looking beyond the standard model with energetic cosmic...
TRANSCRIPT
-
Looking Beyond the StandardModel with Energetic Cosmic
Particles
Andreas Ringwaldhttp://www.desy.de/˜ringwald
DESY
Seminar
Universität Dortmund
June 13, 2006, Dortmund, Germany
-
– Looking Beyond the Standard Model – 11. Introduction
• There is a high energy universe:Gamma rays have been identified upto energies E
-
– Looking Beyond the Standard Model – 21. Introduction
• There is a high energy universe:Gamma rays have been identified upto energies E
-
– Looking Beyond the Standard Model – 31. Introduction
• There is a high energy universe:Gamma rays have been identified upto energies E
-
– Looking Beyond the Standard Model – 41. Introduction
• There is a high energy universe:Gamma rays have been identified upto energies E
-
– Looking Beyond the Standard Model – 5
Outline:
2. Ultrahigh energy cosmic rays and neutrinos
3. TeV scale physics with ultrahigh energy neutrinos
4. GUT scale physics with extremely energetic neutrinos
5. Conclusions
A. Ringwald (DESY) Seminar, Dortmund, June 2006
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– Looking Beyond the Standard Model – 6
2. Ultrahigh energy cosmic rays and neutrinos
• CR spectrum: Large statistical andsystematic uncertainties
⇐ low flux⇐ energy from shower simulations
• Crucial improvement by PAO:
⇐ huge size ⇒ better statistics⇐ hybrid observations ⇒ better
energy calibration through Fly’sEye technique, direction fromground array
• It works[Ahlers et al. ‘05]
A. Ringwald (DESY) Seminar, Dortmund, June 2006
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– Looking Beyond the Standard Model – 7
2. Ultrahigh energy cosmic rays and neutrinos
• CR spectrum: Large statistical andsystematic uncertainties
⇐ low flux⇐ energy from shower simulations
• Crucial improvement by PAO:
⇐ huge size ⇒ better statistics⇐ hybrid observations ⇒ better
energy calibration through Fly’sEye technique, direction fromground array
• It works [www.auger.org]
A. Ringwald (DESY) Seminar, Dortmund, June 2006
-
– Looking Beyond the Standard Model – 8
2. Ultrahigh energy cosmic rays and neutrinos
• CR spectrum: Large statistical andsystematic uncertainties
⇐ low flux⇐ energy from shower simulations
• Crucial improvement by PAO:
⇐ huge size ⇒ better statistics⇐ hybrid observations ⇒ better
energy calibration through Fly’sEye technique, direction fromground array
• It works[Ahlers et al. ‘05]
A. Ringwald (DESY) Seminar, Dortmund, June 2006
-
– Looking Beyond the Standard Model – 9
2. Ultrahigh energy cosmic rays and neutrinos
• CR spectrum: Large statistical andsystematic uncertainties
⇐ low flux⇐ energy from shower simulations
• Crucial improvement by PAO:
⇐ huge size ⇒ better statistics⇐ hybrid observations ⇒ better
energy calibration through Fly’sEye technique, direction fromground array
• It works[Ahlers et al. ‘05]
A. Ringwald (DESY) Seminar, Dortmund, June 2006
-
– Looking Beyond the Standard Model – 102. Ultrahigh energy cosmic rays and neutrinos
• CR angular distribution: ≈ isotrop
• CR composition: Large uncertainty
⇐ studies rely on simulations
• Cosmic rays above >∼ 108.6 GeV, the
“second knee”, dominantly protons
• Assume that CR’s in 10[8.6,11] GeVrange originate from isotropically dis-tributed extragalactic proton sources,with simple power-law injection spec-tra ∝ E−γi (1 + z)
n
[Berezinsky,..’02-’05;...;Ahlers et al. ‘05]
⇒ Good fit; inelastic interactions withCMB (e+e− “dip”; π “bump”) visi-ble; some post-GZK events?
