Super-GZK Neutrinos - DESYringwald/astroparticle/talks/taup05.pdf · White dwarf Protons ... t=328...
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Super-GZK Neutrinos A. Ringwald http://www.desy.de/˜ringwald DESY 9 th International Conference on Topics in Astroparticle and Underground Physics (TAUP 2005) September 10 - 14, 2005, University of Zaragoza, Zaragoza, Spain
Transcript of Super-GZK Neutrinos - DESYringwald/astroparticle/talks/taup05.pdf · White dwarf Protons ... t=328...
Super-GZK Neutrinos
A. Ringwaldhttp://www.desy.de/˜ringwald
DESY
9th International Conference onTopics in Astroparticle and Underground Physics (TAUP 2005)
September 10 - 14, 2005, University of Zaragoza, Zaragoza, Spain
– Super-GZK neutrinos – 1
1. Introduction
• Existing observatories for ExtremelyHigh Energy Cosmic neutrinos pro-vide sensible upper bounds on flux
• Upcoming decade: progressively lar-ger detectors for EHECν’s
⇒ E ≥ 1016 eV:
→ Astrophysics of cosmic rays
⇒ E ≥ 1017 eV:
→ Particle physics beyond LHC
⇒ E ≥ 1021 eV:
→ Cosmology: relics of phase tran-sitions; absorption on big bang re-lic neutrinos
A. Ringwald (DESY) TAUP 2005, Zaragoza, Spain
– Super-GZK neutrinos – 2
1. Introduction
• Existing observatories for ExtremelyHigh Energy Cosmic neutrinos pro-vide sensible upper bounds on flux
• Upcoming decade: progressively lar-ger detectors for EHECν’s
⇒ E ≥ 1016 eV:
→ Astrophysics of cosmic rays
⇒ E ≥ 1017 eV:
→ Particle physics beyond LHC
⇒ E ≥ 1021 eV:
→ Cosmology: relics of phase tran-sitions; absorption on big bang re-lic neutrinos
A. Ringwald (DESY) TAUP 2005, Zaragoza, Spain
– Super-GZK neutrinos – 3
1. Introduction
• Existing observatories for ExtremelyHigh Energy Cosmic neutrinos pro-vide sensible upper bounds on flux
• Upcoming decade: progressively lar-ger detectors for EHECν’s
⇒ E ≥ 1016 eV:
→ Astrophysics of cosmic rays
⇒ E ≥ 1017 eV:
→ Particle physics beyond LHC
⇒ E ≥ 1021 eV:
→ Cosmology: relics of phase tran-sitions; absorption on big bang re-lic neutrinos
A. Ringwald (DESY) TAUP 2005, Zaragoza, Spain
– Super-GZK neutrinos – 4
1. Introduction
• Existing observatories for ExtremelyHigh Energy Cosmic neutrinos pro-vide sensible upper bounds on flux
• Upcoming decade: progressively lar-ger detectors for EHECν’s
⇒ E ≥ 1016 eV:
→ Astrophysics of cosmic rays
⇒ E ≥ 1017 eV:
→ Particle physics beyond LHC
⇒ E ≥ 1021 eV:
→ Cosmology: relics of phase tran-sitions; absorption on big bang re-lic neutrinos
A. Ringwald (DESY) TAUP 2005, Zaragoza, Spain
– Super-GZK neutrinos – 5
• Further content:
2. Sources and fluxes of super-GZK neutrinos3. Fun with super-GZK neutrinos4. Conclusions
A. Ringwald (DESY) TAUP 2005, Zaragoza, Spain
– Super-GZK neutrinos – 62. Sources and fluxes of super-GZK neutrinos
• Paradigm for astrophysical extra-galactic source of protons and neu-trinos: 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)
Hillas: Ep <∼ 1021 eV⇒ Eν <∼ 1020 eV
⇒ Super-GZK (Eν >∼ 1020 eV) neutrinos
← yet unknown acceleration sites← other acceleration mechanism← decay of superheavy particlesA. Ringwald (DESY) TAUP 2005, Zaragoza, Spain
– Super-GZK neutrinos – 72. Sources and fluxes of super-GZK neutrinos
• Paradigm for astrophysical extra-galactic source of protons and neu-trinos: 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)
Hillas: Ep <∼ 1021 eV⇒ Eν <∼ 1020 eV
⇒ Super-GZK (Eν >∼ 1020 eV) neutrinos
← yet unknown acceleration sites← other acceleration mechanism← decay of superheavy particles
p
π+
µ+
e+
nπ−
µ−
e−
p
νµ
ν̄µ
νe
ν̄µ
νµ
ν̄e
SHO
CK
[Ahlers PhD in prep.]
