c = cos θ sol , s = sin θ sol , θ sol ~ 35 o x = sin θ atm = cos θ atm , θ atm ~ 45 0
Post on 08-Feb-2016
34 Views
Preview:
DESCRIPTION
Transcript
Teresa Montaruli, 5 - 7 Apr. 2005Teresa Montaruli, 5 - 7 Apr. 2005
510:2:1 τμe ννν φ:φ:φ
i
ii UUP 2,
2, ||||
c = cosθsol, s = sinθsol, θsol~35o
x = sinθatm = cosθatm, θatm ~ 450
Δmatm=2.5 10-3 eV2, Δmsol=710-5 eV2
For astrophysical sources L>kpc : Δm2 L/2E » 1\\ ee
ee 60%60% 20%20% 20%20%
20%20% 40%40% 40%40%
20%20% 40%40% 40%40%
Beam dump when all s decay:
2158.04.02158.04.0
057.082.00
xcxsxxcxsx
scU
solar CHOOZ (reactor)
atmospheric
2.02.06.0 ee
Neutrino oscillations and astrophysical fluxesNeutrino oscillations and astrophysical fluxes
at Earth
0
p
ee
e
ji
ELmijjii
jieUUUUP,
2,
*,
*,,
2,
i
iiUUP 2,
2,
Other scenarios: neutron decay 2.02.06.0 ee
%2058.057.04.082.0 2222 eP
Teresa Montaruli, 5 - 7 Apr. 2005Teresa Montaruli, 5 - 7 Apr. 2005
Neutrino production: top downNeutrino production: top downDecay of neutrons in sources Decay or annihilation of supermassive relic of Big Bang 1024 eV = 1015 GeV ~ MGUT (monopoles, topological defects, vibrating strings…)Resonant UHE neutrino interactions on relic neutrinos (Z-bursts)
Guaranteed neutrinos: GZK Guaranteed neutrinos: GZK ssUHECR produce UHECR produce s s s s
s from CR interactions in the s from CR interactions in the Galactic plane Galactic plane
Can explain EHECRCan explain EHECR
Gelmini et al, PRD70, 2004
Teresa Montaruli, 5 - 7 Apr. 2005Teresa Montaruli, 5 - 7 Apr. 2005
Radio continuum 408 MHz – Bonn, Jodrell Banks & Parks
Infrared COBE / DIRBE
Near Infrared COBE / DIRBE
Optical Photomosaic - Lausten et al. X-Ray 0.25, 0.75, 1.5 keV – ROSAT / PSPC Gamma Ray >100 MeV – CGRO / EGRET
The Galactic PlaneThe Galactic Plane
Neutrinos ANTARES ?
Teresa Montaruli, 5 - 7 Apr. 2005Teresa Montaruli, 5 - 7 Apr. 2005
8.5 kpc
15 – 20 kpc
Halo1 – 20 kpc
Galactic plane~ 1 kpc
The GalaxyThe Galaxy
spiral arms
Bulge
Halo
Ring + barGalactic center
Sun
1 pc = 3.3 ly
Theorical hypothesis
Propagation
Equilibrium between CR, B and ISM.