[Greisen;Zatsepin,Kuzmin ‘67]
h12
+60
−60
−30
+30
0
o
o
o
o
hh
24
GC
AG
ASA
C
A. Ringwald (DESY) Seminar, Dortmund, June 2006
-
– Looking Beyond the Standard Model – 112. Ultrahigh energy cosmic rays and neutrinos
• CR angular distribution: ≈ isotrop
• CR composition: Large uncertainty
⇐ studies rely on simulations
• Cosmic rays above >∼ 108.6 GeV, the
“second knee”, dominantly protons
• Assume that CR’s in 10[8.6,11] GeVrange originate from isotropically dis-tributed extragalactic proton sources,with simple power-law injection spec-tra ∝ E−γi (1 + z)
n
[Berezinsky,..’02-’05;...;Ahlers et al. ‘05]
⇒ Good fit; inelastic interactions withCMB (e+e− “dip”; π “bump”) visi-ble; some post-GZK events?
[Greisen;Zatsepin,Kuzmin ‘67]
400
500
600
700
800
900
1000
1014
1015
1016
1017
1018
1019
1020
1021
Elab
(eV)
Xm
ax (
g/c
m2)
proton
iron
gamma
gammawith preshower
DPMJET 2.55
neXus 2
neXus 3
QGSJET 01c
QGSJET II
SIBYLL 2.1
Fly´s Eye
HiRes-MIA
HiRes 2004
Yakutsk 2001
Yakutsk 2005
CASA-BLANCA
HEGRA-AIROBICC
SPASE-VULCAN
DICE
TUNKA
[Heck ‘05]
A. Ringwald (DESY) Seminar, Dortmund, June 2006
-
– Looking Beyond the Standard Model – 122. Ultrahigh energy cosmic rays and neutrinos
• CR angular distribution: ≈ isotrop
• CR composition: Large uncertainty
⇐ studies rely on simulations
• Cosmic rays above >∼ 108.6 GeV, the
“second knee”, dominantly protons
• Assume that CR’s in 10[8.6,11] GeVrange originate from isotropically dis-tributed extragalactic proton sources,with simple power-law injection spec-tra ∝ E−γi (1 + z)
n
[Berezinsky,..’02-’05;...;Ahlers et al. ‘05]
⇒ Good fit; inelastic interactions withCMB (e+e− “dip”; π “bump”) visi-ble; some post-GZK events?
[Greisen;Zatsepin,Kuzmin ‘67][Ahlers et al. ‘05]
A. Ringwald (DESY) Seminar, Dortmund, June 2006
-
– Looking Beyond the Standard Model – 132. Ultrahigh energy cosmic rays and neutrinos
• CR angular distribution: ≈ isotrop
• CR composition: Large uncertainty
⇐ studies rely on simulations
• Cosmic rays above >∼ 108.6 GeV, the
“second knee”, dominantly protons
• Assume that CR’s in 10[8.6,11] GeVrange originate from isotropically dis-tributed extragalactic proton sources,with simple power-law injection spec-tra ∝ E−γi (1 + z)
n
[Berezinsky,..’02-’05;...;Ahlers et al. ‘05]
⇒ Good fit; inelastic interactions withCMB (e+e− “dip”; π “bump”) visi-ble; some post-GZK events?
[Greisen;Zatsepin,Kuzmin ‘67][Ahlers et al. ‘05]
A. Ringwald (DESY) Seminar, Dortmund, June 2006
-
– Looking Beyond the Standard Model – 14
• Possible sources of these protons:GRB, AGN, . . .
• Shock acceleration:– p’s, confined by magnetic fields,
accelerate through repeated scat-tering by plasma shock fronts
– production of π’s and n’s throughcollisions of the trapped p’s withambient plasma produces γ’s, ν’sand CR’s (n diffusion from source)
• Neutrinos as diagnostic tool:– ν’s from sources (pγ → n + π’s)
close to be measured– Cosmogenic neutrino flux (from
pγCMB → Nπ’s) dominates above109 GeV
A. Ringwald (DESY) Seminar, Dortmund, June 2006
-
– Looking Beyond the Standard Model – 15
• Possible sources of these protons:GRB, AGN, . . .
