1 Aurelien Barrau LPSC-Grenoble (CNRS / UJF)

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MICROSCOPIC BLACK HOLESAS A PROBE FOR NEW PHYSICS
Aurélien Barrau Julien Grain , Gaelle Boudoul
Laboratory for Subatomic Physics and Cosmology
CNRS/IN2P3 Université Joseph Fourier
Grenoble, France
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I. Reminder on what PBHs have to say on
standard physics and cosmology
In 3 words quite a lot !
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PBH could have formed in the early Universe
Standard mass spectrum in a radiation
dominated era
Near critical phenomena
Bubbles collisions
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Hawking evaporation law
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constant term in the mass loss rate
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Antiproton individual emission
????M2Q2
Jet energy
MQ
Antiproton energy
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Mass spectrum
Convolution of the individual flux with the mass
spectrum
Initial spectrum
Today
Hawking evolution law
Initial mass of a black hole with lifetime age
of the Univers
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Cumulative source
Flux total
(1) ?
FLUX
(2) ?
(2)
(4)
(3) ?
(3)
(1)
(4) ?
Contribution essentielle Masses de trous noirs
entre 1012 et 5.1013 g
Énergie cinétique des antiprotons (GeV)
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Horizon size after inflation ?
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What about a QCD halo ?
Flux
Sans halo
Effet du halo
Antiprotons kinetic energy (GeV)
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Now, let the antiprotons propagate in the Milky
way
Drawing by D. Maurin
Maurin, Taillet, Donato, Salati, Barrau, Boudoul,
review article for Research Signapost (2002)
astro-ph/0212111
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Secondary antiprotons
p-p interactions
p-He, He-p and He-He interactions evaluated
with DTUNUC
Tertiaries
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Secondary antiprotons flux
Experimental data
Antiprotons flux
p-p component
p-He component
He-p component
He-He component
F.Donato, D. Maurin, P. Salati, A. Barrau, G.
Boudoul, R.Taillet Astrophy. J. (2001) 536, 172
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Top of atmosphere spectrum
A. Barrau, G. Boudoul et al., Astronom.
Astrophys., 388, 767 (2002)
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Upper limit on the PBH density
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Gamma-ray new upper limit
Taking into account the expected background from
(Pavlidou fields, ApJ 575, L5-8 (2002)) -
galaxies - quasars The EGRET gamma-ray flux at
100 MeV can be converted into (after integration
over redshift, evolution and absorption)
Omega_PBH lt 3.3 E 9 , improving by a factor 3
the Page MacGibbon upper limit. This limit is
nearly the same as with antiprotons but it relies
on very different physics and assumptions. Barrau
Boudoul, IRCR 2003 proc., asto-ph/0304528
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Cosmological consequences
HYPOTHESIS
Bump in the mass variance
Blais, Bringmann, Kiefer, Polarski Phys. Rev. D
67 (2003) 024024
Near critial phenomena
? 0.35
? 0.7
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Constraints on the PBH fraction ?
b
Contrainte Gravitationnelle
Contrainte due aux antiprotons
Mpeak (g)
Barrau, Blais, Boudoul, Polarski, Phys. Lett. B,
551, 218 (2003)
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Dark Matter
In the BSI framework, PBHs can be reconsidered as
CDM candidates In two different scenarii
A. Barrau, D.Blais, G.Boudoul , D.
Polarski Ann. Phys. 13, 115 (2004)
astro-ph/0303330

• If MRH is very large (greater than 1015 g) , PBHs
  become good candidates

Pour M H,e 10 -15 g p ? 6.5 ?10 -4
Experimental investigations possible above 1022
g by detection of gravitational waves
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A new hope for detection ?Antideuterons !
Secondary noise very small (kinematics)
A few events expected within the AMS detector
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Antideuteron source term
P0
Fragmentation function into antideuterons For a
given coalescence momentum P_0
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Antideuteron spectrum
New computation of the secondary flux
Evaporation
Window for detection
More events in the Low energy tail
Secondary anti(D)
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Parameters space L - P0 - ?
AMS excluded Zone in case of no-detection
P0 (MeV/c)
? (g/cm3)
L (kpc)
A. Barrau, G. Boudoul, et al. Astronom.
Astrophys. 398, 403 (2003)
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The AMS experiment
AMS-01 test fly in 1998
In 2007... AMS-02 on the ISS!
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Main physics topics for AMS