A. Ringwald (DESY) TAUP 2005, Zaragoza, Spain
– Super-GZK neutrinos – 82. Sources and fluxes of super-GZK neutrinos
• Paradigm for astrophysical extra-galactic source of protons and neu-trinos: 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)
Hillas: Ep <∼ 1021 eV⇒ Eν <∼ 1020 eV
⇒ Super-GZK (Eν >∼ 1020 eV) neutrinos
← yet unknown acceleration sites← other acceleration mechanism← decay of superheavy particles
p
π+
µ+
e+
νµ
ν̄µ
νe
n
SHO
CK
[Ahlers PhD in prep.]
A. Ringwald (DESY) TAUP 2005, Zaragoza, Spain
– Super-GZK neutrinos – 92. Sources and fluxes of super-GZK neutrinos
• Paradigm for astrophysical extra-galactic source of protons and neu-trinos: 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)
Hillas: Ep <∼ 1021 eV⇒ Eν <∼ 1020 eV
⇒ Super-GZK (Eν >∼ 1020 eV) neutrinos
← yet unknown acceleration sites← other acceleration mechanism← decay of superheavy particles
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) TAUP 2005, Zaragoza, Spain
– Super-GZK neutrinos – 102. Sources and fluxes of super-GZK neutrinos
• Paradigm for astrophysical extra-galactic source of protons and neu-trinos: 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)
Hillas: Ep <∼ 1021 eV⇒ Eν <∼ 1020 eV
⇒ Super-GZK (Eν >∼ 1020 eV) neutrinos
← yet unknown acceleration sites← other acceleration mechanism← decay of superheavy particles
A. Ringwald (DESY) TAUP 2005, Zaragoza, Spain
– Super-GZK neutrinos – 112. Sources and fluxes of super-GZK neutrinos
• Paradigm for astrophysical extra-galactic source of protons and neu-trinos: 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)
Hillas: Ep <∼ 1021 eV⇒ Eν <∼ 1020 eV
⇒ Super-GZK (Eν >∼ 1020 eV) neutrinos
← yet unknown acceleration sites← other acceleration mechanism← decay of superheavy particles
[Barbot,Drees ‘02]
A. Ringwald (DESY) TAUP 2005, Zaragoza, Spain
– Super-GZK neutrinos – 122. Sources and fluxes of super-GZK neutrinos
• Paradigm for astrophysical extra-galactic source of protons and neu-trinos: 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)
Hillas: Ep <∼ 1021 eV⇒ Eν <∼ 1020 eV
⇒ Super-GZK (Eν >∼ 1020 eV) neutrinos
← yet unknown acceleration sites← other acceleration mechanism← decay of superheavy particles
A. Ringwald (DESY) TAUP 2005, Zaragoza, Spain
– Super-GZK neutrinos – 13
Top-down scenarios for super-GZK neutrinos
• Existence of superheavy particleswith 1012 GeV <∼mX <∼ 1016 GeV,produced during and after inflationthrough e.g.