• Shock acceleration:– p’s, confined by magnetic fields,
accelerate through repeated scat-tering by plasma shock fronts
– production of π’s and n’s throughcollisions of the trapped p’s withambient plasma produces γ’s, ν’sand CR’s (n diffusion from source)
• Neutrinos as diagnostic tool:– ν’s from sources (pγ → n + π’s)
close to be measured– Cosmogenic neutrino flux (from
pγCMB → Nπ’s) dominates above109 GeV
p
π+
µ+
e+
nπ−
µ−
e−
p
νµ
ν̄µ
νe
ν̄µ
νµ
ν̄e
SHO
CK
[Ahlers PhD in prep.]
A. Ringwald (DESY) Seminar, Dortmund, June 2006
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– Looking Beyond the Standard Model – 16
• Possible sources of these protons:GRB, AGN, . . .
• Shock acceleration:– p’s, confined by magnetic fields,
accelerate through repeated scat-tering by plasma shock fronts
– production of π’s and n’s throughcollisions of the trapped p’s withambient plasma produces γ’s, ν’sand CR’s (n diffusion from source)
• Neutrinos as diagnostic tool:– ν’s from sources (pγ → n + π’s)
close to be measured– Cosmogenic neutrino flux (from
pγCMB → Nπ’s) dominates above109 GeV
Hillas-plot
(100 EeV)
(1 ZeV)
Γ
Neutronstar
maxE ~ ZBL
maxE ~ ZBL
White
dwarf
Protons
(candidate sites for E=100 EeV and E=1 ZeV)
GRB
Galacticdisk
halo
galaxiesColliding
jets
nuclei
lobes
hot-spots
SNR
Active
galaxies
Clusters
(Fermi)
(Ultra-relativistic shocks-GRB)
1 au 1 pc 1 kpc 1 Mpc
-9
-3
3
9
15
3 6 9 12 15 18 21
log(Magnetic field, gauss)
log(size, km)
Fe (100 EeV)
Protons
[Pierre Auger Observatory]A. Ringwald (DESY) Seminar, Dortmund, June 2006
-
– Looking Beyond the Standard Model – 17
• Possible sources of these protons:GRB, AGN, . . .
• Shock acceleration:– p’s, confined by magnetic fields,
accelerate through repeated scat-tering by plasma shock fronts
– production of π’s and n’s throughcollisions of the trapped p’s withambient plasma produces γ’s, ν’sand CR’s (n diffusion from source)
• Neutrinos as diagnostic tool:– ν’s from sources (pγ → n + π’s)
close to be measured– Cosmogenic neutrino flux (from
pγCMB → Nπ’s) dominates above109 GeV
p
π+
µ+
e+
νµ
ν̄µ
νe
n
SHO
CK
[Ahlers PhD in prep.]
A. Ringwald (DESY) Seminar, Dortmund, June 2006
-
– Looking Beyond the Standard Model – 18
• Possible sources of these protons:GRB, AGN, . . .
• Shock acceleration:– p’s, confined by magnetic fields,
accelerate through repeated scat-tering by plasma shock fronts
– production of π’s and n’s throughcollisions of the trapped p’s withambient plasma produces γ’s, ν’sand CR’s (n diffusion from source)
• Neutrinos as diagnostic tool:– ν’s from sources (pγ → n + π’s)
close to be measured– Cosmogenic neutrino flux (from
pγCMB → Nπ’s) dominates above109 GeV
[Ahlers et al. ‘05]
A. Ringwald (DESY) Seminar, Dortmund, June 2006
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– Looking Beyond the Standard Model – 19
3. TeV scale physics with ultrahigh energy neutrinos
• Cν’s with Eν >∼ 108 GeV probe νN
scattering at√
sνN >∼ 14 TeV (LHC)
• Perturbative Standard Model (SM)≈ under control (← HERA)
[Gandhi et al. ’98; Glück et al. ’98; ...]
