Black Holes at the LHC

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1 Black Holes at the LHC Dr Cigdem Issever University of Oxford 04. November 2008 Particle Physics Seminar

2 Outline Introduction to Black Holes Gravity and Standard Model Extra Dimension Models Production of BH at the LHC Experimental Signatures Why the Earth is safe C. Issever, University of Oxford 2

3 A Bit of Black Hole History 18th 1915/ Pierre-Simon Laplace & John Michel Albert Einstein Karl Schwarzschild Roy Kerr John A. Wheeler Stephen Hawking C. Issever, University of Oxford 3

4 Schwarzschild Black Holes non-rotating uncharged can t orbit black hole nothing can escape C. Issever, University of Oxford 4

Rotating Black Holes Kerr Solution rotating massive body frame dragging ergosphere: particles have to corotate Penrose effect BH emits energetic

5 Rotating Black Holes Kerr Solution rotating massive body frame dragging ergosphere: particles have to corotate Penrose effect BH emits energetic particles energy loss Stationary horizon C. Issever, University of Oxford 5

6 The No-Hair Theorem Black holes are characterized by their energy, angular momentum, electric charge. Don t conserve B, L or flavour in ordinary world C. Issever, University of Oxford 6

7 Production of Black Holes EVENT HORIZON Bring mass closer than its Schwarzschild Radius, R S, R = S 2 G M c 2 R s SINGULARITY and a black hole will form! C. Issever, University of Oxford 7

8 Production of Black Holes Bring mass closer than its Schwarzschild Radius, R S, R = S 2 G M c 2 and a black hole will form! R S Earth = 8.8mm C. Issever, University of Oxford 8

9 Production of Black Holes Bring mass closer than its Schwarzschild Radius, R S, R s quark R = S 2 G M c 2 quark and a black hole will form! 2quarks 50 R S 10 m C. Issever, University of Oxford 9

10 Gravity and Particle Physics C. Issever, University of Oxford 10

11 The Standard Model C. Issever, University of Oxford 11

12 Comparison of the Forces in Nature Gravity Weak Electromagnetic Strong Graviton (not observed) W +, W -, Z Photon Gluon All Quarks & Leptons Quarks, charged leptons, W +, W - Quarks & gluons Gravity is very weak --- Hierarchy Problem! M PL ~10 19 GeV : M EWK ~10 3 GeV C. Issever, University of Oxford 12

13 The Standard Model Gravity is not included Particles + Forces = Picture of nature Too many elementary particles: 60 C. Issever, University of Oxford 13

14 The Standard Model Gravity is not included Particles + Forces = Picture of nature Too many elementary particles: 60 C. Issever, University of Oxford 14

15 The Standard Model Gravity is not included Particles + Forces = Picture of nature Too many elementary particles: 60 There must be something beyond it! C. Issever, University of Oxford 15

16 Extra Dimensions No theory of first principles Provide simplified framework with testable results Can help us to gain insights about the underlying theory C. Issever, University of Oxford 16

17 Extra Dimensions are not a new idea! 1920 s Kaluza&Klein unify electromagnetism with gravity 1970 String Theory is born 1971 SUSY enters the stage 1974 Gravitons pop out of String theory 1984 Superstring Theory 10, 11 or 26 extra dimensions needed Compactified 1998 Large Extra Dim. Nima Arkani-Hamed, Savas Dimopoulos, and Gia Dvali C. Issever, University of Oxford 17

18 Extra Dimension (ED) Models ED may explain complexity of particle physics Where are they? C. Issever, University of Oxford 18

19 Extra Dimension (ED) Models ED may explain complexity of particle physics Where are they? C. Issever, University of Oxford 19

Extra Dimension (ED) Models ED may explain complexity of particle physics Where are they? http://www.particleadventure.

20 Extra Dimension (ED) Models ED may explain complexity of particle physics Where are they? our world gravity extra dimension Gravity is escaping into the extra dimensions. C. Issever, University of Oxford 20

21 Gravity in Extra Dimension At small distances gravity can be very strong, up to times stronger: F G r D n+ 2 G = GL D n At large distances gravity seems weak n GD G n+2 (2π) F M L n 2 2 D = r r 8πG G is diluted strength of gravity in our 3-dim. space. G D is the (4+n)-dimensional Newton gravity constant. D C. Issever, University of Oxford 21

22 Experimental Limits Table top Particle accelerators Astrophysical observations Cosmic-ray measurements Cosmological considerations C. Issever, University of Oxford 22

