taup conference @ sendai sep 11 2007 cosmic rays emitted by pbhs in a 5d rs braneworld
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TAUP Conference @ Sendai Sep 11 2007 Cosmic rays emitted by PBHs in a 5D RS braneworld. Yuuiti Sendouda (Yukawa Inst., Kyoto) with S. Nagataki (YITP), K. Kohri (Lancaster), K. Sato (Tokyo, RESCEU). Overview. Strategy. Cosmic-ray observations. Modified theories of - PowerPoint PPT PresentationTRANSCRIPT
TAUP Conference @ SendaiSep 11 2007
Cosmic rays emitted by PBHsin a 5D RS braneworld
Yuuiti Sendouda(Yukawa Inst., Kyoto)
withS. Nagataki (YITP), K. Kohri (Lancaster),
K. Sato (Tokyo, RESCEU)
Overview
StrategyCosmic-ray observations
Exotic models for Universe
Modified theories offormation and evaporationof PBHs
Now, Braneworld
What to do
Gamma-ray
10-4
10-3
10-2
10-1
0.1 1.0 10.0
Antip
roto
n flu
x [m
-2s-1
sr-1
GeV
-1]
Kinetic energy [GeV]
BESS 1995BESS 1997BESS 1998
CAPRICE1994CAPRICE 1998
totalsecondary
primaryprimary (4D)
I[ke
V cm
s
srke
V ]
E [keV]
l=l, F=, i=. l=l, F=, i=. l=l, F=, i=. l=l, F=, i=. l=l, F=, i=. l=l, F=, i=.
Too many PBHs would disturb standard cosmologyCosmic-ray spectra differently dependent on extra dimensionImplications to braneworld and PBHs
Antiproton
Braneworld and PBHs
RS2 Braneworld
ℓ . 0.1mm
[Randall & Sundrum (1999a,b)]
Bulk: Anti-de Sitter (<0)
Warped 5D metric
4D onlarge scales
5D gravitybelow ℓ
Tension >
+Matter T
Scales
Cosmology
Inflation
t
a(t)
ℓ
5D RD
Matter
2 distinctive epochs in RD
/ a-4
V ~ const. À
PBHs form
Friedmann eq.
Primordial Black HoleCarr (1975)
t = th
[Carr (1975), Guedens et al. (2002), Kawasaki (2004)]
> c
a(t)/k
H(t)-1 / t
k = aH
In RD: Jeans length ~ Hubble radius ~ Schwarzschild radius
BH
5D Schwarzschild (rS¿ℓ)
Accretion
(t)
Fcdt
Radiation accretes due to “slow” expansion in 5d era[Guedens et al., Majumdar (2002)]
Efficiency (0 < F < 1)
Brane
Mass growth
10-60
10-40
10-20
100
1020
1040
1010 1015 1020 1025 1030 1035 1040 1045
dnbh
/dM
bh,p
[g-1
pc-3
]
Mbh,p [g]
4Dl=0.1mm F=0
F=1
n=1.60
Primordial Mass Function
Scale invariant
“Tilt”
(Normalised at Ly Forest)
Accretion leadsto a huge increase
i: Initial PBH abundance
[YS et al., JCAP 0606 (2006) 003]Formula to calculate from inflationary perturbation
Hawking Radiation
S2
S3
D=5 (RS) D=4
¿
4D particles
KK graviton
Black body
Temperature and mass of a “critical” PBH lifetime being 13.7Gyr
Galactic Antiprotons[YS et al., PRD 71 (2005) 063512]
[Asaoka (2002)]
http://www.kek.jp/newskek/2002/mayjun/bess1.html
Observations
Excess?