⇒ Search for enhancements in σνNbeyond (perturbative) SM:
⋄ Electroweak sphaleron production(B + L violating processes in SM)⋄ Kaluza-Klein, black hole, p-brane
or string ball production in TeVscale gravity models⋄ . . . [Ahlers et al. ‘05]
A. Ringwald (DESY) Seminar, Dortmund, June 2006
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– Looking Beyond the Standard Model – 20
3. TeV scale physics with ultrahigh energy neutrinos
• Cν’s with Eν >∼ 108 GeV probe νN
scattering at√
sνN >∼ 14 TeV (LHC)
• Perturbative Standard Model (SM)≈ under control (← HERA)
[Gandhi et al. ’98; Glück et al. ’98; ...]
⇒ Search for enhancements in σνNbeyond (perturbative) SM:
⋄ Electroweak sphaleron production(B + L violating processes in SM)⋄ Kaluza-Klein, black hole, p-brane
or string ball production in TeVscale gravity models⋄ . . .
[Tu ‘04]
A. Ringwald (DESY) Seminar, Dortmund, June 2006
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– Looking Beyond the Standard Model – 21
3. TeV scale physics with ultrahigh energy neutrinos
• Cν’s with Eν >∼ 108 GeV probe νN
scattering at√
sνN >∼ 14 TeV (LHC)
• Perturbative Standard Model (SM)≈ under control (← HERA)
[Gandhi et al. ’98; Glück et al. ’98; ...]
⇒ Search for enhancements in σνNbeyond (perturbative) SM:
⋄ Electroweak sphaleron production(B + L violating processes in SM)
⋄ Kaluza-Klein, black hole, p-braneor string ball production in TeVscale gravity models⋄ . . .
[Fodor,Katz,AR,Tu ‘03; Han,Hooper ‘03]
A. Ringwald (DESY) Seminar, Dortmund, June 2006
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– Looking Beyond the Standard Model – 22
3. TeV scale physics with ultrahigh energy neutrinos
• Cν’s with Eν >∼ 108 GeV probe νN
scattering at√
sνN >∼ 14 TeV (LHC)
• Perturbative Standard Model (SM)≈ under control (← HERA)
[Gandhi et al. ’98; Glück et al. ’98; ...]
⇒ Search for enhancements in σνNbeyond (perturbative) SM:
⋄ Electroweak sphaleron production(B + L violating processes in SM)
⋄ Kaluza-Klein, black hole, p-braneor string ball production in TeVscale gravity models⋄ . . .
[AR,Tu ‘01; Tu ‘04]
A. Ringwald (DESY) Seminar, Dortmund, June 2006
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– Looking Beyond the Standard Model – 23
“Model-independent” upper bounds on σνN
dN
dt∝
∫dEν Fν(Eν)σνN(Eν)
⇒ Non-observation of deeply-penetra-ting particles, together with lowerbound on Fν (e.g. cosmogenic ν’s)⇒ upper bound on σνN[Berezinsky,Smirnov ‘74; Morris,AR ‘94; Tyler,Olinto,Sigl ‘01;..]
• Recent quantitative analysis:[Anchordoqui,Fodor,Katz,AR,Tu ‘04]
⋄ Best current limits from exploi-tation of RICE search results
[Kravchenko et al. [RICE] ‘02,03]
⋄ Auger will improve these limits byone order of magnitude [Anchordoqui,Fodor,Katz,AR,Tu ‘04]
A. Ringwald (DESY) Seminar, Dortmund, June 2006
-
– Looking Beyond the Standard Model – 24
“Model-independent” upper bounds on σνN
dN
dt∝
∫dEν Fν(Eν)σνN(Eν)
⇒ Non-observation of deeply-penetra-ting particles, together with lowerbound on Fν (e.g. cosmogenic ν’s)⇒ upper bound on σνN[Berezinsky,Smirnov ‘74; Morris,AR ‘94; Tyler,Olinto,Sigl ‘01;..]