23 Table Top Experiments 1/r 2 -law valid for R=44 µm at 95% Ann.Rev.Nucl.Part.Sci.53:77-121,2003, hep-ph/ C. Issever, University of Oxford 23

24 Particle Accelerators hep-ph/ , hep-ex/ , hep-ph/ , hep-ex/ , hep-ex/ LEP: M D =1.5 TeV for n = 2 R = 0.2 µm M D = 0.75 TeV for n = 5 R = 400 fm CDF: M D = 1.33 TeV, n = 2 R = 0.27 µm M D = 0.88 TeV for n = 6 R = 31fm D0 (ll, gg): M D = 1.23 TeV lower limit C. Issever, University of Oxford 24

25 Astrophysical and Cosmological Constraints hep-ph/ , hep-ph/ , hep-ph/ Places the most stringent lower limits on M D in ADD Supernova cooling due to KK G emission SN 1987A did not emit more KK G than compatible with neutrino signal durations observed by Kamiokande and IMB places the limits: M D > 22 (2) TeV for n = 2 (3). Energetic Gamma Ray Experiment Telescope (EGRET) Cosmic γ-ray-bkg: M D > 70 (5) TeV for n = 2 (3) Neutron star halo of 100 MeVγ-rays: M D > 97, 8, 1.5 TeV for n = 2, 3, 4 All neutron stars in the galactic bulge: M D > 1130, 57, 7, 1.8 TeV for n = 2, 3, 4, 5 Neutron star heating: M D >1760, 77, 9, 2 TeV for n = 2, 3, 4, 5 Ultra high-energy cosmic-ray neutrinos: They could be in reach of the LHC lower bound M D = 1 to 1.4 TeV, n = 4 to 7 C. Issever, University of Oxford 25

26 Black LHC C. Issever, University of Oxford 26

27 Production of Black Holes at the LHC R = n 2 G * L M S 2 c quark R s quark x b x a M = sx x = sˆ a b R 2quarks m S BH LHC C. Issever, University of Oxford 27

28 Semi Classical Production Cross Section πr 2 ab BH h σ (s) ˆ valid for M >> M D σ (s) = pp BH+X 1 1 M a a,b s dx dx f (x )f (x ) σ ( sˆ ) 2 2 M x s a b a a b b ab BH parton distribution functions C. Issever, University of Oxford 28

29 Time Evolution of Black Holes 1. Horizon formation 2. Balding phase Class. emission of gravitional waves Kerr BH 4. Planck phase????? Pick what you like 3. Evaporation phase Hawking radiation Superradiance C. Issever, University of Oxford 29

30 Trapped Energy Discussion Formation of BH is very non-linear and complicated M < sˆ BH Fractions of E, p and J are lost before settling to a BH! Yoshino & Rychkov calculated energy loss hep-ph/ C. Issever, University of Oxford 30

31 Effect of energy loss in formation and balding phase M * =1 TeV semi classical hep-ph/ single t ~ 250 pb d=10 d=5 trapped surface cross section C. Issever, University of Oxford 31

32 Production Cross Section for flat tensionless Brane [hep-ph] too close to Planck scale 250 pb C. Issever, University of Oxford 32

33 Production Cross Sections for flat, tensionless Brane [hep-ph] single t ~ 250 pb ~30 smaller d=10 ~150 smaller C. Issever, University of Oxford 33

34 Split Fermion Brane Extra Dimensions hep-ph/ , , , ;gr-qc/ BH don t conserve B or L or flavour induced proton decay! n nbar oscillations! Flavour changing neutron currents or large neutrino mixing gauging B, L, F mini bulk OR leptons quarks SPLIT extra dimension C. Issever, University of Oxford 34

35 Split Fermion Brane Extra Dimensions [hep-ph] fm lepton brane quark brane BH at the LHC will decay mainly into quarks and gluons! C. Issever, University of Oxford 35

36 Production Cross Section for Split Fermion EDs [hep-ph] 250 pb C. Issever, University of Oxford 36

37 Branes with positive Tension φ 1 B ϕ deficit-angle parameter C. Issever, University of Oxford 37

38 Production Cross Section on Brane with Tension 250 pb C. Issever, University of Oxford 38

39 Time Evolution of Black Holes 1. Horizon formation 2. Balding phase Class. emission of gravitional waves Kerr BH 4. Planck phase????? Pick what you like 3. Evaporation phase Hawking radiation Superradiance C. Issever, University of Oxford 39

40 Black Holes decay! Joins gravitation, quantum field theory and thermodynamics!!! c 2 M T = PL H 8π k B 1 1 M BH emit particles black body thermal spectrum. Intensity BH LHC ~ s Decays with equal probability to all particles. Energy C. Issever, University of Oxford 40

