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Peter MészárosPennsylvania State University
Astrophysical Sources of TeV to GZK neutrinos
Energy (eV)
Rad
io
CM
B
Vis
ible
GeV
-r
ays
1 TeV
Flu
x 400 microwave photons per cm3
[slides: Halzen 03]
TeV sources!
cosmic rays
/////////////////
++CMB,IRCMB,IR ee++ ++ e e--
• Photons above Photons above 1 TeV1 TeV do not do not reach us from reach us from
beyond 10-30 Milion light-years, beyond 10-30 Milion light-years, due to their due to their
interaction with IR diffuse interaction with IR diffuse background light. background light.
• Photons abovePhotons above 10103 3 TeVTeV energy energy do not reach do not reach
us from the edge of our galaxy us from the edge of our galaxy because of interaction with the because of interaction with the microwave background.microwave background.
Cosmic Cosmic Ray Ray
spectrumspectrumAtmospheric
neutrinos
Extragalactic flux sets scale for manyaccelerator models
CR spectrum
GZK cutoff or not ?
[Slides: Waxman 04]
Acceleration toAcceleration to 10 102121eV?eV?
~102 Joules ~ 0.01 MGUT
dense regions with exceptionalgravitational force creating relativisticflows of charged particles, e.g.
•coalescing black holes/neutron stars•dense cores of exploding stars•supermassive black holes
CR acceleration
For a few seconds, a GRB dominates the gamma-ray brightness of
the entire Universe
Fig. Credit: Tyce DeYoung
[Waxman 95]
[Frail et al 00]
GZK Sources
• Sources: GRB √ ; AGN.... #?
• Rate: RGRB (z=0)~ 0.5 Gpc-3 yr-1
~ 0.5 10-3 (D/100 Mpc)-3 yr-1
• But, arrival time dispersion:
tdis~3 107yr (B/10-9 G)2 (B/10 Mpc)
(D/100MPC)2 (Ep/1020 eV)-2
• NGRB(>Ep, <D) ~ R. tdisp
~104 B-92 B10 D100
2 Ep202
• GZK event rate: ~ 1 /Km2 /100 yr)
QuickTime™ and aTIFF (LZW) decompressor
are needed to see this picture.
[Waxman 95]
CR data vs. model
[slide: Waxman 05]
(see talk by S. Coutu)
Next : how and where are neutrino beams made ??
[ Halzen 02 ]
Lab
radiationenvelopingblack hole
black hole
Irrespective of the cosmic-ray sources, some fraction will produceIrrespective of the cosmic-ray sources, some fraction will produce pions (and neutrinos) as they escape from the acceleration sitepions (and neutrinos) as they escape from the acceleration site• through hadronic collisions with gasthrough hadronic collisions with gas• through photoproduction with ambient photonsthrough photoproduction with ambient photonsCosmic rays interact with interstellar light/matter even if theyCosmic rays interact with interstellar light/matter even if they escape the sourceescape the source
• Transparent:Transparent:protons (EeV cosmic-rays) ~ photons protons (EeV cosmic-rays) ~ photons (TeV point sources) ~neutrinos(TeV point sources) ~neutrinos
• Obscured sourcesObscured sources• Hidden sourcesHidden sources
Unlike gammas, neutrinos provide unambiguous evidence for cosmic ray acceleration!
Sources:Sources:
Detection principleDetection principle
p
+ N +X
Neutrino passes through the
earth
Interacts near the detector to
produce a muon
Cherenkov light is
observed
Cherenkov light from muons and cascadesCherenkov light from muons and cascades
• Maximum likelihood method
• Use expected time profiles of photon flight times
cascade
Reconstruction
muon
NNevents events ~ ~ PP-->-->Area TimeArea Time
Neutrino flux Neutrino flux requiredrequired to observe N events: to observe N events:
5x10-12
Area (km2) Time (yr)
ergcm2/s
nntarget target RangeRange
~ 10~ 10-4 -4 for 100 TeV neutrinosfor 100 TeV neutrinos
Detection Probability:Detection Probability:
Nevents=
Aerial view of South Pole
AMANDA
Dome
Skiway(for planes!)