– particle creation in time-varyinggravitational field
⇒ super-GZK ν’s from decay or anni-hilation of superheavy dark matter(for τX >∼ τU)
– decomposition of topological de-fects, formed during preheating,into their constituents
⇒ super-GZK ν’s from topologicaldefects [Kolb,Chung,Riotto ‘98]
A. Ringwald (DESY) TAUP 2005, Zaragoza, Spain
– Super-GZK neutrinos – 14
Top-down scenarios for super-GZK neutrinos
• Existence of superheavy particleswith 1012 GeV <∼mX <∼ 1016 GeV,produced during and after inflationthrough e.g.
– particle creation in time-varyinggravitational field
⇒ super-GZK ν’s from decay or anni-hilation of superheavy dark matter(for τX >∼ τU)
– decomposition of topological de-fects, formed during preheating,into their constituents
⇒ super-GZK ν’s from topologicaldefects
0
500
50
t=252t=252
0
500
50
t=280t=280
0
500
50
t=328t=328
0
500
50
t=330t=330
[Tkachev,Khlebnikov,Kofman,Linde ‘98]
A. Ringwald (DESY) TAUP 2005, Zaragoza, Spain
– Super-GZK neutrinos – 15
Top-down scenarios for super-GZK neutrinos
• Existence of superheavy particleswith 1012 GeV <∼mX <∼ 1016 GeV,produced during and after inflationthrough e.g.
– particle creation in time-varyinggravitational field
⇒ super-GZK ν’s from decay or anni-hilation of superheavy dark matter(for τX >∼ τU)
– decomposition of topological de-fects, formed during preheating,into their constituents
⇒ super-GZK ν’s from topologicaldefects
21
22
23
24
25
26
27
28
18 19 20 21 22
Itot� Ihalo IhaloNIextrp
log10(E=eV)log 10(E3 I);m�2 s�1 sr�1 eV
2FIG. 1: Predicted uxes from decaying X-particles: nucleons (p; �p; n; �n) fromthe halo (curve IhaloN ), extragalactic protons (curve Iextrp ), photons from the halo(curve Ihalo ), and neutrinos from the halo and the extragalactic space (curveItot� ). The data points are based on the compilation made in Ref. [21].
[Berezinsky,Kachelriess,Vilenkin ‘97]
A. Ringwald (DESY) TAUP 2005, Zaragoza, Spain
– Super-GZK neutrinos – 16
Top-down scenarios for super-GZK neutrinos
• Existence of superheavy particleswith 1012 GeV <∼mX <∼ 1016 GeV,produced during and after inflationthrough e.g.
– particle creation in time-varyinggravitational field
⇒ super-GZK ν’s from decay or anni-hilation of superheavy dark matter(for τX >∼ τU)
– decomposition of topological de-fects, formed during preheating,into their constituents
⇒ super-GZK ν’s from topologicaldefects [Bhattacharjee,Hill,Schramm ‘92]
A. Ringwald (DESY) TAUP 2005, Zaragoza, Spain
– Super-GZK neutrinos – 17
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
0.001
0.01
0.1
1
10
100
1000
0 0.2 0.4 0.6 0.8 1dN/dx
x
Photons
Neutrinos
Electrons
Protons
mX = 1011 GeV
0.001
0.01
0.1
1
10
100
1000
0 0.2 0.4 0.6 0.8 1dN/dx
x
Photons
Neutrinos
Electrons
Protons
mX = 1011 GeV
0.001
0.01
0.1
1
10
100
1000
0 0.2 0.4 0.6 0.8 1dN/dx
x
Photons
Neutrinos
Electrons
Protons
mX = 1011 GeV
0.001
0.01
0.1
1
10
100
1000
0 0.2 0.4 0.6 0.8 1dN/dx
x
Photons
Neutrinos
Electrons
Protons
mX = 1011 GeV
[Birkel,Sarkar ‘98]
A. Ringwald (DESY) TAUP 2005, Zaragoza, Spain
– Super-GZK neutrinos – 18
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) TAUP 2005, Zaragoza, Spain
– Super-GZK neutrinos – 19
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
[Fodor,Katz ‘01]
A. Ringwald (DESY) TAUP 2005, Zaragoza, Spain
– Super-GZK neutrinos – 20
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) TAUP 2005, Zaragoza, Spain
– Super-GZK neutrinos – 21
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) TAUP 2005, Zaragoza, Spain
– Super-GZK neutrinos – 22
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) TAUP 2005, Zaragoza, Spain
– Super-GZK neutrinos – 23
Top-down scenarios for super-GZK neutrinos
• How natural?