41 Black Holes decay! Astronomical BH -- COLD Low Evaporation Rate Micro BH -- HOT High Evaporation Rate M T 10-6 [ K] H M emit particles black body thermal spectrum. Intensity BH LHC ~ s Decays with equal probability to all particles. Energy C. Issever, University of Oxford 41

42 Black Holes decay! Astronomical BH -- COLD Low Evaporation Rate Micro BH -- HOT High Evaporation Rate T 1+ n H M 1/(1 + n) BH emit particles black body thermal spectrum. Intensity BH LHC ~ s Decays with equal probability to all particles. Energy C. Issever, University of Oxford 42

44 Footprints of Microscopic Black Holes hadron : lepton 5 : 1 Theoretical uncertainties large May be it looks like a yeti?? high multiplicities particles/event decay product s energies up to TeV SM backgrounds expected to be low C. Issever, University of Oxford 44

45 [hep-ph] scenario q + g leptons W, Z ν G H photons d=4, J=0 79% 9.5% 5.7% 3.9% 0.2% 0.9% 0.8% d=10, J=0 74% 7.7% 6.8% 3.2% 6.5% 0.7% 1.5% d=10, J=0, 84% 1.8% 5.4% 0.5% 6.7% 0.3% 1.6% n s =7 d=5, J=0, n s =2, B=0.4 96% 1.6% 1.7% 0.15% 0.4% 0.2% 0.3% d=10, J>0 78% 6.5% 9.6% 2.5%? 0.7% 2.6% C. Issever, University of Oxford 45

46 [hep-ph] scenario q + g leptons W, Z ν G H photons d=4, J=0 79% 9.5% 5.7% 3.9% 0.2% 0.9% 0.8% d=10, J=0 74% 7.7% 6.8% 3.2% 6.5% 0.7% 1.5% d=10, J=0, 84% 1.8% 5.4% 0.5% 6.7% 0.3% 1.6% n s =7 d=5, J=0, n s =2, B=0.4 96% 1.6% 1.7% 0.15% 0.4% 0.2% 0.3% d=10, J>0 78% 6.5% 9.6% 2.5%? 0.7% 2.6% C. Issever, University of Oxford 46

47 [hep-ph] scenario q + g leptons W, Z ν G H photons d=4, J=0 79% 9.5% 5.7% 3.9% 0.2% 0.9% 0.8% d=10, J=0 74% 7.7% 6.8% 3.2% 6.5% 0.7% 1.5% d=10, J=0, 84% 1.8% 5.4% 0.5% 6.7% 0.3% 1.6% n s =7 d=5, J=0, n s =2, B=0.4 96% 1.6% 1.7% 0.15% 0.4% 0.2% 0.3% d=10, J>0 78% 6.5% 9.6% 2.5%? 0.7% 2.6% C. Issever, University of Oxford 47

48 [hep-ph] scenario q + g leptons W, Z ν G H photons d=4, J=0 79% 9.5% 5.7% 3.9% 0.2% 0.9% 0.8% d=10, J=0 74% 7.7% 6.8% 3.2% 6.5% 0.7% 1.5% d=10, J=0, 84% 1.8% 5.4% 0.5% 6.7% 0.3% 1.6% n s =7 d=5, J=0, n s =2, B=0.4 96% 1.6% 1.7% 0.15% 0.4% 0.2% 0.3% d=10, J>0 78% 6.5% 9.6% 2.5%? 0.7% 2.6% C. Issever, University of Oxford 48

49 [hep-ph] scenario q + g leptons W, Z ν G H photons d=4, J=0 79% 9.5% 5.7% 3.9% 0.2% 0.9% 0.8% d=10, J=0 74% 7.7% 6.8% 3.2% 6.5% 0.7% 1.5% d=10, J=0, 84% 1.8% 5.4% 0.5% 6.7% 0.3% 1.6% n s =7 d=5, J=0, n s =2, B=0.4 96% 1.6% 1.7% 0.15% 0.4% 0.2% 0.3% d=10, J>0 78% 6.5% 9.6% 2.5%? 0.7% 2.6% C. Issever, University of Oxford 49

50 Footprints of Microscopic Black Holes hadron : lepton 5 : 1 Theoretical uncertainties large May be it looks like a yeti?? high multiplicities particles/event decay product s energies up to TeV SM backgrounds expected to be low C. Issever, University of Oxford 50