Propagation
p
r
z
Solar wind
p_ p
_
Convection
B
¯
primarysecondary
Source• NFW density profile• QCD Jets treated with
PYTHIA
[Ginzburg, Khazan & Ptuskin (1980), Berezinskii et al. (1991)]
Diffusion eq
[Webber, Lee & Gupta (1992)]
(+Solar modulation)
Typical Flux
10-4
10-3
10-2
10-1
0.1 1.0 10.0
Antip
roto
n flu
x [m
-2s-1
sr-1
GeV
-1]
Kinetic energy [GeV]
BESS 1995BESS 1997BESS 1998
CAPRICE1994CAPRICE 1998
totalsecondary
primaryprimary (4D)
No effect from extra dim?
Positive detection?
Fitted to solar-minimum data
Extra-dim Dependence
E0
Flux
• Contribution only from those currently evaporating• But spectrum unchanged• Flux proportional to →decreasing function of ℓ
106 108 1010 1012 1014 1016 1018
PBH
mas
s sp
ectru
m d
n/dM
[arb
. uni
t]
PBH mass [g]
5D primordial5D present4D present
ℓ small
ℓ large
TH & GeV
Diffusion
Mass function (present-day)
M*
i is same
1018
1020
1022
1024
1026
1028
1030
1032
0.0 0.2 0.4 0.6 0.8 1.0
Size
of t
he e
xtra
dim
ensi
on l/
l 4
Accretion efficiency F
10-13
10-14
10-22
10-23
Effectively 4D
Constraints on i or ℓGi = Ex
tra d
im (ℓ
/l 4)
Accretion (F)
Large ℓ= weaker bound on PBH
×○
Density contrast G » 105
Extragalactic X/-ray Background
[YS et al., PRD 68 (2003) 103510]
10-1 100 101 102 103 104 105 106 107 108 109Photon Energy (keV)
0.1
1.0
10.0
100.0E2 d
J/dE
(keV2 /(c
m2 -s-ke
V-sr)
HEAO A2,A4(LED)
ASCA HEAO-A4 (MED)
COMPTEL
v
EGRET
http://cossc.gsfc.nasa.gov/docs/cgro/images/home/Cartoon_CGRO.jpghttp://heasarc.gsfc.nasa.gov/Images/heao1/heao1_sat_small2.gif
[Strong et al. (2003)]
keV GeVMeV
Observations
SpectrumSuperposing blackbody spectra
log E0
log I
TH/(1+z)
/ Mbh/TH
I / nbh/(1+z)3 ℓ1/2 Mbh3/2
Lifetime=Cosmic age
Heavy (still exist)Light (already died)
Sensitive to extra dimension I » U0/E0
I[ke
V cm
s
srke
V ]
E [keV]
l=l l=l
l=l
i= , F=., f=
(b)
I[ke
V cm
s
srke
V ]
E [keV]
i= , F=, f= l=ll=ll=l
4D
I[ke
V cm
s
srke
V ]
E [keV]
l=l
l=l
l=l
i= , F=., f=
(a)
ℓ ↗Temp ↘ 4
D
Extra-dim Dependence
F=1
F=0
F=0.5
Potential to detect the extra dimAccretion takes important role
0.1mm
Safe
Dangerous
1018
1020
1022
1024
1026
1028
1030
1032
0.0 0.2 0.4 0.6 0.8 1.0
l/l4
F
10-23
10-24
10-25
10-26
10-27
10-28
10-29
10-30
10-31
Effectively 4D
ConstraintsEx
tra d
im (ℓ
/l 4)
Accretion(F)
Small ℓweakensbound
Large ℓ weakens upper bound on PBH
×○
i =
Conclusions
1018
1020
1022
1024
1026
1028
1030
1032
0.0 0.2 0.4 0.6 0.8 1.0
Siz
e of
the
extra
dim
ensi
on l/
l 4
Accretion efficiency F
10-26
