Examples of Science

1
Examples of Science

• Generic fluxes associated with cosmic rays
• Astrophysics gamma ray bursts
• Particle physics cold dark matter search

2
Natures Particle Accelerators

• Electromagnetic Processes
• Synchrotron Emission
• Eg a (Ee/mec2)3 B
• Inverse Compton Scattering
• Ef (Ee/mec2)2 Ei
• Bremmstrahlung
• Eg 0.5 Ee
• Hadronic Cascades
• p g -gt p po -gt e n g
• p p -gt p po -gt e n g

3
High Energy Gamma-Ray Astrophysics
Typical Multiwavelength Spectrum from High Energy
g-ray source
Energy Emitted
Photon Energy
4
Spinning Neutron Star Fills Nebula with Energetic
Electrons gt Synchrotron Radiation and Inverse
Compton Scattering
5
Active Galactic Nuclei

• Massive Black Hole Accelerates Jet of Particles
  to Relativistic Velocities
• gt Synchrotron Emission and Inverse Compton
  and/or Proton Cascades

6
Challenge I Acceleration
shock velocity n
R
(V e F b v/c)
B
n

• boosted energy
• from cosmic accelerator

7
Energy in extra-galactic cosmic rays 3x1037
erg/s or 1044 erg/yr per (Mpc)3
3x1039 erg/s per galaxy 3x1044 erg/s per active
galaxy 2x1052 erg per gamma ray burst
1 TeV 1.6 erg
8
brightest known sources match IF equal energy in
protons and electrons (photons)

• AGN (steady)
• G few requires Lgt1047 erg/s
• Few, brightest AGN
• GRBs (transient)
• G 300 requires Lgt1051 erg/s
• Average Lg1052 erg/s
• equal energy in neutrinos?

9
some definitions

• flux F dN/dE (particles cm-2 s-1)
• fluency f E dN/dE (erg cm-2 s-1)
• luminosity L f x 4pd2 (erg s-1)

10
Point Sources
Signal
Background (atmos. ns)
For 10 -- 1000 TeV
11
Cosmological sources
Most Powerful Cosmological sources AGN
(Steady) GRBs (100s transient)

1. 1 km2 detector
2. Same UHE CR suspects

12
Challenge II Propagation (GZK)

• gt1020eV proton lElt100 Mpc
• Bright AGN (Radio galaxies)- too far ?
• GRBs ?
• Does the spectrum support GZK?

13
Model
EW 95

• Flys Eye fit for Galactic heavy (lt1019eV)
• JGE-3.50
• X-Galactic protons
• Generation spectrum (shock
  acceleration)
• Generation rate
• Redshift evolution SFR

14
Model vs. Data
Bahcall EW 03
X-G Model
Ruled out 7s
5s
15
Conclusions are Robust
16
CR Conclusions

• Yakutsk, Flys Eye, HiRes Consistent with
• XG protons
  GZK
• Robust Consistent with GRB model predictions
• AGASA (25 of total exposure)
• Consistent below 1020eV
• Excess above 1020eV 2.2/-0.8 8
  observed
• New source/ New physics/ 25
  energy
• Local inhomogeneity
  over-estimate
• Stay tuned for Auger (Hybrid)

??
17
diffuse flux
flux velocity x density flux c/4p x
density, for isotropic flux --gt in energy
density E dN/dE dE c/4p x rE E dN/dE A
E -g cm-2 s-1 sr-1 (g -1)
18
diffuse background
Signal
Background (atmos. ns)
Waxman-Bahcall bound
1km2 detector --gt 50 events/yr
19
n Flux Bound

• Observed JCR(gt1019eV)
• For Sources with tgp lt 1
• Strongest know z evolution (QSO, SFR) collect
  ns beyond GZK

EW Bahcall 99, Bahcall EW 01
20
tgp for known sources
eg
p
e
n
e-
eg
ep
21
Antares
Nemo
22
Neutrinos from GRB an example
23
Gamma-ray Bursts
M on 1 Solar Mass BH
Relativistic Outflow
G300
e- acceleration in Collisionless shocks
e- Synchrotron MeV gs Lg1052erg/s
Meszaros, ARAA 02
24
Gamma Ray Burst

• Photons and protons
• coexist in internal
• shocks
• External shocks

25
Correlations to BATSE Gamma Ray Bursts ?
1969
BATSE 1991- May 2000
1997
26
NUMEROLOGY

• Lg 1052 erg/s
• R0 100 km
• Eg 1 MeV
• ?t 1-10 msec
• 300
• tH 1010 years
• dE/dt 4x1044 erg Mpc-3yr-1
• Pdetected 10-6 En0.8 (in TeV)
• spg 10-28cm2 for pg?np
• lt xp ? p gt 0.2

27
GRB1
FRAMES
Fireball Frame
Observer Frame
DR
R
R'
v
c
g 102 - 103 E g E' 1 MeV R g R'
d
DR cDt R0 with R0 R' (t 0)
observed 1 msec
28
grb kinematics

• R0 100 km
• cos ? v/c

-
v2 __ c2
R
q
g 1- -1/2
v
-
102 - 103
q
c
DR __ c
1 _ c
Dt (R - Rcosq)
R __ 2c
v __ c
R __ c
v2 __ c2
R __ 2c

