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

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


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


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


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:


HiRes vs. AGASA UHE spectrum

discovery

opportunity

GZK recovery ?Z-burst discovery ?EUSO reach x 103

FlysEye event goes here


HAS event rate


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


“clear moonless nights”

Blackout_14aug03.jpeg


“Essentially Guaranteed”Xgal Cosmogenic Flux

Cosmogenic ’s:

F(Ep/5/4) = Fp(E>5 1019) x 20

graphs from Semikoz and Sigl


for comparison, AGN and Z-burst fluxes

an AGN prediction and Z-burst fit


Present and Imminent Limits on Neutrino Flux


Model Neutrino Fluxes and Future Limits

Eberle, Ringwald, Song, TJW


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 !


Resonant Neutrino Annihilation Mean-Free-Path

From Fargion, Mele, Salis

nDH/h70


Escher’s Angels and Devils”


Z-bursts

Mpc

TJW, 1982;Revival – 1997


Neutrino mass-spectroscopy: absorption and emission


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


-mass spectroscopy zmax=2, 5, 20 (top to bottom), n-=2(bottom-up acceleration)Eberle, Ringwald, Song, TJW, 2004


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


Fitted Z-burst (Emission) Flux

Gelmini, Varieschi, TJW


Nu-mass limit for Z-burst fitted to EECRs

Gelmini,

Varieschi,

TJW


Neutrino Mass tomography in the Local Super-galactic Cluster

(Fodor, Katz, Ringwald)


Upward and Horizontal Air-shower Rates Versus Neutrino Cross-section

HAS

UAS

Kusenko, TJW


Earth Absorption versus Neutrino Cross-Section


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/


The “Learned Plot”

Oscillation phase is. ( Lm2 / 4 E

Figureparameterizedby m2 / (eV)2


Neutrino Decay -- Models, Signatures, and Reach

P(survive)= e –t/ = e –(L/E)(m/0

)

Beacom, Bell, Hooper, Pakvasa, TJW


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>*


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


AMANDA/IceCube event


Flavor ratio Topology ratio Map


Sensitivity of 1 flavor-projection to MNS parameters


Final “remark”:

Is anyone driving to/by Nottingham East Midlands airport tomorrow morning?

I could use a ride.

Thank you.


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


CR Spectrum above a TeV

from Tom Gaisser

VLHC(100 TeV)2


Hillas Plot -- coherence length= B x L


Orbiting Wide-angle Lens (OWL)

3000 events/year above 1020eV

and UHE Neutrinos!


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


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


“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


“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 !


Schematic: AGN Unified Source Model

annotated by M. Voit


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


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


• 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:


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


e

Log m2

m1

m3

m2

It looks like this

m3

m2

m1

Or maybe …


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


Pseudo-Dirac Mass Spectrum

Beacom, Bell, Hooper, Learned, Pakvasa, TJW


View (Japanese) of Earth-Moon System

radio Cherenkov


Absorption Dips on Relic Nu’s


Xptl spectra in Z rest-frame Boosted spectra in relic nu frame

(from Fodor, Katz, Ringwald)

Spectra: pi 2 gamma vs. nucleon


The finger of god


Does this look natural?

Or a firefly with a lit-up butt?


Model fluxes (Protheroe review)

atmosphere

AGN

GRB GZK

pIsm

SMPs

TDs MGUT

GeV


Protheroe Summary Fluxes

Documents

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