51 Multiplicity for d = 5, M * =1 TeV, Mbh> 5TeV C. Issever, University of Oxford 51

52 Footprints of Microscopic Black Holes hadron : lepton 5 : 1 Theoretical uncertainties large May be it looks like a yeti?? high multiplicities particles/event decay product s energies up to TeV SM backgrounds expected to be low C. Issever, University of Oxford 52

53 Scalar Sum Pt of Black Hole Events Sum P T > 2.5TeV C. Issever, University of Oxford 53

54 Missing Transverse Energy (MET) Sum P T > 2.5TeV Hard to reproduce in other new physics scenarios. C. Issever, University of Oxford 54

55 Reconstructed Mass Sum P T > 2.5TeV Sum P T > 2.5TeV LeptonP > 50GeV T Backgrounds are low C. Issever, University of Oxford 55

56 Discovery Reach for S>10 and S/sqrt(B) > 5 M * =1TeV CoM 14 TeV BH with m>5 TeV with a few pb -1 BH with m>8 TeV with 1 fb -1 C. Issever, University of Oxford 56

57 The US Federal Court scheduled trial to begin 16 June C. Issever, University of Oxford 57

LHC is safe! J. Ellis, http://indico.cern.ch/conferencedisplay.py?confid=39099 LHC@14 TeV=cosmic ray@10 17 ev ~ 3.

58 LHC is safe! J. Ellis, TeV=cosmic 17 ev ~ cosmic rays >10 17 ev have struck Earth Equivalent to 10 5 LHC programmes Area of Sun 10 4 larger stars in galaxy galaxies in Universe Nature has performed LHC programmes Nature carries out LHC programmes per second Flux*E 3 /10 24 (ev 2 m -2 s -1 sr -1 ) 1 10 arxiv: v2 [hep-ph] log 10 (E)[eV ultra-high-energy cosmic rays up to ev C. Issever, University of Oxford 58

59 Black Holes are safe Giddings & Mangano arxiv: [hep-ph] Concerns: Will be produced in LHC Will be neutral and stable Black Holes are unstable Otherwise 2 nd law of thermodynamics violated Hawking, decay is related to their production EVEN IF stable, accretion rate negligible if high D EVEN IF low D, some of those produced by cosmic rays would be charged would have stopped in Earth: We are here!` EVEN IF all neutral, some would have been produced on white dwarfs and neutron stars would have stopped: `White dwarfs and neutron stars are out there!` C. Issever, University of Oxford 59

60 Why the Earth won t be destroyed Small gravitational attraction Mass loss: dm TeV/sec dt Mass gain in quark gluon plasma: hep-ph/ dm+ dt TeV/sec C. Issever, University of Oxford 60

61 Summary Black Holes are not black! Extra Dimension Strong gravity Probe Planck scale physics general relativity quantum theory Discovery possible at the LHC with a few pb -1 Challenging experimental signatures The LHC is safe! C. Issever, University of Oxford 61

62 Credits Dechang Dai Glenn Starkman Dejan Stojkovic ATLAS TeV-Gravity Group C. Issever, University of Oxford 62

63 Backup Slides C. Issever, University of Oxford 63

64 Gravity and Metrics c τ = c dt dr r ( dθ sin 2 θdϕ ) Minkowski metric of special relativity rs 2 2 dr c τ = (1 ) c dt r ( dθ sin 2 θdϕ ) r rs 1 r Schwarzschild metric, solution of Einstein s field equation in empty space r r 2 2 ρ r r 2 2 2r r sin c τ = (1 s ) c dt dr ρ dθ ( r + α + α s sin θ )sin 2θ dϕ + α θ s cdtd ρ Λ ρ ρ C. Issever, University of Oxford 64

65 Planck Scale Definitions M M M n+ 2 D D 2 DL n+ 2 GT (2 ) / 8 (2 ) / 4 G = G *(2 R) D = = 1/ G = D = n + 4 π π n D π n π n π G G D D PDG definition Dimopoulos & Landsberg Giddings & Thomas D-dimensional Newton Gravity constant hep-ph/ , , , Total number of dimensions C. Issever, University of Oxford 65

66 Laws of Black Hole Mechanics BH Thermodynamics 0 th Law Horizon has constant surface gravity, κ 1 st Law κ dm da dj dq 8π Thermodynamics 0 th Law T is constant in a body of thermal equibilirium 1 st Law = + Ω + Φ du = dq dw 2 nd Law da 0 3 rd Law No BH with κ = 0! 2 nd Law entropy of a closed system is a non-decreasing function of time 3 rd Law Can t reach absolute zero in a physical process T BH = κ 2π S = BH C. Issever, University of Oxford 66 A 4

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