Transcript New Physics with 1020 eV Neutrinos, and Advantages of Space-Based Observation Tom Weiler Vanderbilt University Cosmos at Airlie, May 21-24, 2006 Tom Weiler, Vanderbilt University.

New Physics with 1020 eV Neutrinos,
and
Advantages of Space-Based Observation
Tom Weiler
Vanderbilt University
Cosmos at Airlie, May 21-24, 2006
Tom Weiler,
Vanderbilt University
Cosmic Photon- Proton-Spectra
sun
SN87a
Neutrino
Incognito
hadron wall?
no wall a’tall
Cosmos at Airlie, May 21-24, 2006
Tom Weiler,
Vanderbilt University
CR Spectrum above a TeV
from Tom Gaisser
50 Joules
VLHC
(100 TeV)2
Cosmos at Airlie, May 21-24, 2006
Tom Weiler,
Vanderbilt University
3 x1020 eV = macroscopic 50 Joules
Clemens does this with 1027 nucleons;
Nature does this with one nucleon,
1027 times better pitcher !
Cosmos at Airlie, May 21-24, 2006
Tom Weiler,
Vanderbilt University
General Remarks on Neutrinos
Existence of Xgal neutrinos inferred from CR spectrum, up to 1020 eV,
and similarly, Galactic up to 1018 eV,
Need gigaton (km3) mass (volume) for TeV to PeV detection [e.g. IceCube Xpt]
but a teraton of mass at 1019 eV
 SPACE-BASED
[e.g. EUSO Xpt]
Neutrino eyes see farther ( z>1 ),
and deeper (into compact objects) than gamma-photons,
and straighter
than HECRs,
with no absorption at (almost) any energy
Cosmos at Airlie, May 21-24, 2006
Tom Weiler,
Vanderbilt University
Neutrinos versus Cosmic-Rays and Photons
ns come from central engines
- near Rs of massive BHs
- even from dense “hidden” sources
cf. ns vs. gs from the sun
ns not affected by cosmic radiation
(except for annihilation resonance)
ns not bent by magnetic fields
- enables neutrino astronomy
Also, besides Energy and Direction, n’s carry Flavor
Cosmos at Airlie, May 21-24, 2006
Tom Weiler,
Vanderbilt University
EE Neutrinos are young
Consider a 1020 eV neutrino.
Lorentz factor = 1021 for mn = 0.1 eV.
Age of Uni is 1018 sec,
But age of n is 1018/1021 sec = 1 millsec !
And it doesn’t even see the stream of radiation
rushing past it – untouched !
Cosmos at Airlie, May 21-24, 2006
Tom Weiler,
Vanderbilt University
Extreme Energy (EE) Neutrino Sources
Bottom-Up “Zevatrons”
- givens
Cosmogenics
~1019 eV
·
AGNs
·
GRBs
·
Hidden vs. Transparent (the thick/thin debate)
·
·
·
·
·
Top-Down “EE-trons”
Topological Defects
Wimpzillas, M ~H(post-inflation) ~1022 eV
Msee-saw
MGUT
And even MPlanck
- pure speculation
Other:
Mirror-Matter mixing
Multiverse Leakage (Brane-bridges)
- impure thoughts
Cosmos at Airlie, May 21-24, 2006
~ 1023 eV
~ 1025 eV
~ 1028 eV
Tom Weiler,
Vanderbilt University
Protheroe Summary Fluxes
Cosmogenic
n’s:
Fn(Ep/5/4) = Fp(E>5 1019) x 20
Cosmos at Airlie, May 21-24, 2006
Tom Weiler,
Vanderbilt University
In this biz, Size matters
EUSO ~ 300 x AGASA ~ 15 x Auger
EUSO (Instantaneous) ~3000 x AGASA ~ 100 x Auger
Exposure
10000
Exposure
1000
AGASA
HiRes
Auger
EUSO
100
10
1
90 92 94 96 98 00 02 04 06 08 10 12 14
19 19 19 19 19 20 20 20 20 20 20 20 20
Year
Cosmos at Airlie, May 21-24, 2006
Tom Weiler,
Vanderbilt University
Extreme Universe Space Observatory
2009
EUSO onboard the ISS (Or Not!)
2012
Hundredth anniversary of Hess
– EUSO finishes three-year data-taking
Cosmos at Airlie, May 21-24, 2006
Tom Weiler,
Vanderbilt University
“clear moonless nights”
Blackout_14aug03.jpeg
Or New York State
power blackout
Cosmos at Airlie, May 21-24, 2006
Tom Weiler,
Vanderbilt University
Orbiting Wide-angle Lens (OWL)
3000 CR events/year
above 1020eV
and UHE Neutrinos!
Cosmos at Airlie, May 21-24, 2006
Tom Weiler,
Vanderbilt University
Goldstone Lunar Radio (Cherenkov) Experiment (GLUE)
GLUE is related to
RICE, FORTE, and ANITA,
and eventually,
to Lofar
n
and SalSa
radio
Cherenkov
Or better, a lunar orbiting antenna – “Moonita”
Cosmos at Airlie, May 21-24, 2006
Tom Weiler,
Vanderbilt University
Model Neutrino Fluxes and Future Limits
GLUE, RICE, Forte
,Auger, Anita, EUSO
From Eberle, AR, Song, TJW;
Semikoz and Sigl
Cosmos at Airlie, May 21-24, 2006
Tom Weiler,
Vanderbilt University
Neutrino cross-section measurement
Neutrinos at 1020 eV probe the structure of the nucleon
at unprecedented small-x values ;
Provides new QCD information
CM energy at HERA is 0.3 TeV;
while at En~ 1020 eV, Nature gives us Ecm ~ PeV!
And so probes new thresholds,
e.g. SUSY, X-Dimensions, TeV-scale Gravity,
EW Instantons (NonPert. EW), …
Reminder: LHC Ecm =14 TeV, and ILC Ecm =0.5 TeV
Cosmos at Airlie, May 21-24, 2006
Tom Weiler,
Vanderbilt University
n-N cross-section at 1020 eV
Cosmos at Airlie, May 21-24, 2006
Tom Weiler,
Vanderbilt University
Can’t Lose Thm for Space-based
Whatever the weak cross-section,
get robust event rate from HAS or UAS!
and
Get measurement of
neutrino cross-section
(peak angle also gives snN)
A. Kusenko, TJW (PRL2002)
Cosmos at Airlie, May 21-24, 2006
Tom Weiler,
Vanderbilt University
Earth Absorption
versus
Neutrino Cross-Section
~ HERA value
At Ecm=0.3 TeV
Cosmos at Airlie, May 21-24, 2006
Tom Weiler,
Vanderbilt University
Upward and Horizontal Air-shower Rates Versus Neutrino
Cross-section
HAS
UAS
Cosmos at Airlie, May 21-24, 2006
Tom Weiler,
Vanderbilt University
Palomares-Ruiz, Irimia, TJW, Phys Rev D (2006), 33pp.
solid lines are water, dashed lines are land
Volume favors space-based over land-based by one or more orders of magnitude;
for UAS, water also favors space-based by one or more orders of magnitude
Cosmos at Airlie, May 21-24, 2006
Tom Weiler,
Vanderbilt University
Summary
High-Energy Neutrino Astrophysics
can be done
only from Space
Let’s do it !
Cosmos at Airlie, May 21-24, 2006
Tom Weiler,
Vanderbilt University