• Recent quantitative analysis:[Anchordoqui,Fodor,Katz,AR,Tu ‘04]
⋄ Best current limits from exploi-tation of RICE search results
[Kravchenko et al. [RICE] ‘02,03]
⋄ Auger will improve these limits byone order of magnitude [Anchordoqui,Fodor,Katz,AR,Tu ‘04]
A. Ringwald (DESY) Seminar, Dortmund, June 2006
-
– Looking Beyond the Standard Model – 25
Strongly interacting neutrino scenarios
• Bounds exploiting searches for dee-ply-penetrating particles applicableas long as σνN
-
– Looking Beyond the Standard Model – 26
Strongly interacting neutrino scenarios
• Bounds exploiting searches for dee-ply-penetrating particles applicableas long as σνN
-
– Looking Beyond the Standard Model – 27
Strongly interacting neutrino scenarios
• Bounds exploiting searches for dee-ply-penetrating particles applicableas long as σνN
-
– Looking Beyond the Standard Model – 28
Strongly interacting neutrino scenarios
• Bounds exploiting searches for dee-ply-penetrating particles applicableas long as σνN
-
– Looking Beyond the Standard Model – 29
Long-lived staus at IceCube
• In most SUSY extensions of SM,lightest superpartner (LSP) stable
– neutralino dark matter– gravitino dark matter
• Gravitino LSP interacts only gravi-tationally ⇒ next-to-lightest SUSYparticle (NLSP) long-lived
• If NLSP charged, e.g. stau τ̃ , itcan possibly be collected in colliderexperiments. Observation of staudecays ⇒ indirect discovery of thegravitino [Buchmüller et al. ‘04,...,Feng et al. ‘04,...].
[Ahlers,Kersten,AR ‘06]
A. Ringwald (DESY) Seminar, Dortmund, June 2006
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– Looking Beyond the Standard Model – 30
Long-lived staus at IceCube
• Long-lived stau NLSPs resulting fromcosmic νN interactions inside Earthcan be detected in ice or waterCherenkov neutrino telescopes[Albuquerque,Burdman,Chacko ‘03; Ahlers,Kersten,AR ‘06;...]
• SUSY cross-section smaller than SM
• Stau has small energy loss in matter⇒ effective detection volume for staumuch larger than for muon
• Staus always produced in pairs ⇒nearly parallel muon-like tracks in thedetector, in contrast to SM, wheresingle muons dominate
• IceCube: Up to 50 τ̃ pair events/yr
[Ahlers,Kersten,AR ‘06]
A. Ringwald (DESY) Seminar, Dortmund, June 2006
-
– Looking Beyond the Standard Model – 31
Long-lived staus at IceCube
• Long-lived stau NLSPs resulting fromcosmic νN interactions inside Earthcan be detected in ice or waterCherenkov neutrino telescopes[Albuquerque,Burdman,Chacko ‘03; Ahlers,Kersten,AR ‘06;...]
• SUSY cross-section smaller than SM
• Stau has small energy loss in matter⇒ effective detection volume for staumuch larger than for muon
• Staus always produced in pairs ⇒nearly parallel muon-like tracks in thedetector, in contrast to SM, wheresingle muons dominate
• IceCube: Up to 50 τ̃ pair events/yr
[Ahlers,Kersten,AR ‘06]
A. Ringwald (DESY) Seminar, Dortmund, June 2006
-
– Looking Beyond the Standard Model – 32
4. GUT scale physics with extremely energetic neutrinos
• Existing observatories for ExtremelyHigh Energy Cosmic neutrinos pro-vide upper bounds up to GUT scale
• Upcoming decade: Improved sensiti-vity by many orders of magnitude
⇒ E ≥ 107 GeV:→ Astrophysics of cosmic rays
⇒ E ≥ 108 GeV:→ Particle physics beyond LHC
⇒ E ≥ 1012 GeV:→ Cosmology: relics of GUT phase
transitions; absorption on big bangrelic neutrinos [AR,L.Schrempp ‘06]
A. Ringwald (DESY) Seminar, Dortmund, June 2006
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– Looking Beyond the Standard Model – 33
Top-down scenarios for super-GZK neutrinos
• Existence of superheavy particleswith 1012 GeV
-
– Looking Beyond the Standard Model – 34
Top-down scenarios for super-GZK neutrinos
• Existence of superheavy particleswith 1012 GeV
-
– Looking Beyond the Standard Model – 35
Top-down scenarios for super-GZK neutrinos
• Existence of superheavy particleswith 1012 GeV
-
– Looking Beyond the Standard Model – 36
Top-down scenarios for super-GZK neutrinos
• Existence of superheavy particleswith 1012 GeV
-
– Looking Beyond the Standard Model – 37
Top-down scenarios for super-GZK neutrinos
• Existence of superheavy particleswith 1012 GeV
-
– Looking Beyond the Standard Model – 38
Top-down scenarios for super-GZK neutrinos
• Injection spectra: fragmentationfunctions Di(x, µ), i = p, e, γ, ν, de-termined via
– Monte Carlo generators– DGLAP evolution from experi-
mental initial distributions at e.g.µ = mZ to µ = mX
⇒ Reliably predicted!
