neutrino astrophysics: pev to zev (with some whacky particle physics)
DESCRIPTION
Neutrino Astrophysics: PeV to ZeV (with some whacky particle physics). Tom Weiler -- Vanderbilt University & CERN *. For the viewing pleasure of Alan, the only person to make me regret that I don’t play (cough) golf!. * thanks Alan, and Francis. - PowerPoint PPT PresentationTRANSCRIPT
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
Neutrino Astrophysics: PeV to ZeV(with some whacky particle physics)
Tom Weiler
-- Vanderbilt University & CERN*
For the viewing pleasure of Alan, the only person to make me regret
that I don’t play (cough) golf!
* thanks Alan, and Francis
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
Neutrinos versus Cosmic-Rays and Photons
s come from central engines
- near Rs of massive BHs
- even from dense “hidden” sources
cf. s vs. s from the sun
s not affected by cosmic radiation(except for annihilation resonance)
s not bent by magnetic fields- enables neutrino astronomy
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
Cosmic Photo- Proto-Spectra
Rad
io
CM
B
Vis
ible
-ra
ys
CERN/Fermilab
x-ra
ysUV
IRCosmic-rays
TeV
-w
all
(after Ressell & Turner ‘90)
hadron wall?
no wall a’tall
sunSN87a NeutrinoIncognito
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
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 ~ 1023 eV
· MGUT ~ 1025 eV
· And even MPlanck ~ 1028 eV
Other: - ???? Mirror-Matter mixing Multiverse Leakage
Extreme Energy (EE) Neutrino Sources:
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
HiRes vs. AGASA UHE spectrum
discovery
opportunity
GZK recovery ?Z-burst discovery ?EUSO reach x 103
FlysEye event goes here
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
HAS event rate
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
Size mattersEUSO ~ 300 x AGASA ~ 10 x AugerEUSO (Instantaneous) ~3000 x AGASA ~ 100 x Auger
Exposure
1
10
100
1000
10000
Year
Expo
sure AGASA
HiResAugerEUSO
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
“clear moonless nights”
Blackout_14aug03.jpeg
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
“Essentially Guaranteed”Xgal Cosmogenic Flux
Cosmogenic ’s:
F(Ep/5/4) = Fp(E>5 1019) x 20
graphs from Semikoz and Sigl
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
for comparison, AGN and Z-burst fluxes
an AGN prediction and Z-burst fit
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
Present and Imminent Limits on Neutrino Flux
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
Model Neutrino Fluxes and Future Limits
Eberle, Ringwald, Song, TJW
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
EE Neutrinos are young
Consider a 1020 eV neutrino.
Lorentz factor = 1021 for m = 0.1 eV.
Age of Uni is 1018 sec,
But age of is 1018/1021 sec = 1 millsec !
And it doesn’t even see the stream of radiation rushing past it – untouched !
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
Resonant Neutrino Annihilation Mean-Free-Path
From Fargion, Mele, Salis
nDH/h70
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
Escher’s Angels and Devils”
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
Z-bursts
Mpc
TJW, 1982;Revival – 1997
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
Neutrino mass-spectroscopy: absorption and emission
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
e
Log m2
m1
m3
m2
m223 ~ 2.5 x 10-3 eV2
m212 ~ 7 x 10-5
eV2
It “probably” looks something like this
What we think we know about neutrino mass
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
-mass spectroscopy zmax=2, 5, 20 (top to bottom), n-=2(bottom-up acceleration)Eberle, Ringwald, Song, TJW, 2004
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
Dips & sobering realismhidden MX=4 1014 and 1016 GeV,
to explain >GZK w/ Z-bursts; mass = 0.2 (0.4) eV - dashed (solid);Error bars – per energy decade, by 2013,
for flux saturating present limits
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
Fitted Z-burst (Emission) Flux
Gelmini, Varieschi, TJW
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
Nu-mass limit for Z-burst fitted to EECRs
Gelmini,
Varieschi,
TJW
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
Neutrino Mass tomography in the Local Super-galactic Cluster
(Fodor, Katz, Ringwald)
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
Upward and Horizontal Air-shower Rates Versus Neutrino Cross-section
HAS
UAS
Kusenko, TJW
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
Earth Absorption versus Neutrino Cross-Section
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
Can’t Lose Thm
Whatever the weak cross-section, get robust event rate from HAS or UAS!