– Superheavy dark matter: needsymmetry 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) TAUP 2005, Zaragoza, Spain
– Super-GZK neutrinos – 24
Top-down scenarios for super-GZK neutrinos
• How natural?
– Superheavy dark matter: needsymmetry 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
x
y
z
Reφ
Imφ
[Rajantie ‘03]
A. Ringwald (DESY) TAUP 2005, Zaragoza, Spain
– Super-GZK neutrinos – 25
Top-down scenarios for super-GZK neutrinos
• How natural?
– Superheavy dark matter: needsymmetry 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
NECKLACE
M M
M
M M
M
MS NETWORK
[Berezinsky ‘05]
A. Ringwald (DESY) TAUP 2005, Zaragoza, Spain
– Super-GZK neutrinos – 26
3. Fun with super-GZK neutrinos
• Super-GZK ν’s in reach!
• 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
A. Ringwald (DESY) TAUP 2005, Zaragoza, Spain
– Super-GZK neutrinos – 27
3. Fun with super-GZK neutrinos
• Super-GZK ν’s in reach!
• 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
A. Ringwald (DESY) TAUP 2005, Zaragoza, Spain
– Super-GZK neutrinos – 28
3. Fun with super-GZK neutrinos
• Super-GZK ν’s in reach!
• 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) TAUP 2005, Zaragoza, Spain
– Super-GZK neutrinos – 29
3. Fun with super-GZK neutrinos
• Super-GZK ν’s in reach!
• 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) TAUP 2005, Zaragoza, Spain
– Super-GZK neutrinos – 30
3. Fun with super-GZK neutrinos
• Super-GZK ν’s in reach!
• 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) TAUP 2005, Zaragoza, Spain
– Super-GZK neutrinos – 31Absorption of super-GZK neutrinos by the CνB
• At the resonance energies
Eres
ν =m2
Z
2mν
≃ 4× 1021 eV
(
eV
mν
)
super-GZK neutrinos annihilate withrelic neutrinos into Z bosons
⇒ Absorption dips in super-GZK neu-trino spectra
• Detectable within next decade if
– super-GZK neutrino flux close tocurrent observational bounds
– neutrino mass sufficiently large,mνi
>∼ 0.1 eV
A. Ringwald (DESY) TAUP 2005, Zaragoza, Spain
– Super-GZK neutrinos – 32Absorption of super-GZK neutrinos by the CνB
• At the resonance energies
Eres
ν =m2
Z
2mν
≃ 4× 1021 eV
(
eV
mν
)
super-GZK neutrinos annihilate withrelic neutrinos into Z bosons
⇒ Absorption dips in super-GZK neu-trino spectra
• Detectable within next decade if
– super-GZK neutrino flux close tocurrent observational bounds
– neutrino mass sufficiently large,mνi
>∼ 0.1 eV[Weiler ‘82]
A. Ringwald (DESY) TAUP 2005, Zaragoza, Spain
– Super-GZK neutrinos – 33Absorption of super-GZK neutrinos by the CνB
• At the resonance energies
Eres
ν =m2
Z
2mν
≃ 4× 1021 eV
(
eV
mν
)
super-GZK neutrinos annihilate withrelic neutrinos into Z bosons
⇒ Absorption dips in super-GZK neu-trino spectra
• Detectable within next decade if
– super-GZK neutrino flux close tocurrent observational bounds
