Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
Neutrinos – Ghost Particles of the UniverseNeutrinos
Ghost Particles of the UniverseNeutrinos
Ghost Particles of the Universe
Georg G. RaffeltMax-Planck-Institut für Physik, München, Germany
Georg G. RaffeltMax-Planck-Institut für Physik, München, Germany
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
Neutron
ProtonGravitation (Gravitons?)
Weak Interaction (W and Z Bosons)
Periodic System of Elementary Particles
Electromagnetic Interaction (Photon)
Strong Interaction (8 Gluons)
Down
Strange
Bottom
Electron
Muon
Tau
e-Neutrino
m-Neutrino
t-Neutrino nt
nm
nee
m
t
d
s
b
1st Family
2nd Family
3rd Family
Up
Charm
Top
u
c
t
Quarks Leptons
Charge -1/3
Down
Charge -1
Electron
Charge 0
e-Neutrino need
Charge +2/3
Up u
Higgs
Georg Raffelt, MPI Physics, Munich Colloquium, UNSW, Sydney, 4 March 2014
Where do Neutrinos Appear in Nature?
Nuclear Reactors
Particle Accelerators
Earth Atmosphere(Cosmic Rays)
Earth Crust(Natural Radioactivity)
Sun
Supernovae(Stellar Collapse) SN 1987A
Cosmic Big Bang (Today 330 n/cm3) Indirect Evidence
AstrophysicalAccelerators
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
Neutrinos from the Sun
Reaction-chains
Energy26.7 MeV
Helium
Solar radiation: 98 % light (photons) 2 % neutrinosAt Earth 66 billion neutrinos/cm2 sec
Hans Bethe (1906-2005, Nobel prize 1967)Thermonuclear reaction chains (1938)
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
Sun Glasses for Neutrinos?
8.3 light minutes
Several light years of lead needed to shield solar neutrinos
Bethe & Peierls 1934: … this evidently means that one will never be able to observe a neutrino.
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
First Detection (1954 – 1956)
Fred Reines(1918 – 1998)Nobel prize 1995
Clyde Cowan(1919 – 1974)
Detector prototype
Anti-Electron Neutrinosfrom Hanford Nuclear Reactor
3 Gammasin coincidence
𝝂𝐞 p
n Cd
e+¿ ¿ e−
g
g
g
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
First Measurement of Solar Neutrinos
600 tons ofPerchloroethylene
Homestake solar neutrino observatory (1967–2002)
Inverse beta decayof chlorine
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
2002 Physics Nobel Prize for Neutrino Astronomy
Ray Davis Jr.(1914–2006)
Masatoshi Koshiba(*1926)
“for pioneering contributions to astrophysics, inparticular for the detection of cosmic neutrinos”
Georg Raffelt, MPI Physics, Munich Colloquium, UNSW, Sydney, 4 March 2014
Cherenkov Effect
Water
Elastic scattering or CC reaction
NeutrinoLight
Light
Cherenkov Ring
Electron or Muon(Charged Particle)
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
Super-Kamiokande Neutrino Detector (Since 1996)
42 m
39.3 m
Super-Kamiokande: Sun in the Light of Neutrinos
ca. 60,000 solar neutrinos measured in Super-K (1996–2012)
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
Average (1970-1994) 2.56 0.16stat 0.16sys SNU(SNU = Solar Neutrino Unit = 1 Absorption / sec / 1036 Atoms) Theoretical Prediction 6-9 SNU“Solar Neutrino Problem” since 1968
Results of Chlorine Experiment (Homestake)ApJ 496:505, 1998
AverageRate
TheoreticalExpectation
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
Neutrino Flavor Oscillations
Bruno Pontecorvo(1913–1993)
Invented nu oscillations
Two-flavor mixing
Each mass eigenstate propagates as with Phase difference implies flavor oscillations
Oscillation Length
sin 2(2𝜃)Probability
z
(𝜈𝑒
𝜈𝜇)=(c os𝜃 sin 𝜃− sin 𝜃 c os 𝜃)(𝜈1𝜈2)
4𝜋 𝐸𝛿𝑚2 =2 .5m
𝐸MeV (eV𝛿𝑚
2
)
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
Oscillation of Reactor Neutrinos at KamLAND (Japan)Oscillation pattern for anti-electron neutrinos from
Japanese power reactors as a function of L/E
KamLAND Scintillatordetector (1000 t)
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
Atmospheric Neutrino Oscillations (1998)
Atmospheric neutrino oscillations show characteristic L/E variation
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
Long-Baseline (LBL) ExperimentsK2K Experiment(KEK to Kamiokande)measures preciseneutrino oscillationparameters.