1 __ g2
-
( 1 - )
(1- )
-

• ?Dtobs
• ?DEobs g E

-
29
GRB3
Pion (neutrino) production when protons and
photons coexist
neutrinos
pg np
gamma rays
np0

Ep gt 1.4 x 104 TeV
m2D - m2p _________ 4E'g
E'p gt
_
_
En 1/4 lt xp p?gt Ep 1/20 Ep 0.7 PeV
30
Fraction of GRB energy converted into pion
(neutrino) production
GRB4

• f p lt?x p p gt 15
• l-1pg ng spg

DR' ___ lpg
_
e
g (Lg)
synchro/ICompton
fireball
p
n
pions
(LCR)
31
GRB2
Photon Density in the Fireball
LgDt/g ______ 4pR'2DR'
U'g ___ E'g
ng
E'g ___ g
R' g2cDt
DR' gcDt
note for g 1 (no fireball) optical depth of
photons is topt
R0ngsTh 1015
R0 __ lTh
32
GRB 5
Neutrino flux from GRB fireballs
U? ___ E?
1 ___ E?
fn (1/2 f? tH
)
c __ 4p
c __ 4p
dE __ dt
_
charged p only
LCR
Lg
Nevents Psurvived Pdetected fn 20 km -2 yr -1
_
33
GRB 6
NUMEROLOGY

ltxp -gt pgt 1/5 spg 10-28cm2 tH 1010
years dE/dt 4x1044 erg Mpc-3yr-1 Pdetected
10-6 En0.8 (in TeV)
Lg 1052 erg/s R0 100 km Eg 1 MeV ?t 1-10
msec g 300
34
Search for HE n from GRB
35
Correlations to GRB
Background cuts can be loosened considerably ?
high signal efficiency
88 BATSE bursts in 1997
Combined data give sensitivity prediction!
36
Marriage of Astronomy and Physics

• Astronomy new window on the Universe!
• You can see a lot by
  looking
• Physics
• search for dark matter
• search for topological defects and cosmological
  remnants
• search for monopoles
• measure the high-energy neutrino cross section
• (TeV-scale gravity?)
• cosmic ray physics 150 atmospheric nus/day
• array with EeV sensitivity
• test special and general relativity with new
  precision

37
Relic density simple approach

• Decoupling occurs when
• G lt H
• We have

38
The MSSM general

• The Lightest Supersymmetric Particle (LSP)
• Usually the neutralino. If R-parity is
  conserved, it is stable.
• The Neutralino c
• Gaugino fraction

• 1. Select MSSM parameters
• 2. Calculate masses, etc
• 3. Check accelerator constraints
• 4. Calculate relic density
• 5. 0.05 lt Wch2 lt 0.5 ?
• 6. Calculate fluxes, rates,...
• Calculation done with

http//www.physto.se/edsjo/darksusy/
39
The mc-Zg parameter space
Gauginos
Mixed
Higgsinos
40
WIMP search strategies

• Direct detection
• Indirect detection neutrinos from the
  Earth/Sun antiprotons from the galactic
  halo positrons from the galactic halo gamma
  rays from the galactic halo gamma rays from
  external galaxies/halos synchrotron radiation
  from the galactic center / galaxy clusters ...

41
Direct detection - general principles
42
EdelweissJune 2002
43
Direct detection current limits
Spin-independent scattering
Spin-dependent scattering
Direct detection experiments have started
exploring the MSSM parameter space!
44
Neutralino capture and annihilation
Sun
interactions
hadronization
Freese, 86 Krauss, Srednicki Wilczek,
86Gaisser, Steigman Tilav, 86
Silk, Olive and Srednicki, 85Gaisser, Steigman
Tilav, 86
45
Indirect detection for cyclists
e.g. 104 m2 n-telescope searches for 500 GeV WIMP
gt LHC limit
300 km/s
1. ? - flux
500 GeV ________ mz
?? rcv 2.4 x 104 cm-2s-1
500 GeV ________ mz
0.4 GeV cm-3 8 x 10-4 cm-3
2. Solar cross section
M8 __ mN
S? ns s (?N) 1.2x1057 10-41cm2
GF2 ___ mZ2
MZ2 ___ mH4
(GF mN2)2
46
N? capture rate annihilation rate
_ c c
WW
250 GeV
500 GeV
mnm
N8 ?? S?? 3 x 1020 s-1
3. Capture rate by the sun
4. Number of muon-neutrinos Nnm 2 x
0.1 N ?
Leptonic BR0.1
47
Nnm ____ 4pd2
5. ?nm 2 x 10-8 cm-2 s-1
1 A.U.
5.5 x 1023 cm-3
6. events area x ?nm ?x ?ice x sn? ???m x
Rm
104 m2
En ___ GeV

• ?sn? ??m 10-38 cm2 2.5 x 10-36 cm2

_
E? ___ GeV

• Rm 5m 625m (Em 0.5 En)

events 10 per year
48
WIMPs in Center of Earth
Baikal
AMANDA limit 10 strings only
49
IceCube vs
Direct Detection (Zeppelin4/Genius) Black
out Green yes Blue no
50
MSSM parameter spaceFuture probed regions I
IceCube
51
Limits m flux from the Earth/Sun
Earth
Sun
52
Flux from Earth/Sun and future GENIUS/CRESST
limits
Earth
Sun