• Spectra at Earth:
– for superheavy dark matter, injec-tion nearby: jν ∼ jγ ∼ jp
– for topological defects, injectionfar away: jν ≫ jγ ∼ jp
0.01
0.03
0.1
0.3
1
3
10
30
100
300
1/σ
had
dσ
/dx
1/σ
had
dσ
/dx
1/σ
had
dσ
/dx
π± (√s = 91 GeV)
π± (√s = 29 GeV)
π± (√s = 10 GeV)
(a)
0.01
0.03
0.1
0.3
1
3
10
30
K± (√s = 91 GeV)
K± (√s = 29 GeV)
K± (√s = 10 GeV)
(b)
0.01
0.03
0.1
0.3
1
3
10
30
0.005 0.01 0.02 0.05 0.1 0.2 0.5 1
xp = p/p
beam
p, _p (√s = 91 GeV)
p, _p (√s = 29 GeV)
p, _p (√s = 10 GeV)
(c)
[Particle Data Group ‘04]
A. Ringwald (DESY) Seminar, Dortmund, June 2006
-
– Looking Beyond the Standard Model – 39
Top-down scenarios for super-GZK neutrinos
• Injection spectra: fragmentationfunctions Di(x, µ), i = p, e, γ, ν, de-termined via
– Monte Carlo generators– DGLAP evolution from experi-
mental initial distributions at e.g.µ = mZ to µ = mX
⇒ Reliably predicted!
• Spectra at Earth:
– for superheavy dark matter, injec-tion nearby: jν ∼ jγ ∼ jp
– for topological defects, injectionfar away: jν ≫ jγ ∼ jp
1e-05
0.0001
0.001
0.01
0.1
1
10
100
1000
1e-05 0.0001 0.001 0.01 0.1 1
this workBarbot-DreesSarkar-Toldrax
xDp q(x;M X)
MX = 1� 1016 GeV
[Aloisio,Berezinsky,Kachelriess ‘04]
A. Ringwald (DESY) Seminar, Dortmund, June 2006
-
– Looking Beyond the Standard Model – 40
Top-down scenarios for super-GZK neutrinos
• Injection spectra: fragmentationfunctions Di(x, µ), i = p, e, γ, ν, de-termined via
– Monte Carlo generators– DGLAP evolution from experi-
mental initial distributions at e.g.µ = mZ to µ = mX
⇒ Reliably predicted!
• Spectra at Earth:
– for superheavy dark matter, injec-tion nearby: jν ∼ jγ ∼ jp
– for topological defects, injectionfar away: jν ≫ jγ ∼ jp
[Aloisio,Berezinsky,Kachelriess ‘04]
A. Ringwald (DESY) Seminar, Dortmund, June 2006
-
– Looking Beyond the Standard Model – 41
Top-down scenarios for super-GZK neutrinos
• Injection spectra: fragmentationfunctions Di(x, µ), i = p, e, γ, ν, de-termined via
– Monte Carlo generators– DGLAP evolution from experi-
mental initial distributions at e.g.µ = mZ to µ = mX
⇒ Reliably predicted!