Electromagnetic interactions
• Diffusion on magnetic field and galactic winds
• Reacceleration
• Energy losses
• Spallation
•Neutrinos from pp collisions
• Decays
SunSun
Teresa Montaruli, 5 - 7 Apr. 2005Teresa Montaruli, 5 - 7 Apr. 2005
observationsobservations EGRET observed a diffuse emission 100MeV-10 GeV from Galactic Centre EGRET observed a diffuse emission 100MeV-10 GeV from Galactic Centre
region (300 pc): excess > factor 10 around 1 GeV region (300 pc): excess > factor 10 around 1 GeV INTEGRAL: resolved 91 point sources. 90% of ‘diffuse’ flux can be due to INTEGRAL: resolved 91 point sources. 90% of ‘diffuse’ flux can be due to
point sources <100 keVpoint sources <100 keV Milagro: discovery of TeV emission (astr-ph/0502303)Milagro: discovery of TeV emission (astr-ph/0502303) 4.54.5 excess from |b|<5˚ and l excess from |b|<5˚ and l[40˚,100˚][40˚,100˚] Covered pond with 2 layers of PMTs, from relative timing 0.75Covered pond with 2 layers of PMTs, from relative timing 0.75˚ shower direction ˚ shower direction
resolution, gamma-hadron discrimination based on shape of Cherenkov light resolution, gamma-hadron discrimination based on shape of Cherenkov light emitted by showersemitted by showers
Milagro(>1TeV)=5.1 ·10-10 cm-2 s-1 sr-1
Steeper than EGRET alone 2.51 0.05
2.612.61±0.07±0.07
Teresa Montaruli, 5 - 7 Apr. 2005Teresa Montaruli, 5 - 7 Apr. 2005
observationsobservationsExtreme models Extreme models =-(2.4-2.9) (hard electron disfavoured)s follow primary spectrum ( decay dominates over interactions)New model in Strong, Moskalenko, and Reimer, astro-ph/0406254
Figure: Strong, Moskalenko, and Reimer, astro-ph/0406254
red = from 0
INTEGRAL: flux from point sourcesINTEGRAL: flux from point sources
Teresa Montaruli, 5 - 7 Apr. 2005Teresa Montaruli, 5 - 7 Apr. 2005
Extreme ModelsExtreme ModelsHard nucleus model E-2.4
Model HN
TeV
GeV
γ=2.4
EAdE
Ed .)( Gamma from π0
Nu mu + anti nu mu
Hard electron model E-2.9
Model HEMNTeV
GeV
γ=2.94
For E-2.4 20 years of ANTARES to have 88% discovery prob
Teresa Montaruli, 5 - 7 Apr. 2005Teresa Montaruli, 5 - 7 Apr. 2005
Galactic CentreGalactic Centre High matter density and activityHigh matter density and activity compact radio source Sgr A* possibly associated to black hole ~3 10compact radio source Sgr A* possibly associated to black hole ~3 106 6 MMsunsun in in
the centerthe center Sgr A East SNRSgr A East SNR
HESS (6.1 4.7h/9.2 11.8 h)
HESS TeV- spectrum in disagreement with the other experiments Variability? localization? HESS 1 arcmin around Sgr A*
Sgr A EastChandra & Radio
Sgr A*
95%68%
astro-ph/0408145
Four 12 m diameter telescopes running since ~ 1yr in Namibia (16 in the future?) Eth 100 GeV
Cherenkov light is emitted by showers induced by high-energy gamma rays This light is very faint - about 10 s/m2 at E=100 GeV - and the duration of the light flash is only a few nsec. Large mirrors, fast photon detectors and short signal-integration times are required to collect enough light from the shower, with minimal contamination from night-sky background light.
direction < 0.1
High Energy Stereoscopic System
Galactic point SourcesGalactic point SourcesThe case of RXJ1713.7-The case of RXJ1713.7-39463946
Open problem: elusive 0 produced in accelerated nuclei collisions with SN ambient material. Still not a clear evidence BUT…CANGAROO claim
ControversialReimer et al., A&A390,2002Incompatible with EGRET
Enomoto et al, Nature 2002
0
RXJ1713.7-3946RXJ1713.7-3946
RXJ1713.7-3946RXJ1713.7-3946Seen by HESSSeen by HESS
H.E.S.S.: full remnantCANGAROO: hotspot
Index 2.2±0.07±0.1
preliminary
Index 2.84±0.15±0.20
NBCANGAROO measures
the spectrum for the NW part of the rim, HESS for
the entire region
No cut-off in the HE tail of HESS spectrum favors 0 decay scenario respect to the case of em processesStudy of electron density and B can help
Teresa Montaruli, 5 - 7 Apr. 2005Teresa Montaruli, 5 - 7 Apr. 2005
MicroquasarsMicroquasarsGalactic X-ray binaries with radio relativistic jets Their structure make them similar to quasars but ~106 times smaller Most have bursting activity (hrs-days)Persistent: SS433 GX339-4
Neutrinos from p- interactions (photons from synchr. emissionof electrons accelerated in jet or from accretion disc)
Ljet : jet kinetic power (erg/s) δ : jet Doppler factor δ= γ(1- β cosθ) ηp : fraction of jet energy transferred to protons (~0.1) fπ : fraction of p energy transferred pions D : source distance
Teresa Montaruli, 5 - 7 Apr. 2005Teresa Montaruli, 5 - 7 Apr. 2005
Predictions Galactic sources Predictions Galactic sources SourceSourceTypeType
DistanceDistance(kpc)(kpc)
EE
(GeV)(GeV)NNμμ
(km(km-2-2 yr yr-1-1 ) )Ref.Ref.
