Seong Chan Park SNU SUSY 08 COEX SEOUL

Seong Chan Park (SNU) SUSY 08, COEX, SEOUL June 21, 2008

What’s BH? (1 min summary) • Best known as classical solutions to the Einstein equation. • Classically stable (nothing can come out) • Quantum mechanically unstable (Hawking radiation~Thermal radiation, anything can come out of it) • T=surface gravity~1/r (smaller hotter) • S=surface area~ r^(D-2) • BH is unique (4 D), not unique (D>4) • Black Ring (S^2 XS), Black String (S^2 XR) etc. SUSY 08, Seong Chan Park

Black hole is interesting • Everybody knows it is interesting. • Perfect place to do ‘quantum gravity’ • Has provided a nice testing ground for theory calculations (e. g. microscopic entropy counting of stringy-BH etc. ) • Has deep implication to ‘energy-distance’ relation. • Even it is real!! SUSY 08, Seong Chan Park

Observed Black Holes in the sky The list goes more than 100 now. Name of Binary System Companion Star Spectral Type Orbital Period (days) Black Hole Mass (Solar Units) Cygnus X-1 B supergiant 5. 6 6 -15 LMC X-3 B main sequence 1. 7 4 -11 A 0620 -00 (V 616 Mon) K main sequence 7. 8 4 -9 GS 2023+338 (V 404 Cyg) K main sequence 6. 5 >6 GS 2000+25 (QZ Vul) K main sequence 0. 35 5 -14 GS 1124 -683 (Nova Mus 1991) K main sequence 0. 43 4 -6 GRO J 1655 -40 (Nova Sco 1994) F main sequence 2. 4 4 -5 H 1705 -250 (Nova Oph 1977) K main sequence 0. 52 >4 That’s great. But notice that they all SUSY 08, Seong Chan Park Indirectly observed . Cygnus X-1 Circinus galaxy

‘energy-distance’ relation “To probe smaller distance, you need higher energy” W. Heisenberg This is exactly the reason why we want to build big colliders. distance energy SUSY 08, Seong Chan Park

Big Question Does this curve keep going and touch 0? ? Will this program go on forever? distance energy Answer: No! SUSY 08, Seong Chan Park

‘t Hooft picture of Trans-Planckian domain ‘t Hooft (1987) • Gravity becomes strong/dominate in Ultrahigh-Energy Scattering. New window of bh production opens. • The smallest distance scale we can probe is now determined by the size of event horizon (~GE) which becomes larger with higher E! distance energy SUSY 08, Seong Chan Park

The big Picture: Heisenberg-‘t Hooft Planck domain E~Mp Gravity UV-IR duality distance -Quantum -String theory -no concrete prediction , yet Classical Gravity energy Quantum Gravity Sub-Planckian domain E<<Mp -gauge interaction -(broken)SUSY -GUT SUSY 08, Seong Chan Park Trans-Planckian Domain E>>Mp -gravity dominance -new windows of bh production open -Classical gravity!!

D>4 distance energy If MD~Te. V, as is the case in ADD(1998) and RS(1999), the Heisenberg-’t Hooft picture is actually relevant at the LHC **Te. V dimension was first suggested by I. Antoniadis(1990) SUSY 08, Seong Chan Park

LHC: a BH factory Banks-Fischler (1999), Dimopoulos- Lansberg (PRL 87, 2001), Giddings-Thomas(PRD 65, 2002) • Large Cross-Section. Because there is no small dimensionless constant, analogous to alpha, suppress the production of BHs. > • • 10^5 fb (M>5 Te. V, 10 D), 10 fb (M>10 Te. V, 10 D) Hard, Prompt, Charged Leptons and Photons Because thermal decays are flavor-blind. This signature has practically vanishing SM background. • Little Missing Energy. G. Landsberg SUSY 02 SUSY 08, Seong Chan Park

Around 2002 • Several different communities started talking about ‘Mini-Black holes’ • Particle physics, String theory, GR community even SF-community etc. . People got excited SUSY 08, Seong Chan Park

