HighEnergy Neutrino Astrophysics Tom Weiler Vanderbilt University Ole

High-Energy Neutrino Astrophysics Tom Weiler Vanderbilt University Ole Miss colloquium, Nov 04 Tom Weiler, Vanderbilt University

The Cosmic Ray Timeline 1912 1929 Hess (Austrian) balloons to 5 km, his sparks increase; also sees no change during solar eclipse Cloud chambers, and the birth of particle physics: 1933 Anderson’s positron; Kunze’s muon (Rostock) 1937 Anderson’s muon 1938 Auger’s remarkable Pe. V air-shower 1949 -54 Fermi’s “Doppler” acceleration via magnetized shocks 1966 3 K CMB discovered; GZK predict cutoff at 5 x 1019 e. V (But Linsley already reported (PRL) event at 1020 e. V) 1987 IMB/Kamiokande neutrinos from SN 87 a Ole Miss colloquium, Nov 04 Tom Weiler, Vanderbilt University

AUGER’s key discovery Auger, in 1938, separated two particle counters by a km high in the Swiss Alps (Jungfrau, near Bern), he discovered coincident signals. He calculated ETOT to be about 1015 e. V. His inference was correct. His energy was 107 times the prior record event, And now thought to be typical of emission from a SN remnant. 2/23/2021 Cospar 2004 3

1991 Fly’s Eye reports 3 x 1020 e. V, with proton-like profile; Akeno/AGASA Xpt begins mid-90 s. DUMAND taken off life-support; Baikal continues 90 s Super. K neutrinos from the sun (directional astro) 1996 AGASA reports event clustering within 2. 50 ang. res’n and: F(E 1020 e. V) ~ 1/km 2/century, with shower diameter ~ 5 km, N(e ) ~ 1011 2000 20 events at and above 1020 e. V 2001 Hi. Res withdraws 7 events; AGASA adds 6 (from z > 45 o); And the controversy has begun! Importantly, Auger gets first “light” 2002 AMANDA pushes to 1014 e. V thru-Earth neutrinos 2005 Auger Observatory data expected 2008 Extreme Universe Space Observatory (EUSO) ? Ole Miss colloquium, Nov 04 Tom Weiler, Vanderbilt University

CR Spectrum above a Te. V from Tom Gaisser VLHC (100 Te. V)2 Ole Miss colloquium, Nov 04 Tom Weiler, Vanderbilt University

Highest Energy Event The CR record energy is 3 x 1020 e. V (0. 3 Ze. V). Found by Fly’s Eye a decade ago (they got lucky!). This is truly a macroscopic energy: 3 x 1020 e. V = 50 Joules equivalent to a Roger Clemens fastball, a Tiger Woods tee shot, a Pete Sampras tennis serve, Or a speeding bullet. (Also to 12 Calories, which heats a gram of water by 12 o. C) Ole Miss colloquium, Nov 04 Tom Weiler, Vanderbilt University

3 x 1020 e. V = macroscopic 50 Joules Clemens does this with 1027 nucleons; Nature does this with one nucleon, 1027 times more efficient ! Ole Miss colloquium, Nov 04 Tom Weiler, Vanderbilt University

Fly’s Eye 3 x 1020 e. V event (1992) This longitudinal profile is consistent with a primary proton, but not with a primary photon; Disfavors “local” top-down sources such as massive Particle DK, topo-defects, Z-bursts, etc. Ole Miss colloquium, Nov 04 100 billion e+e- pairs at xmax ~ 800 g/cm 2 Tom Weiler, Vanderbilt University

EE Neutrinos are young Liberated at T=Mev, t= 1 sec Depends on energy (Lorentz boost) Consider a 1020 e. V neutrino. Lorentz factor = 1021 for mn = 0. 1 e. V. Age of Uni is 1018 sec, But age of n is 1018/1021 sec = 1 millisecond ! And it doesn’t even see the stream of radiation rushing past it – untouched ! Ole Miss colloquium, Nov 04 Tom Weiler, Vanderbilt University

Hillas Plot -- coherence length= B x L Ole Miss colloquium, Nov 04 Tom Weiler, Vanderbilt University

Size matters EUSO ~ 300 x AGASA ~ 10 x Auger EUSO (Instantaneous) ~3000 x AGASA ~ 100 x Auger Ole Miss colloquium, Nov 04 Tom Weiler, Vanderbilt University