SupernovaeSupernovaeShocksShockspulsarspulsars
10 10 101033
10102 2 101066
101055 101088
10 10 101088
10010050 50 1000 1000
100 100 1000 1000 10001000
Waxman & Loeb 2001Waxman & Loeb 2001Protheroe et al. 1998Protheroe et al. 1998
Beall & Bednarek 2002Beall & Bednarek 2002Nagataki 2004Nagataki 2004
PlerionsPlerions
CrabCrab
0.5 0.5 4.4 4.4
22
<< 10 103 3 101055
10103 3 55··101055
10103 3 55··101055
10103 3 55··10105 5
1010 101066
1 1 12 12 11a fewa few 11
4 4 14 14
Guetta & Amatto 2003Guetta & Amatto 2003Bednarek 2003Bednarek 2003
Bednarek & Protheroe 1997Bednarek & Protheroe 1997Bednarek 2003Bednarek 2003
Amato et al. 2003Amato et al. 2003
Shell SNRsShell SNRsSNR RX J1713.7SNR RX J1713.7
Sgr A EastSgr A East6688
101044
101055
4040 140140
Alvarez-Muñiz & Halzen 2002Alvarez-Muñiz & Halzen 2002
Pulsars + CloudsPulsars + CloudsGalactic CentreGalactic Centre
Cygnus OB2Cygnus OB288
1.71.7101044 101077
>> 10 1033
10104 4 101077
<< 101066
2 2 30 30a fewa few 0.50.544
Bednarek 2002Bednarek 2002Torres et al. 2004Torres et al. 2004Bednarek 2003Bednarek 2003
Anchordoqui et al. 2003Anchordoqui et al. 2003
Binary systemsBinary systemsA0535+26A0535+26 2.62.6 3 3 · · 10102 2 101033 a fewa few Anchordoqui et al. 2003Anchordoqui et al. 2003
MicroquasarsMicroquasars 1 1 10 10 101033 101055 1 1 300 300 Distefano et al. 2002Distefano et al. 2002
MagnetarsMagnetars 3 3 16 16 << 101055 1.7 (0.1/∆1.7 (0.1/∆Ω) (5/dΩ) (5/d22)) Zhang et al. 2003Zhang et al. 2003
Teresa Montaruli, 5 - 7 Apr. 2005Teresa Montaruli, 5 - 7 Apr. 2005
Isotropic Angular Distribution
Gamma-Ray BurstsGamma-Ray Bursts
Bimodal duration distribution
long to short bursts 3:1
Counting rates with time variable from GRB to
GRB
Vela-4 detects the 1Vela-4 detects the 1stst emission E emission E>0.1 MeV on July 2>0.1 MeV on July 2ndnd,1967 ,1967
BATSE (1 GRB/d, 3° error box, FoV 4 sr)EGRET (1 GRB/yr, 10 arcmin, E>30 MeV,FoV 0.6 sr)
1 arcmin = 1/60 deg1 arcmin = 1/60 deg
Teresa Montaruli, 5 - 7 Apr. 2005Teresa Montaruli, 5 - 7 Apr. 2005
BATSE observations on GRBsBATSE observations on GRBs
0β
0EE
α
E
EE,EEE,eEEN 0
Spectra
Parametri: , e E0
E0
Band et al.
