Neutrino Astrophysics: PeV to ZeV (with some whacky particle physics)

1
Neutrino Astrophysics PeV to ZeV (with some
whacky particle physics)
For the viewing pleasure of Alan, the only
person to make me regret that I dont play
(cough) golf!

• Tom Weiler
• -- Vanderbilt University CERN

thanks Alan, and Francis
2
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
3
Cosmic Photo- Proto-Spectra
SN87a
sun
Neutrino Incognito
hadron wall?
no wall atall
4
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
1023 eV      MGUT
1025 eV      And even MPlanck
1028 eV   Other - ????  
Mirror-Matter mixing Multiverse Leakage
5
HiRes vs. AGASA UHE spectrum
FlysEye event goes here
discovery
opportunity
GZK recovery ? Z-burst discovery ? EUSO reach x
103
6
n HAS event rate
7
Size matters
EUSO 300 x AGASA 10 x Auger EUSO
(Instantaneous) 3000 x AGASA 100 x Auger
8
clear moonless nights
9
Essentially GuaranteedXgal Cosmogenic n Flux
Cosmogenic ns Fn(Ep/5/4) Fp(Egt5 1019) x 20
graphs from Semikoz and Sigl
10
for comparison, AGN and Z-burst fluxes
an AGN prediction
and Z-burst fit
11
Present and Imminent Limits on Neutrino Flux
12
Model Neutrino Fluxes and Future Limits
Eberle, Ringwald, Song, TJW
13
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 doesnt even see the stream of
radiation rushing past it untouched !
14
Resonant Neutrino Annihilation Mean-Free-Path
From Fargion, Mele, Salis
l(nn sn)-1 40 DH/h70
15
Eschers Angels and Devils
 
16
Z-bursts
TJW, 1982 Revival 1997
50 Mpc
17
Neutrino mass-spectroscopy absorption and
emission
18
What we think we know about neutrino mass
Log m2
19
n-mass spectroscopy
zmax2, 5, 20 (top to bottom), n-a2 (bottom-up
acceleration) Eberle, Ringwald, Song, TJW, 2004
20
Dips sobering realism

• hidden MX4 1014 and 1016 GeV,
• to explain gtGZK w/ Z-bursts
• mass 0.2 (0.4) eV - dashed (solid)
• Error bars per energy decade, by 2013,
• for flux saturating present limits

21
Fitted Z-burst (Emission) Flux
Gelmini, Varieschi, TJW


22
Nu-mass limit for Z-burst fitted to EECRs

Gelmini, Varieschi, TJW
23
Neutrino Mass tomography in the Local
Super-galactic Cluster
(Fodor, Katz, Ringwald)
24
Upward and Horizontal Air-shower Rates Versus
Neutrino Cross-section
Kusenko, TJW
HAS
UAS
25
Earth Absorption versus Neutrino Cross-Section
26
Cant 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 snN)
Kusenko, TJW hep-ph/
27
The Learned Plot
Oscillation phase is . ( L dm2 / 4 En )
Figure parameterized by dm2 / (eV)2
28
Neutrino Decay -- Models, Signatures, and Reach
P(survive) e t/t e (L/E)(m/t0)
Beacom, Bell, Hooper, Pakvasa, TJW
29
PMNS neutrino-mixing matrix
Weak-interaction and mass vectors point
differently nkgtUki nigt, or Uki ltni nkgt
ltnk nigt
30
The cosmic n flavor-mixing thm
If theta32 is maximal (it is), And if Re(Ue3) is
minimal (it is), Then nm and nt
equilibrate Further, if initial ne flux is
1/3 (as from pion-muon decay chain), Then all
three flavors equilibrate.
nenmnt 1 1 1 at Earth
31
AMANDA/IceCube nm event
32
Flavor ratio ? Topology ratio Map
33
Sensitivity of n1 flavor-projection to
MNS parameters
34
Final remarkIs anyone driving to/by
Nottingham East Midlands airport tomorrow
morning?I could use a ride.Thank you.
35
1991 Flys Eye reports 3x1020 eV, with
proton-like profile Akeno/AGASA Xpt
begins 1993 Baikal sees underwater
neutrinos  mid-90s DUMAND taken off
life-support  90s SuperK neutrinos from the sun
(directional astro)  1996 AGASA reports event
clustering within 2.50 ang. resn 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 gt 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  
36
CR Spectrum above a TeV
from Tom Gaisser
VLHC (100 TeV)2
37
Hillas Plot -- coherence length B x L
38
Orbiting Wide-angle Lens (OWL)
3000 events/year above 1020eV and UHE
Neutrinos!
39
WINDOWS on the UNIVERSE
Crab Nebula
Stars Galaxies
Galaxy Clusters
Big Bang
Planets
Black Holes
Neutron Stars
Distant Galaxies
Gamma Ray Bursts
10-3
1
103
106
109
1012
Limited Vision
E L E C T R O M A G N E T I C S P E C T R U M
Radio ?-wave
IR /Visible/ UV
X-rays
?-rays
VHE ?-rays
Accelerators
Reactors, Nuclear Decays
N E U T R I N O S P E C
T R U M
1018
1015
10-3
1
103
106
109
1012
1021 eV
Sun
Crab Nebula
Produced by New Particles
Atmospheric Neutrinos
Big Bang
Stars
Dark Matter
Produced by Ultra-High-Energy Cosmic Rays
Neutron Stars
Supermassive Black Holes
Supernovae
Gamma Ray Bursts
Underground Lab
IceCube
Auger EUSO radio
From Turner Olinto
40
EUSO

