anita meeting uc irvine 23 november 2002 ehe cosmic rays, ehe neutrinos and gev- tev gamma rays...

ANITA MeetingUC Irvine

23 November 2002

EHE Cosmic Rays, EHE Neutrinos

and GeV- TeV Gamma rays

David Kieda

University of Utah

Department of Physics

24 November 2002ANITA Meeting UCI David Kieda, Utah

Outline

1) GZK energy Cosmic Ray Measurements

2) GZK energy Cosmic Ray Origin

3) EHE neutrino production

4) EHE neutrino fluxes

5) Conclusion


UHE/EHE Cosmic Ray Astrophysics

HiRes Fly’s Eye (2002)


EHE Cosmic Ray Astrophysics

Fly’s Eye Detector (Dugway, Utah)

Hires Fly’s Eye Detector (Dugway, Utah)


EHE Cosmic Ray Astrophysics

320 EeV Cosmic Ray: Energy beyond GZK cutoff (D. Bird et al Ap. J 441, 144 (1995))

GZK cutoff: (d>20 Mpc)

Greisen PRL 16, 748 (1966) Zatsepin & Kuzmin JETP Lett 4, 78 (1966)

0' pp CMB np CMB


EHE Cosmic Ray Spectrum

HiRes Fly’s Eye (2002)



AGASA Array (2002)



A simple energy rescale looks promising, But…..

Aertures are energy dependent (especially for HiRes & Fly’s Eye)

Bachall & Waxman (2002)

Discrepancy due to differences energy scale factors (within quoted systematics)?


EHE Cosmic Ray Arrival Directions

Cosmic Ray

Akeno (2000). Clustering random chance probabilty ~1% In conflict with HiRes experiment (similar exposure) Hamburg 2001).

Large Scale Anisotropy: Probe correlation with anisotropy of local Galactic population (SuperGalactic Plane) or Galactic Center, Galactic Plane.

>AGN, starburst, magentar, GRB populations correlated with luminous mass

>Dark Matter Halo: Annihilation, Z-burst of relic massive neutrinos

Small Scale Anisotropy: Event clustering with < 10 degree separation. Point source searches.

Competition between increasing particle rigidity and decreasing statistic>Narrow energy window?


EHE Cosmic Ray SourcesBottom-Up


EHE Cosmic Ray PropagationEffects

1) Quantum Gravity Lorentz violation eliminates GZK (Gonzales-Mestres 1999, 2000) *Reduced interaction cross section (smaller final product phase space)

*Reduced Lorentz boosted energy of CMB

-> Probe with time delay of TeV Gamma rays from AGN

2) Z-Burst Models: High Energy Neutrino interacts with heavy relic neutrino in Galactic DM halo (But isn’t this just making thing worse?)


EHE Cosmic Ray PropagationEffects

If CR are indeed extragalactic, and if GZK cutoff does exist,

pion decay leads to guaranteed neutrino flux.

0' pp CMB np CMB

Adapted from C. Spiering (2002).



AGN with Pair production creating dip at 10 EeV

V. Berezinsky et al (2002) eepp CMB '



Nearby Magnetars population (< 50 Mpc)

with PetaGauss B fields yields dip

Arons astro-ph/0208444


EHE Cosmic Ray SourcesTop-Down

Typical Topological defect fragmentation :

Production of gammas, e+/e-, neutrinos with fluxes substantially greater than the cosmic rays

(O. Kalashev et al 2002)


EHE Neutrinos

• Top-Down Models vs. Bottom up give strongly different predictions for Neutrino flux

• Absolute neutrino flux constrained by gamma/neutrino production ratio (GeV/TeV gamma measurements)

•Absolute neutrino flux constrained by absolute cosmic ray flux (Bachall & Waxman bound, Mannheim, Protheroe & Rachen bound)

Some wiggle room if sources are opaque to gammas/cosmic rays and/or large distances to CR sources

VERITAS, 2005 4 tel.2007 7 tel.

ANITA 2005 flight

MAGIC, 1 tel., 2003

GLAST2005 flight


EHE Neutrinos

Production:

•Direct production in Top-Down Models

(Topologcal defect decay, super-heavy dark matter annihilation, super-heavy X particle decay)

Peak Energy ~100 EeV


EHE Neutrinos

Production:

•Direct production in Top-Down Models

Z-burst (Gelmaini, Cline, others)

Peak Energy > 100 EeV


EHE Neutrinos

Production:

• Secondary interactions of CR & production/decay near

acceleration region at EHE CR source (AGN, GRB)

Peak energy ~ 10 PeV (Stecker and Salamon 1996)


EHE Cosmic Ray Backgroundfor Radio Cherenkov Measurements?

Shock Wave


EHE Neutrino Observations

C. Spiering (2002).

ANITA pushes EeV neutrino limits

>Well below diffuse gamma/MPR bounds

>Approaches W&B bond


Conclusions

Shock Wave

•Super GZK Cosmic rays Exist.

•Rate, energy spectrum, isotropy statistically limited

•Difficult to separate Top-Down vs. Bottom up models in cosmic ray properties

•TeV Gamma, BW & MPR bounds do not exclude a strongly peaked flux above 100 EeV.

•GZK+Universal EHE CR production yields predictable 10-100 EeV flux

•Absence of GZK production probably implies GQ Lorentz violation

•Confluence of next generation TeV gamma ray, high energy neutrino & high energy cosmic ray provide strong constraints.

•Radio observations by ANITA play a key role in the next 5-10 years.

anita meeting uc irvine 23 november 2002 ehe cosmic rays, ehe neutrinos and gev- tev gamma rays...

Documents

utah slide

eev cosmic ray

ehe cosmic rays

anita meeting uci outline

gzk energy cosmic ray

ehe neutrinos

anita meeting uc irvine

conclusion slide