Seoul in 2002 SUSY 08, Seong Chan Park

Some people concerns if bh eats us : a survey by BBC SUSY 08, Seong Chan Park

Official comment by the CERN homepage: http: //public. web. cern. ch/Public/en/LHC/Safety-en. html SUSY 08, Seong Chan Park

BHs from cosmic rays • Anchordoqui-Feng-Goldberg-Shapere (PRD 2002) Pierre-Auger Ice Cube Etc. . are searching for these events. If the LHC can produce microscopic black holes, cosmic rays of much higher energies would already have produced many more. Since the Earth is still here, there is no reason to believe that collisions inside the LHC are harmful. SUSY 08, Seong Chan Park

Two major Progresses since 2002 Production Decay • BH production by collision proved. • Greybody factors of black hole in D>4 for brane fields with spin s=0, 1/2, 1 (i. e. for all the SM particles) obtained • • (b=0, D>4) Eardley-Giddings (2002) (b>0, D>4) Yoshino-Nambu (2003) • • ** Penrose (b=0, D=4) long ago Ida-Oda-SCP (2003, 2004, 2005, 2006) Duffy-Harris-Kanti. Winstanley(2005), Casals-Kanti. Winstanley (2006), Casals-Dolan -Kanti-Winstanley(2007) SUSY 08, Seong Chan Park

Production: Hoop Conjecture (Kip Thorne 1972) • “An imploding object forms a Black Hole when, and only when, a circular hoop with a specific critical circumference could be placed around the object and rotated. The critical circumference is given by 2 times Pi times the Schwarzschild Radius corresponding to the object’s mass. ” big energy in a small space, BH always appears!! I am a This is the hoop r = GM BH (M) SUSY 08, Seong Chan Park

It’s like putting an elephant into a freezer. . It is hard to do this. But once you can do it, you will have a BH. R= RBH(M) Mass=M SUSY 08, Seong Chan Park

Classical BH formation proved using two Aichelberg-Sexl shocks =t-z Eardley-Giddings 2002 Yoshino-Nambu PRD 66, 2003 Yoshino-Nambu PRD 67, 2003 =t+z Yoshino-Rychkov PRD 71, 2005 Boundary Value Problem: Setup: two particles (BHs) with • boost→∞, • mass→ 0, • energy: fixed. t z • Close Trapped Surface forms when b<b(max) (CTS=a closed spacelike surface on which the outgoing orthogonal null geodesics converge) • The Area Theorem : Classically the horizon area of the ultimate bh must be greater than the original CTS. i. e. BH really forms SUSY 08, Seong Chan Park

Latest result: bmax/rs Yoshino-Rychkov PRD 71, 2005 SUSY 08, Seong Chan Park

Another approach: (based on Hoop conjecture, taking angular momentum into account) SCP-Song 2001 Ida-Oda-SCP 2003 M/2 b M/2 Hoop Conjecture: Error ~3% (D=5)-17%(D=11) SUSY 08, Seong Chan This Park picture is essentially correct

Angular momentum Most of BHs are produced with “large” angular momentum! SUSY 08, Seong Chan Park

Signal: How will we know if we’ve seen one? • Black hole decays by emitting Hawking radiation. • We will see the radiated particles. • Smaller black holes are hotter and radiate more efficiently. (T~ Te. V, every SM particles can come out of the bh!) • Live short!! Life Time~10^-25 sec or shorter. • So please don’t worry about the possible destroy of the earth by mini black holes. SUSY 08, Seong Chan Park

Closer look: Hawking radiation • Here is the master equation S. Hawking (1975) T= surface gravity ~1/rh : Smaller bh is hotter : The probability is not equal to every particle but crucially depends on spin and angular mode. Anisotropic and nontrivial Hawking radiation is expected. We have to know this “greybody factor” to understand Hawking Radiation. SUSY 08, Seong Chan Park

Greybody factor Modification factor to take the curved geometry NH into account. = Absorption Probability of wave mode (s, l, m) Looks not black to me. It looks Grey! T SUSY 08, Seong Chan Park

