1 aurelien barrau lpsc-grenoble (cnrs / ujf) microscopic black holes as a probe for new physics...

1 Aurelien Barrau LPSC-Grenoble (CNRS / UJF)

MICROSCOPIC BLACK HOLESAS A PROBE FOR NEW

PHYSICS

Aurélien BarrauJulien Grain , Gaelle Boudoul

Laboratory for Subatomic Physics and CosmologyCNRS/IN2P3 – Université Joseph Fourier – Grenoble, France


I. Reminder on what PBHs have to say on “standard”

physics and cosmology

In 3 words : quite a lot !


PBH could have formed in the early Universe

2

2

2

2

1)(

eP

2

2

2

1

)(

c

c

edPi

* Standard mass spectrum in a radiation dominated era

PBHcBH

BHBH MM

MMn

2*

*

)2(

* Near critical phenomena * Bubbles collisions

kcBHM )'(


Hawking evaporation law

sch

Qs

ehdQdt

Nd

24/

2

)1(2T

Q

eQMdQdt

Nd 22

2

kGM

hcT

16

3

2

)(

M

M

dt

dM

stGeVTgM

stGeVTgM

11010

10101049

21116


“constant” term in the mass loss rate


Antiproton individual emission

dQdE

EQdge

h

TQ

dEdt

NdpjskT

Q

j EQ

jj

p),(

)1(),( __

1

2

2

Jetenergy

Antiprotonenergy

MQ

M2Q2


Mass spectrum

dMdMdV

z)n(rd

dEdT

E)N(Md=E)z(rq prim ,,

,,22

dM

dM

dM

dn=

dM

dn init

init*

2 ↔ MMMdM

dn

Convolution of the individual flux with the mass spectrum

Initial spectrum

Today :

3/13 3 )mαt(M init Hawking evolution law gM 1410 5

Initial mass of a black hole with lifetime ~ age of the Univers


Cumulative source

(1)

(2)

(3)

(4)

g][MM Pl

12,10

g]g[M 1312 10 ,10

g]g[M 1313 10 5 ,10

gM 1310 5

Contribution essentielle:Masses de trous noirs entre

1012 et 5.1013 g

FL

UX

Énergie cinétique des antiprotons (GeV)

(1)

(2)

(3)(4)

Flux total


Horizon size after inflation ?

tt

MM

Pl

Pl

8

1

22

1

3.0RH

PlRH T

Mgt

Flu

x

Antiprotons kinetic energy (GeV)


What about a QCD halo ?

0

2T

E

edEdt

Nd

)1(6.8)(

GeV

TTP

Sans halo

Effet du halo

Flu

x

Antiprotons kinetic energy (GeV)


Now, let the antiprotons propagate in the Milky way…

Maurin, Taillet, Donato, Salati, Barrau, Boudoul, review article for “Research Signapost” (2002) [astro-ph/0212111]

Drawing by D. Maurin


Secondary antiprotons

),,(1

),0,()(2),0,()(22

2

_ EzrNr

rrzz

Kz

VErNzhErqzh cine

p

')',(4)'(),(_

dEErnpHEpdE

dErq

Threshlod

pHISM

),(')',(''),( ____

__

ErNvnEdEErNvnEEdE

dErq

pH

XpHpE

pH

XpHp

p-p interactions :

p-He, He-p and He-He interactions : evaluated with DTUNUC

Tertiaries :


Secondary antiprotons fluxExperimental data

Antiprotons flux

p-p component

He-He component

He-p componentp-He component

F.Donato, D. Maurin, P. Salati, A. Barrau, G. Boudoul, R.TailletAstrophy. J. (2001) 536, 172


Top of atmosphere spectrum

A. Barrau, G. Boudoul et al., Astronom. Astrophys., 388, 767 (2002)


Upper limit on the PBH density

33433 .105105 cmg )3(104 351 kpcLcmn 9104


Gamma-ray new upper limitTaking 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 < 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]


Cosmological consequences

Bump in the mass variance

Near critial phenomena

0.35

Blais, Bringmann, Kiefer, PolarskiPhys. Rev. D 67 (2003) 024024

cHMM 0.7

HYPOTHESIS:


Constraints on the PBH fraction

ContrainteGravitationnelle

Contrainte due aux

antiprotons

Mpeak (g)

Barrau, Blais, Boudoul, Polarski, Phys. Lett. B, 551, 218 (2003)


Dark Matter

In the BSI framework, PBHs can be reconsidered as CDM candidatesIn two different scenarii

Experimental investigations possible above 1022 gby detection of gravitational waves

If MRH

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

Pour M H,e

=gp

3

,

15

2

6

min

, 10

2

103.5

eHPBH

COBEH

MLWp

A. Barrau, D.Blais, G.Boudoul , D. PolarskiAnn. Phys. 13, 115 (2004) [astro-ph/0303330]


A new hope for detection ?Antideuterons !