• Spectra at Earth:
– for superheavy dark matter, injec-tion nearby: jν ∼ jγ ∼ jp
– for topological defects, injectionfar away: jν ≫ jγ ∼ jp
1e+22
1e+23
1e+24
1e+25
1e+26
1e+27
1e+18 1e+19 1e+20 1e+21 1e+22E (eV)
E3 J(E)(eV2 m�2 s�1 sr�
1 ) MX = 1� 1014 GeV�p
p+
[Aloisio,Berezinsky,Kachelriess ‘04]
A. Ringwald (DESY) Seminar, Dortmund, June 2006
-
– Looking Beyond the Standard Model – 42
Top-down scenarios for super-GZK neutrinos
• How generic?– Superheavy dark matter: need
symmetry to prevent fast X decay∗ gauge ⇒ X stable∗ discrete⇒ stable or quasi-stable
– Topological defects: generic pre-diction of symmetry breaking (SB)in GUT’s, including fundamentalstring theory, e.g.∗ G→ H×U(1) SB: monopoles∗ U(1) SB: ordinary or supercon-
ducting strings∗ G→ H×U(1)→ H× ZN SB:
monopoles connected by strings
A. Ringwald (DESY) Seminar, Dortmund, June 2006
-
– Looking Beyond the Standard Model – 43
Top-down scenarios for super-GZK neutrinos
• How generic?– Superheavy dark matter: need
symmetry to prevent fast X decay∗ gauge ⇒ X stable∗ discrete⇒ stable or quasi-stable
– Topological defects: generic pre-diction of symmetry breaking (SB)in GUT’s, and even fundamentalstring theory, e.g.∗ G→ H×U(1) SB: monopoles∗ U(1) SB: ordinary or supercon-
ducting strings∗ G→ H×U(1)→ H× ZN SB:
monopoles connected by strings
x
y
z
Reφ
Imφ
[Rajantie ‘03]
A. Ringwald (DESY) Seminar, Dortmund, June 2006
-
– Looking Beyond the Standard Model – 44
Top-down scenarios for super-GZK neutrinos
• How generic?– Superheavy dark matter: need
symmetry to prevent fast X decay∗ gauge ⇒ X stable∗ discrete⇒ stable or quasi-stable
– Topological defects: generic pre-diction of symmetry breaking (SB)in GUT’s, and even fundamentalstring theory, e.g.∗ G→ H×U(1) SB: monopoles∗ U(1) SB: ordinary or supercon-
ducting strings∗ G→ H×U(1)→ H× ZN SB:
monopoles connected by strings
NECKLACE
M M
M
M M
M
MS NETWORK
[Berezinsky ‘05]
A. Ringwald (DESY) Seminar, Dortmund, June 2006
-
– Looking Beyond the Standard Model – 45
Top-down scenarios for super-GZK neutrinos
• How generic?– Superheavy dark matter: need
symmetry to prevent fast X decay∗ gauge ⇒ X stable∗ discrete⇒ stable or quasi-stable
– Topological defects: generic pre-diction of symmetry breaking (SB)in GUT’s, including fundamentalstring theory, e.g.∗ G→ H×U(1) SB: monopoles∗ U(1) SB: ordinary or supercon-
ducting strings∗ G→ H×U(1)→ H× ZN SB:
monopoles connected by strings
SO(10)1
−→ 4C 2L 2R
8>>>>>>>>>>>>>>>>>>>>>>>>>:
1−→ 3C 2L 2R 1B−L
8
-
– Looking Beyond the Standard Model – 46
Top-down scenarios for super-GZK neutrinos
• Strong impact of measurement for
– particle physics
∗ GUT parameters, e.g. mX∗ particle content of the desert,
e.g. SM vs. MSSM∗ νN scattering at
√s≫ LHC
– cosmology
∗ window on early phase transition∗ Hubble expansion rate H(z)∗ existence of the big bang relic
neutrino background
[Fodor,Katz,AR,Weiler,Wong,in prep.]