Brief History of greybody factors for rotating BHs • Derivation of Teukolsky equation (Kerr) =Wave equation for general (s, l, m) wave for 4 D Kerr BH S. Teukolsky 1972, 1973) • Generalized to (D=4+n, Meyers-Perry) for brane fields Ida-Oda-SCP, PRD 67(2003) Solution to Teukolsky eq. / Greybody Factors (D=4, Kerr) : Analytic and Numerical methods were developed by Teukolsky-Press, Starobinsky, Unruh, Page in 1973 -1976 Analytic sol. (5 D), low energy limit, s=0, 1/2, 1: Ida-Oda-SCP, PRD 67(2003) Numerical (D>4), full energy, s=0 Ida-Oda-SCP PRD 71(2005) Result Presented at JGRG meeting by SCP (Dec. 2004, ar. Xiv: 0501210) Duffy-Harris-Kanti-Winstanley (ar. Xiv: 0507274, JHEP 0509, 2005) SUSY 08, Seong Chan Park

For s=0, D>4 Ida, Oda, SCP (s=1/2, 1, ar. Xiv: 0602188, PRD 73, 2006) Casals, Kanti, Winstanley (for s=1 only) (ar. Xiv: 0511163 JHEP 0602, 2006) Casals, Dolan, kanti, Winstanley (s=1/2) JHEP 0703, (2007) Finally!! Hawking radiation and its evolution : Hawking 1975, Page 1976 (4 D) Ida, Oda, SCP , PRD 73, 2006(D>4) including all the SM fields. Still s>1 modes (i. e. s=3/2, 2) missing Graviton part can be important when D>>4 Because of large number of helicity states SUSY 08, Seong Chan Park

Generalized Teukolsky eq. Ida, Oda, SCP PRD 67, 2003 • Meyers-Perry sol. (rating D>4 BH) • Define Null tetrad • Use ‘Newman-Penrose’ formalism, derive the equation • Turned out to be separable (Petrov Type-D) +angular part spin-weighted spheroidal harmonics +radial 2 nd order ODE with singular BCs. Believe me. This guy is tough! SUSY 08, Seong Chan Park

Schematic view of the greybody factor calculation Ida, Oda, SCP I, III Generalized Teukolsky Eq. Far from the Horizon Near the Horizon Sol (FF) Purely ingoing Sol (NH) Analytic or Numeric integration “Matching” Sol (whole space) Greybody factor (Absorption Probability) =[In]/[Out] SUSY 08, Seong Chan Park

D=5, S=1/2 Non-rotating Highly Rotating Greybody Number Energy Angular mom Ida, Oda, Park PRD 06’ SUSY 08, Seong Chan Park

D=10, s=1/2 Non-rotating Highly Rotating Greybody Number Energy Angular mom Ida, Oda, Park PRD 06’ SUSY 08, Seong Chan Park

D=5, s=1 Non-rotating Greybody rotating Highly Rotating Energy Angular mom Ida, Oda, Park PRD 06’ SUSY 08, Seong Chan Park

D=10, s=1 Greybody Non-rotating Highly Rotating Energy Angular mom Ida, Oda, Park PRD 06’ SUSY 08, Seong Chan Park

Evolution of BH f Obtained by integrating Hawking’s Formula with the calculated Greybody Factors. s SM M v 5 D J The full result (SM) is almost exactly described by ‘Vector’. • Vector emission is the most efficient way to extract angular momentum. • Large Gluon emission • 10 D similar SUSY 08, Seong Chan Park

Black Hole’s Life made simple Balding Phase (Production of BHs. Study “Dynamics” required. ) ? Spin Down Phase (Losing energy and Time angular momentum : 60 -80% Energy lost For D>4, to mostly gluons, anisotropic) Schwarzschild Phase (Losing Mass: 20 -40% energy, spherical, to every fields) Planck Phase (Remnant ? ? ? , Stringy study required ) SUSY 08, Seong Chan Park

New MC event generators are available. • Black. Max [ar. Xiv: 0711. 3012 ], Dai, Stojkovic, Issever, Rizvi, Tseng • Greybody factors for rotating BH implemented. • “Most realistic MC” simulation for bh events at the LHC. (N. B. )Yesterday (James Frost’s talk P 6 (on behalf of ATLAS)) I’ve learned that Black. Max has some bugs which should be removed. • CHARIBDIS ver. 2. is under development with Greybody factors for rotating BH. SUSY 08, Seong Chan Park