Secondary noise very small (kinematics)

A few events expected within the AMS detector


Antideuteron source term

Fragmentation function into antideuteronsFor a given coalescence momentum P_0

D

dQdE

PEQdge

h

TQ

dEdt

Ndj

DjjskTQEQ

j

jD

),,()1(

),( 012/2

n

pP0


Antideuteron spectrum

Evaporation

Secondary anti(D)

Window for detection

New computationof the secondaryflux

More events in theLow energy tail


Parameters space {L - P

0 -

L (kpc)g/cm 3)

P0 (

MeV

/c) AMS excluded

Zone in case ofno-detection

A. Barrau, G. Boudoul, et al. Astronom. Astrophys. 398, 403 (2003)


The AMS experiment

AMS-01: test fly in 1998 In 2007... AMS-02 on the ISS!


Main physics topics for AMS

•Search for CDM

•Cosmic-rays

•Gamma-rays

•Search for antimatter


TOFHodoscopes(TOF & dE/dX)

Cryostat & Aimant SC

(B = 1T)

Trajectomètre(P & dE/dX )

Calorimetre electrom.(ID em particules)

RICH(particule ID

A<~27, Z<~26)

TRDe+/p & e-/p

Discrim P<300GeV/c

-

The AMS-02 spectrometer

VETO

3m


Particles identification


What can de done ?

Antimatter Cosmic-rays

Bouchet et al.Nucl. Phys A 688,417 (2001)


Calorimetre

PMTs

radiator

mirror

The RICHCounter

Number of photons Z2

Ring size V


II. New Physics with small black holes

In 3 words : We will see…In 3 more words : Let’s hope !


If PBHs don’t exist, let’s create them !

Hierarchy problem : M_Planck >> 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 dimensionHarkani-Hamed, Dimopoulos & Dvali, Phys. Lett. B 429, 257 (1998)

If the spacetime structure is made of numerous large dimensions : Mp ~ TeV if D=10 and V6=1fm6


Generalized Schwarschild solution

)3/(1

22

4

0 )2(

)2(4

D

DPlD

D

Jh MD

Mr

h

JH r

DT

43

0

)exp( )3/()2( DDMNS Experimental detection

Myers & Perry, Amm. Phys. 172, 304 (1986)


Detection at the LHC

Dimopoulos & Landsberg, Phys. Rev. Lett. 85, 499 (2001)Giddings & Thomas, Phys. Rev. D 65, 056010 (2002)

If the center of mass energy is > E_Planck for an impact parameter < R_S

Black Hole !


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)


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.)


Gauss Bonnet BH thermodynamics

Boulware & Deser, Phys. Rev. Lett., 88, 3370 (1985)Cai, Phys. Rev. D, 65, 084014 (2002)


Temperature behaviour

Non monotomic behaviour integration over time

Barrau, Grain, Alexeyev, submitted to Phys. Lett. B (2003) [hep-ph/0311238]


Flux computation

Multi-D grey body factorsTaken at the relativistic limit

(Kanti et al.)


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


Results : beyond the dimensionality of space

Barrau, Grain, Alexeyev, Phys. Lett. B 584 (2004) 114

In any case, D And the GB coupling constant can be reconstructed


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


EDGB cosmic black holes

2

24

4

2

RRRRRS

SeRgxdS

ijij

ijklijklGB

GB

)sin( 222222

22 ddrdrdtds

Effects of Moduli fields, higher order curvature corrections and time perturbations OK

Alexeyev, Barrau, Boudoul, Sazhin, Class. & Quantum Grav., 19, 4431 (2002)


Metric functions revisited

hhr 64inf

...)()(

...)(

...)()(

22100

10

221

hh

h

hh

rrrr

rrss

rrdrrd

Alexeyev, Barrau, Boudoul et al., Astronom. Lett., 28, 7, (2002)


Evaporation law in the Planck era

M

M

r

r

out

in

dHr

drS Im)Im(

3min )()Im( MMkS

Hawking law


Integrated relic flux

tMGM

ckMM

Pl344

min

25

min 8

9

E

tMGM

ckEtkMMcG

dEdt

Nd

PlPl 344

min

6542

3

2

510min

2

15152

2510

2

32

8

9

9

8

3

32

max

02

222

4

)(tan)(),1(

R

univ dRR

RR

c

RtzE

dEdt

NdF

12117101.1 srmsJF


Relics dark matter

If MRH

is small (smaller than 109 g) , stable relics becomegood canidates

A. Barrau, D.Blais, G.Boudoul , D. Polarski, Ann. Phys. 13, 115 (2003) [astro-ph/0303330]

Pour M rel

=M P

3.9 10 -4 < p < 7.1 10 -4

3

,

152

2

6

min

, 10

2

100.8

eHp

rel

PBH

COBEH

MM

MLWp


Constraints on SUGRA

Lower limit on the reheating temperature as a functionof the 100 MeV antideuteron flux

Barrau & Ponthieu, Phys. Rev. D (2004) , hep-ph/0402187


Gravitino mass


Conclusion

Big black-holes are fascinating

But small black holes are far more fascinating !

1 aurelien barrau lpsc-grenoble (cnrs / ujf) microscopic black holes as a probe for new physics...

Documents

barrau boudoul

maurin slide

france slide

univers slide

flux total slide

pbh density slide

p component p

astoph0304528 slide