and
Get measurement of neutrino cross-section(peak angle also gives )
Kusenko, TJWhep-ph/
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
The “Learned Plot”
Oscillation phase is. ( Lm2 / 4 E
Figureparameterizedby m2 / (eV)2
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
Neutrino Decay -- Models, Signatures, and Reach
P(survive)= e –t/ = e –(L/E)(m/0
)
Beacom, Bell, Hooper, Pakvasa, TJW
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
PMNS neutrino-mixing matrix
ijijijij
τττ
μμμ
eee
li
sandcwhere
cs
sc
iδecs
sccs
sc
UUU
UUU
UUU
U
sin,cos
0
010
0
00
010
001
0
0
001
100
0
0
1313
1313
2323
23231212
1212
321
321
321
Weak-interaction and mass “vectors” point differently:|nk>=Uki |ni>, or Uki = <ni | nk> = <nk | ni>*
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
The cosmic flavor-mixing thm
If theta32 is maximal (it is),And if Re(Ue3) is minimal (it is),
Then and equilibrate;
Further, if initial e flux is 1/3
(as from pion-muon decay chain),Then all three flavors equilibrate. e:: = 1 : 1 : 1 at Earth
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
AMANDA/IceCube event
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
Flavor ratio Topology ratio Map
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
Sensitivity of 1 flavor-projection to MNS parameters
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
Final “remark”:
Is anyone driving to/by Nottingham East Midlands airport tomorrow morning?
I could use a ride.
Thank you.
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
1991 Fly’s Eye reports 3x1020 eV, with proton-like profile;
Akeno/AGASA Xpt begins
1993 Baikal sees underwater neutrinos
mid-90sDUMAND taken off life-support
90s SuperK neutrinos from the sun (directional astro)
1996 AGASA reports event clustering within 2.50 ang. res’n
and: F(E 1020 eV) ~ 1/km2/century,
with shower diameter ~ 5km, N(e) ~ 1011
2000 20 events at and above 1020 eV
2001 HiRes withdraws 7 events; AGASA adds 6 (from z > 45o);
And the controversy has begun!
Importantly, Auger gets first “light”
2002 AMANDA pushes to 1014 eV thru-Earth neutrinos
2005 Auger expected to go public
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
CR Spectrum above a TeV
from Tom Gaisser
VLHC(100 TeV)2
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
Hillas Plot -- coherence length= B x L
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
Orbiting Wide-angle Lens (OWL)
3000 events/year above 1020eV
and UHE Neutrinos!
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
WINDOWS on the WINDOWS on the UNIVERSEUNIVERSE
10-3
10181015
1 103 106 109 1012
1021 eV10-3 1 103 106 109 1012
E L E C T R O M A G N E T I C S P E C T R U M
N E U T R I N O S P E C T R U M
IR /Visible/ UV X-rays -rays VHE -raysRadio -wave
Big Bang
Stars & Galaxies
PlanetsBlack Holes
Crab Nebula
Galaxy Clusters
Big Bang
Sun
Stars
Neutron Stars Supermassive Black Holes
Gamma Ray Bursts
Produced by
Ultra-High-EnergyCosmic Rays
Limited
Vision
Produced by
New Particles
AcceleratorsReactors, Nuclear Decays
Crab Nebula
Supernovae
Dark Matter
DistantGalaxies
Underground Lab IceCube
Gamma Ray Bursts
Neutron Stars
AtmosphericNeutrinos
Auger EUSO radioFrom Turner & Olinto
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
EUSO
FOV = 2 105 km2,Aperture = 106 km2 sr,and 2 teratons of visible mass
2012 Hundredth anniversary of V. Hess
– EUSO finishes three-year data-taking
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
“Essentially Guaranteed” High-Energy Galactic Neutrino Flux
cn = 10 kpc (En / EeV)and
E/ En ~ Q / mn ~ 0.8 x 10-3
E ~ PeV, for En ~ EeV
Anchordoqui, Goldberg, Halzen, TJW;hep-ph/0311002
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
“More Guaranteed”
So, atmos background in 1o circle is just 1.5events/yr, 3.5 events offers 95% CL detection in 1 yr;
Calculated signal is 4 /yr and 16 e+ showers/yr.