It seems we are more or less ready now but. . • There are still rooms to be improved (mostly theoretical) – Balding phase should be understood by dynamical simulation (most probably numerical) (cf) success of Bh-Bh merging process (this is important!!) – For D>>4, spin-2 graviton emission can be sizable. non-rotating case done for D>4 Cardoso, Cavaglia, Gualtieri JHEP 0602(2006) – BH final state: Full QG (string theory )calculation is required. – Many other issues : Chromosphere (Alig-Drees-Oda , Anchordoqui et. at. ), recoil(Stojkovic et. al), splitbrane (Stojkovic), etc – Unification of ‘convention’ required. SUSY 08, Seong Chan Park

Conventions • Planck scale (I would take PDG convention) • In the PDG convention

Physical quantities (PDG convention)

Two most important characteristics of BH signal • Large Entropy high Multiplicity. • Thermal radiation Flavor Blind. Typically, BH signals contains -Many jets -Statistically, N(e)=N(mu)=N(tau) SUSY 08, Seong Chan Park

Multi-’hard’-jet RS-1 (5 D), Pt>200 Ge. V Cross-Section [pb] 1000 Ge. V 100 1460 Ge. V 10 1960 Ge. V J. -H. Kim, SCP, S. Schumann (in preparation) SM 1 Black. Max 1. 0 0. 1 0. 001 0. 0001 1 E-05 Cross Section [pb] 1000 2 3 4 5 6 7 8 9 ADD (D=10), Pt>200 Ge. V 10 1000 Ge. V 100 1460 Ge. V 10 1964 Ge. V SM 1 0. 01 0. 0001 1 E-05 2 3 4 5 6 7 8 9 10 SUSY 08, Seong Chan Park

Multi-`harder’-jet Cross Section[Pb] 1000 ADD (D=10), Pt>500 Ge. V 100 1460 Ge. V 10 1960 Ge. V J. -H. Kim, SCP, S. Schumann (in preparation) SM 1 Black. Max 1. 0 0. 1 0. 001 0. 0001 1 E-05 cross-section[pb] 1000 2 3 4 5 6 RS-1 (D=5), Pt>500 Ge. V 7 8 1000 Ge. V 100 1410 Ge. V 10 1960 Ge. V SM 1 Again, there is Chromospher issue here. Dense jets look not really like Jets but fuzzy Chromospher. (Alig, Drees, Oda JHEP 0612 (2006) Anchordoqui , Goldberg PRD 67 (2003) ) 0. 1 0. 001 0. 0001 1 E-05 2 3 4 5 6 7 8 SUSY 08, Seong Chan Park

SM background –(Njet ≤ 6) Message from Steffen Schumann • For the background calculation I used Sherpa. • In my setup I combined matrix element calculations for 2, 3 and 4 jet production with parton showers attached. • The underlying method is referred to as CKKW (Catani-Krauss. Kuhn-Webber) and it avoids any double counting of jet configuration emerging from the matrix element or the parton shower. • However, in this approach the 5 th jet is produced from the parton shower, what means it may be underestimated and a full matrix element calculation could yield a higher rate here, but this is a very complicated computation and cutting edge with present day tools. • Anyhow, at some point we may want to include higher matrix elements yielding an improved background estimate for Njet>5. However, I do not expect the overall pattern to change and the difference between the QCD background and your multijet rates is significant. Wonderful Collaboration! SUSY 08, Seong Chan Park

Finally, some comments on Randall-Sundrum ‘Scale’ runs with the position: UV/IR hierarchy is explained by ‘Warping’: UV Ad. S 5 IR Y=d Y=0 Relevant energy scale for IR-localized scattering is M(d)~Te. V SUSY 08, Seong Chan Park

BH production on UV brane IR UV Ad. S 5 Y=0 Y=d We will not see this event since it is Mpl suppressed!