E0200 keV
-2
-1
Teresa Montaruli, 5 - 7 Apr. 2005Teresa Montaruli, 5 - 7 Apr. 2005
BeppoBeppo-SAX and afterglows-SAX and afterglows
Determined in 5-8 h precise GRB position thanks to detection in X (WFC)
From optical afterglow spectrum redshift cosmological distance Emitted energy (isotropic) 1054 erg Beaming (light curve changes in slope):
= 1/EobsEemitted ~102-103
Eemitted~ 5 ·1050 erg
Beppo-SAX (54 GRBs/6yrs, 5’ error box, 40-700 keV, FoV 20 ˚ 20 ˚)
Xray afterglow discovery: delayed emission even after ~ 1d optical counterparts SN association: GRB980425-SN1998bw GRB030329-SN2003dh position coincidence and SN like spectrum in afterglowLong GRBs: stellar core collapse into a BH,accretes mass driving a relativistic jet thatpenetrates the mantle and produces GRBControversial: observation off-axis suppresses flux
Teresa Montaruli, 5 - 7 Apr. 2005Teresa Montaruli, 5 - 7 Apr. 2005
Current and future missionsCurrent and future missionsMissionMission Error box Rate Error box Rate
((˚) (GRB/yr)) (GRB/yr)GLASTGLAST <0.125 300<0.125 300
SWIFTSWIFT ~~0.004 2000.004 200
HETE-2HETE-2 ~~0.03 250.03 25
INTEGRALINTEGRAL <0.2 35<0.2 35
The Gamma-ray bursts Coordinate network GCN: The Gamma-ray bursts Coordinate network GCN: Distribution of alertsDistribution of alerts
Delay of satelliteDelay of satellitedata processing anddata processing andtransmission+transmissiontransmission+transmissionof alertsof alerts
Teresa Montaruli, 5 - 7 Apr. 2005Teresa Montaruli, 5 - 7 Apr. 2005
The fireball modelCompactness problem: the optical depth for pair production very high if initial energy Compactness problem: the optical depth for pair production very high if initial energy emitted from a volume with radius R emitted from a volume with radius R <c dt ~300 km with dt = variability time scale ~ ms <c dt ~300 km with dt = variability time scale ~ ms in in photons photons with the observed spectrum with the observed spectrum this would imply thermal spectra contrary t this would imply thermal spectra contrary t observationsobservations
Solution: relativistic motion Solution: relativistic motion dimension of source R dimension of source R <<22 c dt and E c dt and Eobsobs = = E Emitted mitted
A fireball (A fireball (, e, e, baryon loading <10, baryon loading <10-5 -5 MMsunsun to reach observed to reach observed ) forms due to the high ) forms due to the high energy density, that expands. When it becomes optically thin it emits the observed energy density, that expands. When it becomes optically thin it emits the observed radiation through the dissipation of particle kinetic energy into relativistic shocksradiation through the dissipation of particle kinetic energy into relativistic shocks
External shocks:External shocks: relativistic matter runs on external medium, interstellar or wind earlier relativistic matter runs on external medium, interstellar or wind earlier emitted by the progenitoremitted by the progenitor
Internal shocks:Internal shocks: inner engine emits inner engine emits many shells with different Lorentz many shells with different Lorentz factors colliding into one another, and factors colliding into one another, and thermalizing a fraction of their kinetic thermalizing a fraction of their kinetic energy energy
Review
Teresa Montaruli, 5 - 7 Apr. 2005Teresa Montaruli, 5 - 7 Apr. 2005
Active Galactic NucleiActive Galactic Nuclei
VLA image of Cygnus A
Rotating massive BH with jets along rotation axis with matter outflow + accretion disc Spectra have a thermal part due to synchrotron radiation of electrons in a magnetic field (UV bump at optical-UV frequencies)+non thermal componentextending up to 20 orders of magnitudeexplained by leptonic/hadronic modelsNeutrino production in p or pp processes
