus ∞, past the BH and each other, then out to plus ∞ BUT bremsstrahlung cross-section assumes interacting particles travel in from minus ∞ interaction cross-section is decreased MacGibbon, Carr & Page "Black Hole Chromospheres/Photospheres" MG12 Paris July 12 - 18 2009 IS THE HECKLER MODEL CORRECT? Causality Constraint Two particles must be in casual contact to interact BUT negligible fraction of Hawking emitted particles are in causal contact with each other Time between subsequent Hawking emissions is Δte ~ 200 / Epeak For causal contact within ~ 1 / me of BH require Δte < Δtc ~1 / γ me where γ ~ Epeak / me Δtc << Δte for almost all emitted particles MacGibbon, Carr & Page "Black Hole Chromospheres/Photospheres" MG12 Paris July 12 - 18 2009 IS THE HECKLER MODEL CORRECT? Scale for Completion of Interaction Heckler assumed distance required for formation of final on-shell electron and outgoing photon is dform ~1 / me in CM frame BUT average angle between final on-shell electron and photon is φav~ me / 2E so dform ~E / me2 in CM frame Electron must travel dform ~E / me2 before it can undergo next on-shell interaction Any multiple interactions of electron within ~1 / me of BH are off-shell interactions and so strongly suppressed by LPM effect MacGibbon, Carr & Page "Black Hole Chromospheres/Photospheres" MG12 Paris July 12 - 18 2009 IS THE HECKLER MODEL CORRECT? The Heckler QED photosphere model does not work because it neglects the requirement that the emitted particles must be in causal contact to interact and neglects LPM effects in any (very rare) multiple scatterings MacGibbon, Carr & Page "Black Hole Chromospheres/Photospheres" MG12 Paris July 12 - 18 2009 QCD CHROMOSPHERE? when TBH >>ΛQCD the causality constraint (Δte ~ 20 / Epeak ) and LPM suppression in any (rare) multiple scatterings also prevent QCD chromosphere formation for 4D BHs BUT could a QCD chromosphere form when TBH ~ ΛQCD? MacGibbon, Carr & Page "Black Hole Chromospheres/Photospheres" MG12 Paris July 12 - 18 2009 QCD CHROMOSPHERE WHEN TBH~ ΛQCD? Hawking emission damped (lower flux and greater Δt between emissions) near rest mass threshold (eg ΛQCD) + low multiplicity per jet near ΛQCD Δt between consecutive Hawking emissions increases around ΛQCD causality constraint is stronger MacGibbon, Carr & Page "Black Hole Chromospheres/Photospheres" MG12 Paris July 12 - 18 2009 QCD CHROMOSPHERE WHEN TBH~ ΛQCD? e+e- accelerator collisions – smooth transition around ΛQCD from direct π regime to quark/gluon mediated regime – sets in when π relativistic i.e. sets in when constituent quarks relativistic when BH goes from directly emitting π to directly emitting quarks and gluons, initial quarks and gluons are relativistic MacGibbon, Carr & Page "Black Hole Chromospheres/Photospheres" MG12 Paris July 12 - 18 2009 QCD CHROMOSPHERE WHEN TBH~ ΛQCD? number of final states from hadronization is limited by available energy (E ~ ΛQCD per Hawking emitted particle) + conservation laws decays produce mainly π (only a couple of π) around ΛQCD and soft gluon bremsstrahlung is insignificant (because lowest colourless state from g is π) MacGibbon, Carr & Page "Black Hole Chromospheres/Photospheres" MG12 Paris July 12 - 18 2009 QCD CHROMOSPHERE WHEN TBH~ ΛQCD? TBH ~ ΛQCD BH no simultaneous production of ultrahigh density QCD particles TBH ~ ΛQCD BH can NOT form quark-gluon plasma No analogy to RHIC quark-gluon plasma (RHIC ~ 200 GeV per nucleon, gluon-saturated, high baryon/antibaryon asymmetry) MacGibbon, Carr & Page "Black Hole Chromospheres/Photospheres" MG12 Paris July 12 - 18 2009 OTHER PHOTOSPHERE/ CHROMOSPHERE MODELS • Kapusta and Daghigh – assumes plasma thermalized by QED and QCD bremsstrahlung and pair-production of Heckler model • Belyanin et al – ‘collisionless’ QED plasma – omits Lorentz factors no self-induced MHD photosphere but strong ambient magnetic field may induce (weak) photosphere • Bugaev et al – ‘Stretched Horizon’ Tpl region just outside horizon neglects LPM suppression (and thermalization scales) • D. Cline and Hong – Hagedorn-type emission of remaining BH mass into exponentially growing number of states at TBH ~ ΛQCD state occupancy should be determined by available energy E ~ ΛQCD model would require direct coupling of BH mass to Hagedorn states (but TBH increases as 1/MBH 2) BREMSSTRAHLUNG EFFECTS (Page, Carr and MacGibbon 2008) Inner Bremsstrahlung 2-vertex Bremsstrahlung 3-vertex Bremsstrahlung MacGibbon, Carr & Page "Black Hole Chromospheres/Photospheres" MG12 Paris July 12 - 18 2009 INNER BREMSSTRAHLUNG Number flux of inner bremsstrahlung photons radiated by charged particles of mass m and γav~ 4.20TBH / m emitted by BH with spectrum dN/dt: d 2 N b 2 dN ln 2 av 1 dtd dt Nearly flat power spectrum up to ω ~ E – m cut-off Total power in inner bremsstrahlung photons radiated by charged particles emitted by BH with power dE/dt: dEb 2 dE ln 2 av 1 dt dt MacGibbon, Carr & Page "Black Hole Chromospheres/Photospheres" MG12 Paris July 12 - 18 2009 INNER BREMSSTRAHLUNG Total power in inner bremsstrahlung photons radiated by charged particle emitted by BH with power dE/dt: dEb 2 dE ln 2 av 1 dt dt Compare with power in direct photons: dEd dt 4 0.3364 x 10 M BH For MBH = 5x1014 g BH, 2 At low 0, d 2 Eb d 2 Ed dtd 1.73 x 1019 s 1 8 3 2 M 3 4 dtd inner bremsstrahlung photons dominate the directly Hawking emitted photons below 57 MeV MacGibbon, Carr & Page "Black Hole Chromospheres/Photospheres" MG12 Paris July 12 - 18 2009 CONCLUSIONS (FOR 4D BLACK HOLES) MacGibbon, Carr and Page 2008: None of the photosphere/chromosphere models work because they neglect the requirement that the emitted particles must be in causal contact to interact and/or neglect LPM effects in any multiple scatterings and/or energy constraints Energy and quantum conservation laws prevent significant increase in particle states near TBH ~ ΛQCD no quark-gluon plasma near TBH ~ ΛQCD MacGibbon, Carr & Page "Black Hole Chromospheres/Photospheres" MG12 Paris July 12 - 18 2009 Predicted Black Hole Spectra Source: MacGibbon and Webber (1990) Astrophysical Spectra from Uniformly Distributed PBHs with dn/dMi α Mi-2.5 Source: MacGibbon and Carr (1991) HIGHER-DIMENSIONAL BLACK HOLES? Even one interaction (ie N ~ 1) could modify expected signal compared with experimental precision MacGibbon, Carr & Page "Black Hole Chromospheres/Photospheres" MG12 Paris July 12 - 18 2009