BH production at an arbitrary `y’ IR UV Ad. S 5 Y=0 Y=d

BH production on IR brane IR UV Ad. S 5 Y=0 *Note: (E/M) is scale invariant. *Cross section~1/Te. V^2. Y=d

RS 1 -orginal • All the SM particles lie on the IR brane. • They `feel’ strong gravity at the IR scale. • BH production rate ~1/Te. V 2 • The LHC as a BH factory IR UV Ad. S 5 Y=0 Y=d

Profile: RS 1 -bulk SM (See K. Agashe’s PL talk) IR UV Ad. S 5 Up, Down Gluon, W, Z, photon Zero-mode graviton Y=0 Higgs Top, bottom • Higgs, top, bottom as well as the longitudinal components of (W, Z) `feel’ the Te. V gravity. KK graviton, • The IR-tip of gluon, photon and KK gluon, the transverse components of Other KK states (W, Z) `feel’ the Te. V gravity. • Others (such as 1 st, 2 nd Y=d generation fermions) `feel’ the Planck –weak- gravity.

Closer look: bb+bbbar x 1 x 2 Suppressed by PDF!

Closer look: gg • Only `tip’ of the gluon contribute to the bh formation. • `Bulk’ contribution is exponentially suppressed. (negligible) ~1/70

Closer look: WL, ZL • By the equivalence theorem, the longitudinal components of the weak gauge bosons are effectively the unphysical Higgs. • Localized on the IR brane and feel the Te. V gravity. • Suppressed by d u WL WL d u WL

Production Cross section SCP 2008 Prelim. Thermal black hole production is highly suppressed. (See, Meade-Randall ar. Xiv: 0708. 3017) But still sizable to be detected.

• BH plays important role in BHs at ATLAS Heisenberg-’t Hooft picture. • BHs can be produced by scattering. (proved for D>4 cases in 2002 -2005) • Greybody factors for brane-fields are obtained for generic spin(<2), rotating, higher dimensional black holes in 2003 -2007 • MC gens are available (Black. Max, CHARIBDIS ver. 2. CATFISH. . ) • The LHC will test all these beautiful ideas and will show us results for Md~Te. V case soon. SUSY 08, Seong Chan Park

Backups SUSY 08, Seong Chan Park

Future/open issues • Dynamics of BH formation by ‘merging’ two particles will be important. We will be able to understand ‘balding phase’ • Hawking radiation to the Bulk graviton is still missing. It can be important if there are several large extra dimensions because of large number of angular momentum vectors. [2+n/2] • Blackhole-String transition (entropy, scattering), Information paradox etc. SUSY 08, Seong Chan Park

The legal defense fund site Seeking for donations to shut-down the LHC SUSY 08, Seong Chan Park

Conventions • Planck scale (I would take PDG convention) • I would follow the PDG convention

Thinking experiment: with E=10^6 Mp (E/2, 0, 0, E/2) (E/2, 0, 0, -E/2) Once the impact parameter is less than GE = 10^6/Mp, BH forms!! We cannot see behind the event horizon which is now million times larger than the Planck length. SUSY 08, Seong Chan Park

RS 1 -bulk SM • To address the hierarchy problem, we would put the Higgs boson on the IR brane (or in the vicinity of the IR brane) • For flavor problem, longevity of proton, better low energy data fit, etc. , we would put 1 st, 2 nd generations on the UV brane (or in the vicinity of UV brane). • 3 rd generation (b. R, t. L, t. R) may be on the IR brane. As a bonus, Large Yukawa for the top is also understandable due to the large overlap with the Higgs. • (Massless, zero-mode) Gauge bosons are `flat’ in the bulk. • (Probably) The most realistic set-up in RS 1 models.

Excellent agreement Yoshino-Rychkov 2005 n 1 2 3 4 5 6 7 RYN 1. 145 1. 333 1. 441 1. 515 1. 570 1. 613 1. 648 RIOP 1. 110 1. 170 1. 218 1. 262 1. 300 1. 334 1. 364 Ida, Oda, SCP 2003 Error ~3% (D=5)-17%(D=11) SUSY 08, Seong Chan Park