Conclude that in a few years, IceCube attains 5discovery sensitivity for Fe n e Providing “smoking ice” for GP neutron hypothesis.
a signal in a km3.
Comparing to “guaranteed” cosmogenic flux, Galactic beam (here) is higher !
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
Schematic: AGN Unified Source Model
annotated by M. Voit
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
The TeV -ray -- PeV connectionA handful of TeV -ray emitters have been identified, all of the BL-Lac class, with a relativistic jet slightly off-set from the line of sight.
Two principle production mechanisms: Electrons: synchrotron on magnetic field,
or inverse Compton on gamma’s; Hadrons: pion production off ’s and nucleons,
with and 2+e + e )
Only the latter accommodates production of observed CRs !
In the Unified Source Model, BL-Lacs, FR-I’s, … are all Accreting Super-Massive Black Holes
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
Nearest are Cen-A (3.4 Mpc) in South and M87 (16 Mpc) in North
The -mixing thm predicts a nearly equal flux for each flavor
“j”, normalized to the -ray flux as (factor 2 from scaling energy bin)
The resulting flux on Earth from Cen-A during a bursting phase (~ yr, Narrabri 4.5, 1970s) is
Prediction:
Ergo, may be the best candidate Xgal neutrino sources
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
• From HEGRA, 4.1, 98-99• Consistent with Cen-A and 1/r2
• ~ 2 events/yr in IceCube, similar to atmospheric background
between bursts.
The diffuse flux on Earth then follows:
leading to:
And for M87:
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
Auger neutrons form Cen-A
Since cn = 0.9 Mpc E20,
Neutron survival probability from Cen-A = e –3.8/E
20
= 2% at 1020 eV= 15% at 2 1020 eV= 1/e at 3.8 1020 eV
Maybe 2 evts/yr at Auger, more at EUSO,with Glennys’ flux (Farrar-Piran)
Anchordoqui, Goldberg, TJW;hep-ph/01
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
e
Log m2
m1
m3
m2
It looks like this
m3
m2
m1
Or maybe …
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
R
L
R
L
R
L
C
P
T
C
P
T
Lorentz
Boost,
E, B
Majorana
Dirac neutrino vs Majorana neutrino
Dirac
So is a Dirac just two Majoranas?Yes, iff the two Majoranas are
mass-degenerate andhave opposite CP parity
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
Pseudo-Dirac Mass Spectrum
Beacom, Bell, Hooper, Learned, Pakvasa, TJW
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
View (Japanese) of Earth-Moon System
radio Cherenkov
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
Absorption Dips on Relic Nu’s
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
Xptl spectra in Z rest-frame Boosted spectra in relic nu frame
(from Fodor, Katz, Ringwald)
Spectra: pi 2 gamma vs. nucleon
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
The finger of god
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
Does this look natural?
Or a firefly with a lit-up butt?
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
Model fluxes (Protheroe review)
atmosphere
AGN
GRB GZK
pIsm
SMPs
TDs MGUT
GeV
AlanFest, 23July2004Tom Weiler, Vanderbilt & CERN
Protheroe Summary Fluxes