Extreme Universe Space Observatory 2009 EUSO onboard the ISS (Or Not!) 20102012 Hundredth anniversary of Hess – EUSO finishes three-year data-taking Ole Miss colloquium, Nov 04 Tom Weiler, Vanderbilt University

“clear moonless nights” Or New York State power blackout Ole Miss colloquium, Nov 04 Tom Weiler, Vanderbilt University

Orbiting Wide-angle Lens (OWL) 3000 events/year above 1020 e. V and UHE Neutrinos! Ole Miss colloquium, Nov 04 Tom Weiler, Vanderbilt University

n HAS event rate is small e. g. FCR at 1020 e. V implies 10 -2 events/yr; Ole Miss colloquium, Nov 04 Tom Weiler, Vanderbilt University

AGASA Spectrum: Ee. V to Ze. V AGASA, July 2002 Ole Miss colloquium, Nov 04 Tom Weiler, Vanderbilt University

Greisen-Zatsepin-Kuzmin and the Cosmic-Ray Wall Photo-pion production off CMB p+ cmb p/n+ -resonance multi-pions Ole Miss colloquium, Nov 04 Tom Weiler, Vanderbilt University

Hi. Res vs. AGASA UHE spectrum Flys. Eye event goes here discovery opportunity GZK recovery ? Z-burst uncovery ? EUSO reach x 103 better Ole Miss colloquium, Nov 04 Tom Weiler, Vanderbilt University

AGASA hot-spots -- Data red: E > 4 1019 e. V green: E > 1020 e. V Cluster Component ~ E -1. 8± 0. 5 Neutrinos will point better Ole Miss colloquium, Nov 04 Tom Weiler, Vanderbilt University

AGASA hot-spots -- numbers Within 2. 5 degree circles, AGASA identifies six doublet, one triplet, Out of 57 events; Opening the angle to just 2. 6 degrees, AGASA identifies seven doublets, two triplets; Source number ~ N 12/2 N 2 ~ 270 to 50%, weighting with GZK suppression, ~ 10 -5 /Mpc 3 for source density Haverah Park contributes two more paired events in AGASA directions. NOT corroborated by Hi. Res. Ole Miss colloquium, Nov 04 Tom Weiler, Vanderbilt University

Berezinsky et al Xgal proton flux Mass-composition data (Hi. Res 2002) Theory threshold for pg 2. 7 K pe+e- and data (knee) are at 1017. 6 e. V. Xgal proton dominance begins at 1018 e. V, not 1019 e. V ! Fn ~ 50 x Waxman-Bahcall AMANDA/RICE/EAS-sensitive !! (AGHW, 2004) Ole Miss colloquium, Nov 04 Tom Weiler, Vanderbilt University

AMANDA to 100 Te. V Ole Miss colloquium, Nov 04 Tom Weiler, Vanderbilt University

AMANDA/Ice. Cube nm event Ole Miss colloquium, Nov 04 Tom Weiler, Vanderbilt University

Xgal proton fit huge n flux low Xgal dominance flux, with no evolution WB fluxes AGHW, hep-ph/04010003 xp is pion energy/CR energy at source (1 for WB “limit”); xz is cosmic evolution factor, 0. 6 (no) to 3. 0 (SFR) Ole Miss colloquium, Nov 04 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 Ole Miss colloquium, Nov 04 Tom Weiler, Vanderbilt University

n diagnostic of astro-engines: pp p vs. pg p The process ne+e-- W-- is resonant at 6. 4 Pe. V; Ice. Cube will have flavor ID, and E/E of 25%, and so can measure On-Res/Off-Res ratio. pp make nearly equal p+p- nm: ne: ne = 2: 2: 1: 1 flavor democracy, ne = 1/6 total pg via + make p+ nm: ne = 1: 1: 1 (no ne) ne = 1/15 total Ice. Cube can resolve this (AGHW, Ar. Xiv this week) Ole Miss colloquium, Nov 04 Tom Weiler, Vanderbilt University

The cosmic n flavor-mixing theorem If theta 32 is maximal (it is), And if Re(Ue 3) 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. ne: nm: nt = 1 : 1 at Earth Ole Miss colloquium, Nov 04 Tom Weiler, Vanderbilt University

Democracy Broken: 1. n decay (15 minutes of fame) 2. Vacuum resonance (Ma. Va. Ns, LIV vector) 3. Pseudo-Dirac n oscillations 4. Source dynamics (w/ Farzan) Ole Miss colloquium, Nov 04 Tom Weiler, Vanderbilt University

