looking beyond the standard model with energetic cosmic...

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 – 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



• 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]









• It works [www.auger.org]


– 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









n



[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]









n



[Greisen;Zatsepin,Kuzmin ‘67][Ahlers et al. ‘05]



• 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.]










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









p

π+

µ+

e+

νµ

ν̄µ

νe

n

SHO

CK

[Ahlers PhD in prep.]










[Ahlers et al. ‘05]




• 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]





scattering at√





⋄ 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]





scattering at√





⋄ 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]





scattering at√





⋄ 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]



“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]



Strongly interacting neutrino scenarios

• Bounds exploiting searches for dee-ply-penetrating particles applicableas long as σνN


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]




• 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




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]



Top-down scenarios for super-GZK neutrinos

• Existence of superheavy particleswith 1012 GeV



• 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]











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]











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+





• 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






– 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-



x

y

z

Reφ

Imφ

[Rajantie ‘03]






– 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-



NECKLACE

M M

M

M M

M

MS NETWORK

[Berezinsky ‘05]






– 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-



SO(10)1

−→ 4C 2L 2R

8>>>>>>>>>>>>>>>>>>>>>>>>>:

1−→ 3C 2L 2R 1B−L

8



• 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.]








√s≫ LHC

– cosmology


neutrino background









√s≫ LHC

– cosmology


neutrino background [Barbot,Drees ‘02]








√s≫ LHC

– cosmology


neutrino background[Tu ‘04]








√s≫ LHC

– cosmology


neutrino background (CνB)








√s≫ LHC

– cosmology











√s≫ LHC

– cosmology



[AR,L. Schrempp ‘06]



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


looking beyond the standard model with energetic cosmic...

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