SouthPole
1 km
ANTARTICA, South Pole Station:
Amanda & IceCubeANTARTICA, South Pole Station:
Amanda & IceCube
IceCube
Building AMANDA: The Optical Building AMANDA: The Optical Module and the StringModule and the String
• Hot-water-drill 2km-deep holes & insert strings of PMTs in pressure vessels.
– AMANDA-B10: 302 PMTs, completed in 1997• Old & new A-B10
results presented– AMANDA-II: 677
PMTs, completed in 2000• Prelimin. results
presented • AMANDA challenges:
– Natural medium– Remote location– Unfettered bkgd.
source– Prototype detector
AMANDA-II
The AMANDA Detector
IceCubeIceCube
1400 m1400 m
2400 m2400 m
AMANDAAMANDA
South PoleSouth Pole
IceTopIceTop
RunwayRunway• 80 Strings80 Strings
• 4800 PMT4800 PMT • Instrumented volume: Instrumented volume:
1 km3 (1 Gton)1 km3 (1 Gton)
• IceCube is designed to IceCube is designed to detect neutrinos of all detect neutrinos of all flavors at energies from flavors at energies from 101077 eV (SN) to 10 eV (SN) to 102020 eV eV
even neutronseven neutrons do not escapedo not escape
neutronsneutrons escapeescape
neutrinos associated with the source of the cosmic rays?neutrinos associated with the source of the cosmic rays?
Neutrino ID (solid)Neutrino ID (solid)Energy and angle (shaded)Energy and angle (shaded)
Neu
trin
o fl
avor
•FilledFilled area: particle id, direction, energyarea: particle id, direction, energy
•Shaded area: energy onlyShaded area: energy only
KM3NeT
• Km3 water Cherenkov detector• Deployment approx. 2010• Complement ICECUBE: sc,abs~(100,10) H20, sc,abs~(20,100) Ice
• Northern site: at lower E , complementary sky coverage
•EU collaboration•Site :Mediterranean Sea• based on: NESTOR, NEMO, ANTARES
p + ,p → UHE , • If protons present in (baryonic) jet → p+ Fermi accelerated (as are e-)• p, → → ,→e,,e, (-res.: Ep E 0.3 GeV2 in jet frame)
→ E,br 1014 eV for MeV s (int. shock)
→ E,br 1018 eV for 100 eV s (ext. rev. sh.) ICECUBE • →0 →2 → cascade GLAST, ACTs.. (Waxman-Bahcall 1997;99; Boettcher-Dermer 1998; 00; )
• Test hadronic content of jets (are they pure MHD/e , or baryonic …?)• Test acceleration physics (injection effic., e, B..) • Test scattering length (magnetic inhomog. scale?..or non-Fermi?..)• Test shock radius: cascade cut-off:
~ GeV (internal shock) ; ~ TeV (ext shock/IGM)
→ photon cut-off: diagnostic for int. vs. ext-rev shock
UHE in GRB 6 possible collapsar GRB -sites
• 1) at collapse, make GW + thermal s (MeV)• 2) If jet outflow is baryonic, have p,n → p,n relative drift, pp/pn collisions → inelastic nuclear collisions → VHE (GeV)
• 3 Int. shocks while jet is inside can accel. protons → p, pp/pn collisions
→ UHE (TeV)• 4 Int. shocks outside accel. protons → p collisions → UHE (100 TeV)
• 5) ← Ext. rev. shock → EeV (1018 eV)
• 6) If supranova shell present outside (SN ocurred >2 days before GRB?) → p, pp of jet protons on shell targets → UHE (> TeV) [..now constrained]
e- capt p,n
p, pp
p
1,2
3,4
5,6
“Hadronic” GRB Fireballs:
Thermal p,n decoupling → VHE ,• p,n in fireball move together while tpn < texp (rad. acts on p, elastic scatt.
couples p,n)• p,n decouple when tpn >texp , where pn1, vrel c, pn inelastic; this occurs
for > ~400 (Derishev etal 99; Bahcall,Meszaros 00; Fuller etal 00)
• Inelastic pn ±,e±,e ,
→ 0 → 2 : 5-10 GeV → ICECUBE?