Neutrino Decay -- Models, Signatures, and Reach Ole Miss colloquium, Nov 04 Tom Weiler, Vanderbilt University

“Essentially Guaranteed” Xgal n Flux Hi. Res 2004 fit: Green: galactic component Red: Xgal component Evolution parameter 2. 8 +/- 0. 3 n Cosmogenic ’s: Fn(Ep/5/4) = Fp(E>5 1019) x 20 Ole Miss colloquium, Nov 04 Tom Weiler, Vanderbilt University

“Essentially Guaranteed” Xgal Cosmogenic n Flux n Cosmogenic ’s: Fn(Ep/5/4) = Fp(E>5 1019) x 20 graphs from Semikoz and Sigl Ole Miss colloquium, Nov 04 Tom Weiler, Vanderbilt University

“Essentially Guaranteed” High-Energy Galactic Neutrino Flux ctn = 10 kpc (En / Ee. V) and En / En ~ Q / mn ~ 0. 8 x 10 -3 En ~ Pe. V, for En ~ Ee. V Ole Miss colloquium, Nov 04 Tom Weiler, Vanderbilt University

Comparing to “guaranteed” cosmogenic flux, Galactic beam (here) is higher ! “More Guaranteed” Icecube atmos background in 1 o circle is just 1. 5 events/yr, 3. 5 events offers 95% CL detection in 1 yr; Calculated signal is 4 nm /yr and 16 ne+nt showers/yr. Conclude that in a few years, Ice. Cube attains 5 s discovery sensitivity for Fe n ne nm, Providing “smoking ice” for GP neutron hypothesis. Ole Miss colloquium, Nov 04 Tom Weiler, Vanderbilt University

Relic Neutrino density – me. V astrophysics Neutrino density from CMB density Ole Miss colloquium, Nov 04 Tom Weiler, Vanderbilt University

Resonant Neutrino Annihilation Mean-Free-Path From Fargion, Mele, Salis Ole Miss colloquium, Nov 04 l=(nn sn)-1 = 40 DH/h 70 (neglecting higher densities at earlier times) Tom Weiler, Vanderbilt University

Escher’s Angels and Devils” Looking back, nn~(1+z)3, And so the absorption is greatly Enhanced for n’s from high-z sources Ole Miss colloquium, Nov 04 Tom Weiler, Vanderbilt University

Neutrino mass-spectroscopy: absorption and emission The only possibility to directly infer the relic n density Ole Miss colloquium, Nov 04 Tom Weiler, Vanderbilt University

n-mass spectroscopy Ole Miss colloquium, Nov 04 zmax=2, 5, 20 (top to bottom), n-a=2 (bottom-up acceleration) Eberle, Ringwald, Song, TJW, 2004 Tom Weiler, Vanderbilt University

Dips & sobering realism hidden MX=4 1014 and 1016 Ge. V, to explain >GZK w/ Z-bursts; n mass = 0. 2 (0. 4) e. V - dashed (solid); Error bars – per energy decade, by 2013, for flux saturating present limits Ole Miss colloquium, Nov 04 Tom Weiler, Vanderbilt University

Z-bursts TJW, 1982; Revival – 1997 ~ 50 Mpc Ole Miss colloquium, Nov 04 Tom Weiler, Vanderbilt University

Fitted Z-burst (Emission) Flux Ole Miss colloquium, Nov 04 Tom Weiler, Vanderbilt University

Nu-mass limit for Z-burst fitted to EECRs Ole Miss colloquium, Nov 04 Tom Weiler, Vanderbilt University

Hi. Res vs. AGASA UHE spectrum Flys. Eye event goes here discovery opportunity GZK recovery ? Z-burst uncovery ? EUSO reach x 103 Ole Miss colloquium, Nov 04 Tom Weiler, Vanderbilt University

Model Neutrino Fluxes and Future Limits Ole Miss colloquium, Nov 04 Tom Weiler, Vanderbilt University

View (Japanese) of Earth-Moon System n Ole Miss colloquium, Nov 04 radio Cherenkov Tom Weiler, Vanderbilt University

Summary Neutrino Astrophysics: – now in the hands of theorists (speculation) and engineers (construction) -- soon in the hands of experimenters (real data) Promise to reveal -- neutrino physics (cross-section, lifetime, pseudo. Dirac) -- extreme astrophysics (source dynamics, source environment) -- cosmology (Cn. B, Omega‘s) Next ten years will be critical, and, the deities willing, fruitful ! Ole Miss colloquium, Nov 04 Tom Weiler, Vanderbilt University