• Search for CDM
• Cosmic-rays
• Gamma-rays

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The AMS-02 spectrometer
TOF Hodoscopes(TOF dE/dX)
Cryostat Aimant SC(B 1T)
VETO
Trajectomètre(P dE/dX )
RICH(particule ID Alt27, Zlt26)
Calorimetre electrom.(ID em particules)
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Particles identification
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What can de done ?
Bouchet et al. Nucl. Phys A 688,417 (2001)
Antimatter
Cosmic-rays
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The RICHCounter
Number of photons ? Z2 Ring size ? V
radiator
mirror
PMTs
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II. New Physics with small black holes
In 3 words We will see In 3 more words Lets
hope !
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If PBHs dont exist, lets create them !
Hierarchy problem M_Planck gtgt E_EW Two
interesting ways to address this problem are -
Warped extra dimensional geometries
(RS) Randall Sundrum, Phys. Rev. Lett. 83,
3370 (1999) - Large extra dimension Harkani-Ham
ed, Dimopoulos Dvali, Phys. Lett. B 429, 257
(1998) If the spacetime structure is made of
numerous large dimensions Mp TeV if D10 and
V61fm6
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Generalized Schwarschild solution
Myers Perry, Amm. Phys. 172, 304 (1986)
Experimental detection
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Detection at the LHC
If the center of mass energy is gt E_Planck for
an impact parameter lt R_S ? Black Hole !
Dimopoulos Landsberg, Phys. Rev. Lett. 85, 499
(2001) Giddings Thomas, Phys. Rev. D 65, 056010
(2002)
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Dimensionality of space / new particles
Plot from Dimopoulos Landsberg
The dimensionality of space can be reconstructed
in most cases There is also a promising
possibility to search for new particles 100
GeV (e.g. a 130 GeV Higgs boson)
Landsberg, Phys. Rev. Lett. 88, 18 (2004)
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The Gauss Bonnet term
From General Relativity
To the Gauss-Bonnet action
- Phenomenological approach only ghost-free
quadratic correction - String theoretical
approach leading order in heterotic string models
Successfully used Cosmology (e.g. Deruelle et
al.) and BH Physics (e.g. Alexeyev et al.)
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Gauss Bonnet BH thermodynamics
Boulware Deser, Phys. Rev. Lett., 88, 3370
(1985) Cai, Phys. Rev. D, 65, 084014 (2002)
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Temperature behaviour
Non monotomic behaviour ? integration over time
Barrau, Grain, Alexeyev, submitted to Phys. Lett.
B (2003) hep-ph/0311238
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Flux computation
Multi-D grey body factors Taken at the
relativistic limit (Kanti et al.)
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ATLAS detection

• Mp 1 TeV
• Rs (and production rate) modified by the GB term

• Hard electrons and photons kept for determining
  the spectrum
• Energy resolution taken into account

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Results beyond the dimensionality of space
In any case, D And the GB coupling constant can
be reconstructed
Barrau, Grain, Alexeyev, Phys. Lett. B 584 (2004)
114
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Perspectives in this direction

• Improving the endpoint treatment
• Spinning black holes
• dS / AdS background ( CFT motivated )
• Cross section estimates

Alexeyev, Popov, Barrau, Grain in preparation
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EDGB cosmic black holes
Effects of Moduli fields, higher order curvature
corrections and time perturbations OK
Alexeyev, Barrau, Boudoul, Sazhin, Class.
Quantum Grav., 19, 4431 (2002)
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Metric functions revisited
Alexeyev, Barrau, Boudoul et al., Astronom.
Lett., 28, 7, (2002)
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Evaporation law in the Planck era
Hawking law
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Integrated relic flux
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Relics dark matter

• If MRH is small (smaller than 109 g) , stable
  relics become
• good canidates

Pour M rel M P 3.9 ?10 -4 lt p lt 7.1 ?10 -4
A. Barrau, D.Blais, G.Boudoul , D. Polarski,
Ann. Phys. 13, 115 (2003) astro-ph/0303330
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Constraints on SUGRA
Lower limit on the reheating temperature as a
function of the 100 MeV antideuteron flux
Barrau Ponthieu, Phys. Rev. D (2004) ,
hep-ph/0402187
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Gravitino mass
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Conclusion
Big black-holes are fascinating But small black
holes are far more fascinating !