det @ z1, R7/yr from all GRB, but only if larger PMT density
-rays: 02 , → GLAST,
10 GeV, detect @ z < 0.1
(Bahcall & Meszaros 2000 PRL 85:1362); Lemoine 2002; Beloborodov, 2002
pn
pn
rdec
While jet is inside progenitor:
(2) Jet inside star: GRB , Precursor
• Jet propagating through progenitor, BEFORE emerging from stellar envelope, can have int. shocks which accel. p+ → p on unobserved X-rays , → ±, pp, pn on stellar envelope → ±,
few TeV neutrino precursor • If progenitor has H-layer R1012 cm (BSG) →
Rate( , TeV ) prec > Rate( , 100 TeV )int.shock
( easier to detect in ICECUBE )• but, if WR (He core), R1011 cm → Rate( , TeV) prec < Rate( , 100 TeV ) int.shock
→ test progen. size (e.g. @ high z : popIII?)
• If jet DOES NOT escape ⇒ “choked” jet, s escape, s don’t → “hidden
source”
• If jet break-out: → photon flashes
(3) Blue - spectrum: ~100 TeV p,→ from shocks outside star
Meszaros , Waxman 01 PRL 17 1102
Razzaque, Mészáros, Waxman 03 PRD 68, 3OO1)
WR
H
When jet is outside progenitor star: GRB internal & external shocks
s from p in internal & external shocks in GRB
• Shocks accelerate p+ (as well as the e- which produce MeV )
-res.: E’p E’ 0.3GeV2 in comoving frame, in lab:
→ Ep ≥ 3x106 Γ22 GeV
→ E ≥ 1.5x102 Γ22 TeV
• Internal shock p,MeV
→ ~100 TeV s• External shock p,UV
→ ~ 0.1-1 EeV s
• Diffuse flux: detect in km3Waxman, Bahcall 97 PRL
GRB 030329: precursor(& pre-SN shell?) with ICECUBE
Razzaque, Mészáros, Waxman 03 PRD 69, 23001
Burst of L1051 erg/s, ESN 1052.5 erg, @ z0.17, 68o
Prob.of interaction
Flux of
Core collapse SN : slow jets? • Maybe all core coll. (or Ib/c) SN
resemble (watered-down) GRB?• Evidence for asymmetric expansion
of c.c. (Ib/c) SNR: slow jets Γ~ few ?
• If so, accel protons while jet inside star, p→πμ→ μ (TeV)
• Diffuse flux: might be interesting (if 100% SNII make jets), but, more interestingly:• individual SN in nearby (2-3 Mpc)
gals, e.g. M82, NGC253, detectable (if have slow jets), at a rate ~ 1 SN/few yr, fluence ~ 100 up-muons/SN, negligible background, in km3
detectors - ICECUBE, KM3NeT
Razzaque, Mészáros, Waxman ‘04, PRL 93, 181101; (err: ‘05, PRL 94, 9903)Ando, Beacom (Kaons from pp - astro-ph/0502521)
Diffuse UHE from pop.III collapse• At z~5-30(?) pop.III , M ~ 30-300 M , core coll →BH+ accr.• Buried jets→p→ , → -bursts (but: dep. on stellar rot.rate)• Eiso~1054-1056 (?) erg (dep. on BH mass, dM/dt)• Detect high z star formation,
primordial IMF • Recent (8/04) : can constrain
w. AMANDA latest results: → Eiso~1056 erg only for ≤1%, → Eiso≥1054 erg for ≤ 50% !
Schneider, Guetta, Ferrara aph/0201342
Recent AMANDA u.l.
AGN as UHE sources• Big brother of GRB: massive
BH (107-108 Msun ) fed by an accretion disk → jet –• But, jet jet,agn ~10-20 (while grb ~ 102-103 )• UV photons from disk; in
addition, line clouds provide extra photons
(+back-scatter)• Typical (“leptonic”) model: SSC (sync-self-compton);
SEC(sync-exter.compton)
Radio-loud blazars (jet nearly head-on):
Mrk 501 • 1997 flare: TeV;
(GeV: upper lim only w EGRET)
• GeV detected sometime @ quiescence
• ←Typical “astrophysical” SSC or ESC
“leptonic” jet
model fit
• But: competing
“hadronic” jet
model fits
Radio-loud hadronic Blazar models (PSB-proton synchrotron blazar - -ray spectrum from cascades)
• Full : synchrotron SED (target photons)• Dash: p-sync. casc.; Dash-3 dot: ±-sync. casc; Dots:
0 casc; Dash-dot: ± casc(Muecke, et al, Apph, astro-ph/0206164 )
Mrk 501 : protypical HBL
• a) PSB: Quiet state • b) PSB: Flare state e-sync targets + p-sync + p, casacdes, casacdes & sync (Muecke et al,
a-ph/0206164)
• c) → LEP:Flare state → e-sync + e-Inv. Compton scatt (Ghisellini et al, e.g.