Teresa Montaruli, 5 - 7 Apr. 2005Teresa Montaruli, 5 - 7 Apr. 2005
Upper bounds on X-galactic fluxesUpper bounds on X-galactic fluxes
This bound does not apply to harder This bound does not apply to harder spectra or optically thickspectra or optically thick
Cosmic p accelerators produce CRs, ’s and ’s Ultimate bound of any scenario involving and production from s: diffuse extra-galactic background E2F< 6 10-7 GeV /cm2 s sr (EGRET) Measured UHECR flux provides most restrictive limit (Waxman & Bahcall (1999) - optically thin sources: nucleons from photohadronic interactions escape - CR flux above the ankle (>3 ·1018eV) are extragalactic protons with E-2 spectrum E2F< 4.5 10-8 GeV /(cm2 s sr)
Mannheim, Protheroe & Rachen (2000): Magnetic fields and uncertainties in photohadronic interactions of protons can largely affect the bound as these effects restrict number of protons able to escape
CR rate evolves with z
Teresa Montaruli, 5 - 7 Apr. 2005Teresa Montaruli, 5 - 7 Apr. 2005
Suggested referencesSuggested references
Halzen and Hooper, Rept.Prog.Phys.65:1025-1078,2002 Learned and Mannheim, Ann.Rev.Nucl.Part.Sci.50:679-749,2000 Burgio, Bednarek, TM, New Astron. Rev. 49, 2005 (galactic
point sources) http://arxiv.org/PS_cache/astro-ph/pdf/0405/0405503.pdf (GRBs) Books: Longair, High Energy Astrophysics Berezinski, Neutrino
Astrophysics 1995 These transparencies:
http://www.icecube.wisc.edu/~tmontaruli/
Teresa Montaruli, 5 - 7 Apr. 2005Teresa Montaruli, 5 - 7 Apr. 2005
Neutrino Detection PrincipleNeutrino Detection Principles are weekly interacting require large target mass andrequire large target mass andconversion into charged particleMarkov/ Greisen idea (1960)Markov/ Greisen idea (1960)
Target is surrounding matterTarget is surrounding matter M =M = RRS (ES (E = 1 TeV : R = 1 TeV : R = 2.5 = 2.5
km)km)
Events are upgoingEvents are upgoing
XN
)(
Muon neutrinosMuon neutrinosare the only topologyare the only topologyto allow source pointingto allow source pointingBut since But since s oscillate s oscillate other topologies shouldother topologies shouldbe considered thatbe considered thatallow to observe upper allow to observe upper skysky
Teresa Montaruli, 5 - 7 Apr. 2005Teresa Montaruli, 5 - 7 Apr. 2005
Energy lossesEnergy lossesIonization and atomic excitationIonization and atomic excitation: interactions with electrons in the media: interactions with electrons in the mediaContinuous processContinuous processmip: particles at the minimum of ionization mip: particles at the minimum of ionization 2 MeV/g/cm2 MeV/g/cm22
Radiative: discrete process and stochasticRadiative: discrete process and stochasticBremmsstrahlung:Bremmsstrahlung: radiation emitted by an radiation emitted by anaccelerated or decelerated particle throughaccelerated or decelerated particle throughthe field of an atomic nucleithe field of an atomic nucleiEnergy emitted Energy emitted 1/m1/m22
Pair production:Pair production: +N +N e e++ee--
Photonuclear : Photonuclear : inelastic interaction ofinelastic interaction ofmuons with nuclei, produces hadronic muons with nuclei, produces hadronic showersshowers
Teresa Montaruli, 5 - 7 Apr. 2005Teresa Montaruli, 5 - 7 Apr. 2005
The target massThe target mass
)/1log(11
00c
EE
EEb
dEbEa
dEdEdxR
Ionization Stochastic losses ~2 MeV/g/cm2 (dominate > 1TeV )
baEc / critical energy
Upgoing muons: much larger interaction volume than what is in the instrumented region
Pair production
bremsstrahlung
rockrock
ionizationphotonuclear
top related