10-27 10-28
Effectively 4DPhoton
Antiproton
(G = 105)
i > 10-27
Always i<10-28
Always i =10-27 » 10-
28
Cooperative
As the constraint on ℓComparison
Firm Limit on Inflation
10-6
10-5
10-4
10-3
10-2
10-1
100
100 105 1010 1015 1020 1025 1030
Pow
er s
pect
rum
PR
c
1/2
Comoving scale k -1 [m]
F=1 F=0 4D
pbar
10-6
10-5
10-4
10-3
10-2
10-1
100
100 105 1010 1015 1020 1025 1030
Pow
er s
pect
rum
PR
c
1/2
Comoving scale k -1 [m]
F=1 F=0 4D
WMAPLy
Seljak et al. 200510-6
10-5
10-4
10-3
10-2
10-1
100
100 105 1010 1015 1020 1025 1030
Pow
er s
pect
rum
PR
c
1/2
Comoving scale k -1 [m]
F=1 F=0 4D
WMAPLy
10-6
10-5
10-4
10-3
10-2
10-1
100
100 105 1010 1015 1020 1025 1030
Pow
er s
pect
rum
PR
c
1/2
Comoving scale k -1 [m]
F=1 F=0 4D
WMAPLy
10-6
10-5
10-4
10-3
10-2
10-1
100
100 105 1010 1015 1020 1025 1030
Pow
er s
pect
rum
PR
c
1/2
Comoving scale k -1 [m]
F=1 F=0 4D
WMAPLy
10-6
10-5
10-4
10-3
10-2
10-1
100
100 105 1010 1015 1020 1025 1030
Pow
er s
pect
rum
PR
c
1/2
Comoving scale k -1 [m]
F=1 F=0 4D
WMAPLy
10-6
10-5
10-4
10-3
10-2
10-1
100
100 105 1010 1015 1020 1025 1030
Pow
er s
pect
rum
PR
c
1/2
Comoving scale k -1 [m]
F=1 F=0 4D
pbar
10-6
10-5
10-4
10-3
10-2
10-1
100
100 105 1010 1015 1020 1025 1030
Pow
er s
pect
rum
PR
c
1/2
Comoving scale k -1 [m]
F=1 F=0 4D
WMAPLy
Seljak et al. 200510-6
10-5
10-4
10-3
10-2
10-1
100
100 105 1010 1015 1020 1025 1030
Pow
er s
pect
rum
PR
c
1/2
Comoving scale k -1 [m]
F=1 F=0 4D
WMAPLy
10-6
10-5
10-4
10-3
10-2
10-1
100
100 105 1010 1015 1020 1025 1030
Pow
er s
pect
rum
PR
c
1/2
Comoving scale k -1 [m]
F=1 F=0 4D
WMAPLy
10-6
10-5
10-4
10-3
10-2
10-1
100
100 105 1010 1015 1020 1025 1030
Pow
er s
pect
rum
PR
c
1/2
Comoving scale k -1 [m]
F=1 F=0 4D
WMAPLy
10-6
10-5
10-4
10-3
10-2
10-1
100
100 105 1010 1015 1020 1025 1030
Pow
er s
pect
rum
PR
c
1/2
Comoving scale k -1 [m]
F=1 F=0 4D
WMAPLy
Curv
atur
e pe
rtura
batio
n
n=1.28 1.35 1.39
1018
1020
1022
1024
1026
1028
1030
1032
0.0 0.2 0.4 0.6 0.8 1.0
Size
of t
he e
xtra
dim
ensi
on l/
l 4
Accretion efficiency F
10-26
10-27 10-28
Effectively 4DPhoton
Antiproton
10-4
10-3
10-2
10-1
0.1 1.0 10.0
Ant
ipro
ton
flux
[m-2
s-1sr
-1G
eV-1
]
Kinetic energy [GeV]
BESS 1995BESS 1997BESS 1998
CAPRICE1994CAPRICE 1998
totalsecondary
primaryprimary (4D)
Best-fit
If the sub-GeV pbar excess is real, allowed parameter region is very restrictive
i » 10-27
¼ 0.05
pbar visible
invisibleℓ . 1 pm
Braneworld disfavoured?Bess-Polar 2007 should give a hint
Being Speculative