A. Ringwald (DESY) Seminar, Dortmund, June 2006
-
– Looking Beyond the Standard Model – 47
Top-down scenarios for super-GZK neutrinos
• Strong impact of measurement for
– particle physics
∗ GUT parameters, e.g. mX∗ particle content of the desert,
e.g. SM vs. MSSM∗ νN scattering at
√s≫ LHC
– cosmology
∗ window on early phase transition∗ Hubble expansion rate H(z)∗ existence of the big bang relic
neutrino background
[Fodor,Katz,AR,Weiler,Wong,in prep.]
A. Ringwald (DESY) Seminar, Dortmund, June 2006
-
– Looking Beyond the Standard Model – 48
Top-down scenarios for super-GZK neutrinos
• Strong impact of measurement for
– particle physics
∗ GUT parameters, e.g. mX∗ particle content of the desert,
e.g. SM vs. MSSM∗ νN scattering at
√s≫ LHC
– cosmology
∗ window on early phase transition∗ Hubble expansion rate H(z)∗ existence of the big bang relic
neutrino background [Barbot,Drees ‘02]
A. Ringwald (DESY) Seminar, Dortmund, June 2006
-
– Looking Beyond the Standard Model – 49
Top-down scenarios for super-GZK neutrinos
• Strong impact of measurement for
– particle physics
∗ GUT parameters, e.g. mX∗ particle content of the desert,
e.g. SM vs. MSSM∗ νN scattering at
√s≫ LHC
– cosmology
∗ window on early phase transition∗ Hubble expansion rate H(z)∗ existence of the big bang relic
neutrino background[Tu ‘04]
A. Ringwald (DESY) Seminar, Dortmund, June 2006
-
– Looking Beyond the Standard Model – 50
Top-down scenarios for super-GZK neutrinos
• Strong impact of measurement for
– particle physics
∗ GUT parameters, e.g. mX∗ particle content of the desert,
e.g. SM vs. MSSM∗ νN scattering at
√s≫ LHC
– cosmology
∗ window on early phase transition∗ Hubble expansion rate H(z)∗ existence of the big bang relic
neutrino background (CνB)
A. Ringwald (DESY) Seminar, Dortmund, June 2006
-
– Looking Beyond the Standard Model – 51
Top-down scenarios for super-GZK neutrinos
• Strong impact of measurement for
– particle physics
∗ GUT parameters, e.g. mX∗ particle content of the desert,
e.g. SM vs. MSSM∗ νN scattering at
√s≫ LHC
– cosmology
∗ window on early phase transition∗ Hubble expansion rate H(z)∗ existence of the big bang relic
neutrino background (CνB)
[Fodor,Katz,AR,Weiler,Wong,in prep.]
A. Ringwald (DESY) Seminar, Dortmund, June 2006
-
– Looking Beyond the Standard Model – 52
Top-down scenarios for super-GZK neutrinos
• Strong impact of measurement for
– particle physics
∗ GUT parameters, e.g. mX∗ particle content of the desert,
e.g. SM vs. MSSM∗ νN scattering at
√s≫ LHC
– cosmology
∗ window on early phase transition∗ Hubble expansion rate H(z)∗ existence of the big bang relic
neutrino background (CνB)
[Fodor,Katz,AR,Weiler,Wong,in prep.]
A. Ringwald (DESY) Seminar, Dortmund, June 2006
-
– Looking Beyond the Standard Model – 53
Top-down scenarios for super-GZK neutrinos
• Strong impact of measurement for
– particle physics
∗ GUT parameters, e.g. mX∗ particle content of the desert,
e.g. SM vs. MSSM∗ νN scattering at
√s≫ LHC
– cosmology
∗ window on early phase transition∗ Hubble expansion rate H(z)∗ existence of the big bang relic
neutrino background (CνB)
[AR,L. Schrempp ‘06]
A. Ringwald (DESY) Seminar, Dortmund, June 2006
-
– Looking Beyond the Standard Model – 54
5. Conclusions
• Exciting times for ultrahigh energycosmic rays and neutrinos:
– many observatories under con-struction
⇒ appreciable event samples
• Expect strong impact on
– astrophysics– particle physics– cosmology
A. Ringwald (DESY) Seminar, Dortmund, June 2006