• Hundredth anniversary of V. Hess
• EUSO finishes three-year data-taking

FOV 2 105 km2, Aperture 106 km2 sr, and 2
teratons of visible mass
41
Essentially Guaranteed High-Energy Galactic
Neutrino Flux
ctn 10 kpc (En / EeV) and En / En Q / mn
0.8 x 10-3 ? En PeV, for En EeV
Anchordoqui, Goldberg, Halzen, TJW hep-ph/0311002
42
More Guaranteed
Comparing to guaranteed cosmogenic flux,
Galactic beam (here) is higher !
a signal in a km3.
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 nm /yr
and 16 nent showers/yr. Conclude that in a few
years, IceCube attains 5s discovery sensitivity
for Fe ? n ? ne ? nm, Providing smoking ice for
GP neutron hypothesis.
43
Schematic AGN Unified Source Model

• annotated by M. Voit

44
The TeV g-ray -- PeV n connection

• A handful of TeV g-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 gammas
• Hadrons pion production off gs and nucleons,
• with p0 ? g g (and p/- ? 2 nm ne e )
• Only the latter accommodates production of
  observed CRs !
• In the Unified Source Model, BL-Lacs, FR-Is,
• are all Accreting Super-Massive Black Holes

45
Nearest are Cen-A (3.4 Mpc) in South and M87 (16
Mpc) in North
Ergo, may be the best candidate Xgal neutrino
sources
The n-mixing thm predicts a nearly equal flux for
each flavor j, normalized to the g-ray flux as
(factor 2 from scaling energy bin)
The resulting n flux on Earth from Cen-A during a
bursting phase ( yr, Narrabri 4.5s, 1970s) is
? Prediction
46
And for M87

• From HEGRA, 4.1s, 98-99
• Consistent with Cen-A and 1/r2
• 2 events/yr in IceCube, similar to atmospheric
  background

The diffuse flux on Earth then follows
leading to
between bursts.
47
Auger neutrons form Cen-A
Since ctn 0.9 Mpc E20, Neutron survival
probability from Cen-A e 3.8/E20 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
48
Or maybe
It looks like this
Log m2
49
Dirac neutrino vs Majorana neutrino
Majorana
Dirac
Lorentz Boost, E, B
C P T
C P T
So is a Dirac just two Majoranas? Yes, iff the
two Majoranas are mass-degenerate and have
opposite CP parity
50
Pseudo-Dirac Mass Spectrum
Beacom, Bell, Hooper, Learned, Pakvasa, TJW
51
View (Japanese) of Earth-Moon System
n
radio Cherenkov
52
Absorption Dips on Relic Nus
53
Spectra pi ? 2 gamma vs. nucleon
Xptl spectra in Z rest-frame
Boosted spectra in relic nu frame
(from Fodor, Katz, Ringwald)
54
The finger of god
55
Does this look natural?
Or a firefly with a lit-up butt?
56
Model n fluxes (Protheroe review)
atmosphere
AGN
pgIsm
GRB
GZK
GeV
SMPs
TDs
MGUT
57
Protheroe Summary Fluxes
58
Galaxy Distribution 7-21 MpcVisible from the
southern site
59
Galaxy Distribution 7-21 MpcVisible from the
northern site
60
Auger neutrons form Cen-A
Since ctn 0.9 Mpc E20, Neutron survival
probability from Cen-A e 3.8/E20 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
61
Important to ask

1. Can flavor ratios be measured ?
2. What would NOT 111 mean ?

62
AMANDA/IceCube nm event
To be contrasted with localized shower event
63
Flavor ratio ? Topology ratio Map
64
Neutrino Decay -- Models, Signatures, and Reach
P(survive) e t/t e (L/E)(m/t0)
Beacom, Bell, Hooper, Pakvasa, TJW