A&A 386, 833 (2002) etc – “standard” astrophysical. picture
Radio-quiet (core) AGN s
• AGN are powered by accretion
on massive (106-108 M ) BHs • 90% of AGNs are radio-quiet
(no jets), core X-ray• Core emission model: aborted
jet → cloud collisions →shocks →
p accel → p → Diffuse flux: already
constrained by latest AMANDA results
Alvarez-Muñiz & Mészáros, 2004, PRD 70, 123001
Other Implications of GRB UHE • Special relativity: simultaneity of arrival of , tested to t < 1 s (10-3 s in short bursts)• Time delay due to i mass:
t (i ) ~ 10-12 (D/100Mpc)(Ei/100TeV)-2(mi /eV)2 s (whereas for SN 1987a t (i )~ 10-8 s )
• Vacuum oscillations: at source exp. N ~ 2Ne
at observer exp. ratios , upgoing appearance• → sensitive to
m2 <10-16 (E/100TeV)(100Mpc/D) eV2
(for m 0.1 eV due to finite pion life mixing is caused by decoherence rather than oscillation)
GZK neutrinos:
GZKbrick wall
GZK neutrinos probably 2nd most likely source of UHE neutrinos!
they are a guaranteed source!!
•Two predictions–1. There is a brick wall for the highest energy cosmic rays. We should observe energies below about 1020 eV.–2. Reactions that limit the cosmic ray energies produce neutrinos as a by-product
•Ultra-high energy cosmic rays:–Origin; unknown, but
•Standard Model: –Ordinary charged particles accelerated by distant sources: AGN, GRBs…
•If so: GZK neutrinos are the signature
–Probably necessary and sufficient to confirm standard GZK model
(Courtesy A. Silvestri via D. Saltzberg)
What do we need for a GZK detector?
Askaryan process: coherent radio Cherenkov emission:EM cascades produce a charge asymmetry radio pulseProcess is coherent Quadratic rise of power with cascade energyNeutrinos can shower in radio-transparent media:
air, ice, rock salt, etc.RF economy of scale very competitive for giant detectors
How can we get the ~100-1000 km3 sr yr exposures needed to detect GZK neutrinos at an acceptable rate?
ANSWER
Standard model GZK: : <1 per km2 per day
Only 1 in 500 interact in ice
QUESTION:
Both AMANDA-II or IceCube may expect to see 1 event every 2 years in its fiducial volume—requires astronomical level of patience!
from GZK CRs to GZK s
Seckel & Stanev astroph/050244
2 ≠CR models same GZK fit
≠ GZK flux
ANtarctic Impulsive Transient Antenna
• NASA funding started 2003 for full launch in 2006 • ANITA-lite succesfully launched & tested Dec 2003
600 km radius,1.1 million km2
ANITA concept
Antarctic Ice at f<1GHz, T<-30C Nearly Lossless RF transmission Negligible scattering largest homogenous, RF-transmissive solid mass in the world!
EUSO• ISS project
ESA/NASA/RSA/JSA; precursor for OWL (free-flyer)
• 5.1019 – 1021 eV EECRs, EENUs
• Monocular 2.5m Fresnel lens, measure EAS through atm. fluor
• Thresh: 3.1019 eV; Effic. @ 1020 eV : 300-1000 event/yr
• Launch: 2010-12, but: shuttle ?• Possibly: JSA
unmanned shuttle
CR & bounds
Summary: UHE • GRBs 1020 eV protons
- Predictions 103 km2 area detectors
- Experiments: HiRes, Auger, EUSO/OWL
• GRBs 10 GeV, 1 Tev, 100 TeV, 1018 eV ’s
- Flux 1 Gton detectors
- Exp’s: AMANDA, IceCube, Antares, Nestor, Nemo detection
- GRBs: CR puzzle, GRB progenitors & physics
- physics: appearance
- Cross sections at E > LHC