– neutrino mass sufficiently large,mνi
>∼ 0.1 eV[Eberle,AR,Song,Weiler ‘04]
A. Ringwald (DESY) TAUP 2005, Zaragoza, Spain
– Super-GZK neutrinos – 34Absorption of super-GZK neutrinos by the CνB
• At the resonance energies
Eres
ν =m2
Z
2mν
≃ 4× 1021 eV
(
eV
mν
)
super-GZK neutrinos annihilate withrelic neutrinos into Z bosons
⇒ Absorption dips in super-GZK neu-trino spectra
• Detectable within next decade
– super-GZK neutrino flux close tocurrent observational bounds
– neutrino mass sufficiently large,mνi
>∼ 0.1 eV[Barenboim,Mena,Quigg ‘05]
A. Ringwald (DESY) TAUP 2005, Zaragoza, Spain
– Super-GZK neutrinos – 35Absorption of super-GZK neutrinos by the CνB
• At the resonance energies
Eres
ν =m2
Z
2mν
≃ 4× 1021 eV
(
eV
mν
)
super-GZK neutrinos annihilate withrelic neutrinos into Z bosons
⇒ Absorption dips in super-GZK neu-trino spectra
• Detectable within next decade if
– super-GZK neutrino flux close tocurrent observational bounds
– neutrino mass sufficiently large,mνi
>∼ 0.1 eV
20 21 22 23 24X
0.2
0.4
0.6
0.8
1.
Y21 22 23 24 25
X
0.2
0.4
0.6
0.8
1.
Y
[D’Olivo,Nellen,Sahu,Van Elewyck ‘05]
A. Ringwald (DESY) TAUP 2005, Zaragoza, Spain
– Super-GZK neutrinos – 36Absorption of super-GZK neutrinos by the CνB
• At the resonance energies
Eres
ν =m2
Z
2mν
≃ 4× 1021 eV
(
eV
mν
)
super-GZK neutrinos annihilate withrelic neutrinos into Z bosons
⇒ Absorption dips in super-GZK neu-trino spectra
• Detectable within next decade if
– mX >∼ 1015 GeV– super-GZK neutrino flux close to
current observational bounds
[Eberle,AR,Weiler,Wong,in prep.]
A. Ringwald (DESY) TAUP 2005, Zaragoza, Spain
– Super-GZK neutrinos – 37Absorption of super-GZK neutrinos by the CνB
• At the resonance energies
Eres
ν =m2
Z
2mν
≃ 4× 1021 eV
(
eV
mν
)
super-GZK neutrinos annihilate withrelic neutrinos into Z bosons
⇒ Absorption dips in super-GZK neu-trino spectra
• Detectable within next decade if
– mX >∼ 1015 GeV– super-GZK neutrino flux close to
current observational bounds
[Eberle,AR,Weiler,Wong,in prep.]
A. Ringwald (DESY) TAUP 2005, Zaragoza, Spain
– Super-GZK neutrinos – 38Absorption of super-GZK neutrinos by the CνB
• At the resonance energies
Eres
ν =m2
Z
2mν
≃ 4× 1021 eV
(
eV
mν
)
super-GZK neutrinos annihilate withrelic neutrinos into Z bosons
⇒ Absorption dips in super-GZK neu-trino spectra
• Detectable within next decade if
– mX >∼ 1015 GeV– super-GZK neutrino flux close to
current observational bounds
• Z-bursts as super-GZK recovery[Eberle,AR,Weiler,Wong,in prep.]
A. Ringwald (DESY) TAUP 2005, Zaragoza, Spain
– Super-GZK neutrinos – 39
4. Conclusions
• Exciting times for super-GZK neu-trinos:
– many observatories under con-struction
⇒ appreciable event samples
• Expect strong impact on
– astrophysics– particle physics– cosmology
A. Ringwald (DESY) TAUP 2005, Zaragoza, Spain
