aspen winter 2003 conference on particle physics: at the frontiers jan 19-25 2003
DESCRIPTION
Aspen Winter 2003 Conference on Particle Physics: At the Frontiers Jan 19-25 2003. BLACK HOLES & GRAVITONS AT HECs. Maria Spiropulu Enrico Fermi Institute UofC. What ?. A singular classical object (black hole) - PowerPoint PPT PresentationTRANSCRIPT
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
Aspen Winter 2003 Conference on Particle Physics: At the Frontiers Jan 19-25 2003
BLACK HOLES
&GRAVITONS
AT HECs
Maria SpiropuluEnrico Fermi Institute
UofC
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
What ?
• A singular classical object (black hole)• A massles spin 2 particle whose long-
wavelength interactions are described by general relativity (graviton)
produced in high energy collisions!!
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
It is a matter of scale and geometry
• From contact interaction to a gauge boson: the GFE2 behavior was tamed at short length scales
• From gauge theory to string theory the GNE2 behavior seems to be tamed at even shorter length scales– With this comes a change in how we perceive
spacetime geometry and dynamics: eg. Extra dimenisons
– The Standared Model, Supersymmetry and the Kaluza-Klein theory under one umbrella
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
Models of extra dimensions
• Large compact extra dimensions (ADD type)
• Warped extra dimensions (RS type)
• inverse TeV extra dimensions (Ignatios type)
• (most) all hybrids and combinations of above
• Fat branes, skiny branes, solid branes, soft branes, no branes, curved bulk, flat bulk, supersymmetric bulk, gravity in the bulk, gauge fields in the bulk, no gauge fields in the bulk, fermions in the bulk, no fermions in the bulk, right handed neutrinos in the bulk, &tc
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
As JoAnne taught me
Only high Tc superconductivity you cannot solve with extra dimensionseverything else YES
• EWKB• hierarchy problem• SUSY Breaking• flavor Breaking• neutrino masses• proton decay suppression• Grand Unification• the cosmological constant• ...
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
Going down, a step at a time
• Bring down the Planck • to the GUT• to the TeV scale • in string theory with
extra dimensions,• the 5th slightly bigger,• and then even bigger • and then more of them
huge• (eg Kaluza-Klein,
Witten-Horava, Lykken, ADD, RS)
MPlanck, Mstring, MGUT,M*, MD ,M?, MEWK
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
Black Holes• Initial current work by
Banks+Fisckler(hep-th/9906038), Dimopoulos+Landsberg(hep-th/0106295), Giddings+Thomas(hep-ph/0106219)
• Rizzo(hep-ph/0201228),Chang (hep-ph/0205033)
• goes back to early work by D’Eath and Payne [mosre recent Eardley+Giddings gr-qc/0201034, Yoshino+Nambu gr-qc/0209003]
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
Black Hole, mass, radius, entropy
• A gravitational potential well whose gravitational potential energy is greater than the energy required to get out of the well = Black Hole
• GNMBH (RS)-1 = 1 GNMBH= RS
– the radius of a black hole mass of the black hole
• Entropy SBH~black hole area~RS2~MBH
2
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003High Energy vs High
Entropy• At higher and higher energies the
production of a class of objects with higher and higher entropy will suppress the production of everything else…
• or, iow above the energy scale where BH can be produced, ONLY BH will be produced
• what is that energy scale? Is it possible that LHC turns on and we can only do diffraction particle physics and the rest is all black holes? And stringy stuff?
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
String State Entropy • The mass of an Nth
mode string state is M2
string= N MS2
• and the associated string state entropy Sstring=Mstring/MS
• Sstring~Mstring, SBH~M2BH
• scales: Planck, String, Effective Planck ?
• MBHmin > MS, M*
SBH
Sstring
energy
S
?
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
BH domination• Conservatively BH production should
dominate for MBH~(5-10)M*
• cross section: ij BH = F(s) R2S
• F(s)<1 (not all energy gets trapped, geometrical considerations for spherical formation etc)
• arguments for suppression(Voloshin et al) but overall domination(Rizzo, D’Eath and Payne etc)
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
BH Production• Total cross section
for BH formation eg.• for n=2…7 by
proton proton scattering at LHC (14 TeV). Assume M*=1 TeV and
• threshold for Black Hole formation at MBH,min= 3 M*=3 TeV
Cavaglia et all/hep-ph/0210296
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
With or Without suppressionsRizzo hep-ph/0201228
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
BH decay• Hawking radiation with
1/T=dS/dE~MBH~RS
• Decay like a point source into brane modes and bulk modes.
• Gravity couples democratically so expect final state with GaugeBoson:Quark:Leptons= 29:72:18 (although recent work by Tao Han et al points to modification depending on the brane configuration)
• High Multiplicity stuff with a lot of jets until the BH shrinks and stringy modes show up
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003LHC maybe a Black
Hole factoryDimopoulos & Landsberg
# of BH @LHC in e or decay channels as a function of BH massShadow=2…7 extra dimensions, -- total SM bgr, … Z(ee)+X{even Higgs and SUSY discovery in the BH decays, the dimensionalityof space &tc…]
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
Oven Fresh (the gangs of arizona)
Mocioiu,Nara,Sarcevic hep-ph/0301073
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
(brief) Model Description & Parameters
• ADD-type– # of extra dimensions,
– effective Planck scale,
MD
• RS-type – curvature of AdS5, k
– extent of 5th dimension, R
nnPl
nPlanck MRM
2
)4(2 ~
nnPl
nPlanck MRM
2
)4(2 ~
MPl (8)-½ e-kR MPl (8)-½ e-kR
0 R
AdS5
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
(brief) Model Description & Parameters
• ADD– mn= (n2/R2)½ n=(n1,n2,…n)
– evenly spaced KK states
– set MD=1 TeV • =1 R 1011 m • =2 R~0.4 mm 1/R~5 10-4
eV• =4 R~10-5 mm 1/R~20 keV• =6 R~30 fm 1/R~7 MeV
• RS– mn=kxn(8) ½(MPl)-1 xn
denotes the roots of the first-order Bessel function
– not evenly spaced KK states
– set =1 TeV • kR ~ 11-12
• m1~TeV order
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
Collider Signatures• KK-Graviton Emission., KK-Graviton
Exchange, KK-Graviton Resonant Production, KK-Boson Resonant production
• Monojets+Missing Energy, Dijets+Missing Energy, Monophotons+Missing Energy, Diphotons+Missing Energy, Dijets, Dileptons, Dileptons+missing energy, Diphotons, Dibosons
• Results/Studies LEP, TeVI, TeVII, LHC, NLC/TESLA
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003High Mass Dijet Event
Run 152507 event 1222318Dijet Mass = 1364 GeV (corr)cos * = 0.30z vertex = -25 cm
J1 ET = 666 GeV (corr)
583 GeV (raw)
J1 = 0.31 (detector)= 0.43 (correct z)
J2 ET = 633 GeV (corr)
546 GeV (raw)
J2 = -0.30 (detector)= -0.19 (correct z)
Corrected ET and mass are preliminary
(thanks to Rob Harris)
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
Backgrounds
• Z + jets• W + jets• W e + jets• QCD• Dibosons• tt, single top
– STRATEGY: Normalize wherever possible using data
normalize using Zee data normalize using Zee data,
SM W/Z ratio and universality
normalize using dijet data normalize using theory
cross section
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
Backgrounds
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
Zee: standard(izable) candle
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
Zee: standard candle
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
Eg. Graviton Emission
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
Eg Graviton exchange
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
Signal topology
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
Signal topology
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
two events are real CDF data and one is graviton simulation; Can you pick the graviton?
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
Monojet+missing energy: DØ limit
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
n 14 TeV100 fb-1
14 TeV1000 fb-1
28 TeV100 fb-1
28 TeV1000 fb-1
2 9 12 15 19
3 6.8 8.3 11.5 14
4 5.8 6.9 10 12
Ian Hinchliffe
Monojet + missing energy: LHC reach
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
Davoudiasl, Hewett,Rizzo
1500 GeV KK graviton/ its tower of states at LHC
500 GeV KK gravitonand neutral gauge boson excitations
e+e-
500 GeV KK graviton/ its tower of states at a lepton collider
RS phenomenology
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
A spin 2 graviton: Can we tell?
1.5 TeV gravitonin Randal Sundrumat LHC
Large Hadron Collider (CERN, 2006)
new accelerators for new physics
Linear Collider (?,~2012)
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003
Plethora of new models that involve extra dimensions
Use Extra Dimensions Geomerty to solve:EWKBhierarchy problemSUSY Breakingflavor Breakingneutrino massesproton decay supressionGrand Unificationthe cosmological problem
More ideas are being explored
Mari
a S
pir
op
ulu
, A
sp
en
, Ja
n 2
1
2003