Since then other LBLExperiments:• Minos (US)• Opera (Europe)• T2K (Japan)• Nova (US) (construction)
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
Q13 from Reactor Experiments (2012)
4MeV ͞e
sin22θ13 = 0.089 ± 0.010 (stat) ± 0.005 (syst)
0.113 ± 0.013 (stat) ± 0.019 (syst)
Daya Bay (China)
Reno (Korea)
0.086 ± 0.041 (stat) ± 0.030 (syst) Double Chooz (Europe)
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
v
Three-Flavor Neutrino Parameters
(𝜈𝑒
𝜈𝜇
𝜈𝜏)=(1 0 00 𝑐23 𝑠230 −𝑠23 𝑐23
)( 𝑐13 0 𝑒−𝑖 𝛿𝑠130 1 0
−𝑒𝑖 𝛿𝑠13 0 𝑐13)( 𝑐12 𝑠12 0−𝑠12 𝑐12 00 0 1)(
1 0 0
0 𝑒𝑖𝛼2
2 0
0 0 𝑒𝑖𝛼3
2)(𝜈1𝜈2𝜈3)
Three mixing angles , , (Euler angles for 3D rotation), ,a CP-violating “Dirac phase” , and two “Majorana phases” and
⏟⏟⏟⏟39∘<𝜃23<53
∘ 7∘<𝜃13<11∘ 33∘<𝜃12<37
∘ Relevant for 0n2b decayAtmospheric/LBL-Beams Reactor Solar/KamLAND
me t
me t
m t
1Sun
Normal
2
3
Atmosphere
me t
me t
m t
1Sun
Inverted
2
3
Atmosphere
72–80 meV2
2180–2640 meV2
Tasks and Open Questions• Precision for all angles• CP-violating phase d ?• Mass ordering ? (normal vs inverted)• Absolute masses ? (hierarchical vs degenerate)• Dirac or Majorana ?
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
Antineutrino Oscillations Different from Neutrinos?
Dirac phase causes different 3-flavor oscillationsfor neutrinos and antineutrinos
Distance [1000 km] for E = 1 GeV
same as
𝜈𝑒→𝜈𝜇
𝜈𝑒→𝜈𝜇
𝝂𝐞=𝑐12𝑐13𝝂𝟏+𝑠12𝑐13𝝂𝟐+𝑠13𝑒−𝑖 𝛿𝝂𝟑
𝝂𝐞=𝑐12𝑐13𝝂𝟏+𝑠12𝑐13𝝂𝟐+𝑠13𝑒+𝑖 𝛿𝝂𝟑
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
Neutrino CarabinerNamed for a subatomic particlewith almost zero mass, …
nGreek “nu”Now also in color
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
“Weighing” Neutrinos with KATRIN• Sensitive to common mass scale m for all flavors because of small mass differences from oscillations• Best limit from Mainz und Troitsk m < 2.2 eV (95% CL)• KATRIN can reach 0.2 eV• Under construction• Data taking to begin 2015/16• http://www.katrin.kit.edu
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
KATRIN Ante Portas (25 Nov 2006)
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
Weighing Neutrinos with the Universe
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
Cosmological Limit on Neutrino Masses
JETP Lett. 4 (1966) 120
Cosmic neutrino “sea” 112 cm-3 neutrinos + anti-neutrinos per flavor
Ω𝜈h2=∑ 𝑚𝜈
93 eV<0.25
For allstable flavors∑𝑚𝜈≲20eV
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
What is wrong with neutrino dark matter?
Galactic Phase Space (“Tremaine-Gunn-Limit”)Maximum mass density of a degenerateFermi gas
𝜌max=𝑚𝜈
𝑝max3
3𝜋 2⏟𝑛max
=𝑚𝜈 (𝑚𝜈𝑣escape )
3
3𝜋 2
Spiral galaxies mn > 20–40 eVDwarf galaxies mn > 100–200 eV
Neutrino Free Streaming (Collisionless Phase Mixing)
NeutrinosNeutrinos
Over-density
• At T < 1 MeV neutrino scattering in early universe is ineffective• Stream freely until non-relativistic• Wash out density contrasts on small scales
• Neutrinos are “Hot Dark Matter”• Ruled out by structure formation
Sky Map of Galaxies (XMASS XSC)
http://spider.ipac.caltech.edu/staff/jarrett/2mass/XSC/jarrett_allsky.html
Georg Raffelt, MPI Physics, Munich Colloquium, UNSW, Sydney, 4 March 2014
Structure Formation with Hot Dark Matter
Neutrinos with Smn = 6.9 eVStandard LCDM Model
Structure fromation simulated with Gadget codeCube size 256 Mpc at zero redshift
Troels Haugbølle, http://users-phys.au.dk/haugboel
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
Neutrino Mass Limits Post Planck (2013)
Ade et al. (Planck Collaboration), arXiv:1303.5076
CMB alone constraining Smn CMB + BAO constraining Smn + Neff
CMB + BAO limit: Sm n < 0.23 eV (95% CL)
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
Future Cosmological Neutrino Mass Sensitivity
Basse, Bjælde, Hamann, Hannestad & Wong, arXiv:1304.2321:Dark energy and neutrino constraints from a future EUCLID-like survey
ESA’s Euclid satellite to be launched in 2020Precision measurement of theuniverse out to redshift of 2
Pin down the neutrino mass in the sky!
Georg Raffelt, MPI Physics, Munich Colloquium, UNSW, Sydney, 4 March 2014
Neutrinos as Astrophysical Messengers
Nuclear Reactors
Particle Accelerators
Earth Atmosphere(Cosmic Rays)
Earth Crust(Natural Radioactivity)
Sun
Supernovae(Stellar Collapse) SN 1987A
Cosmic Big Bang (Today 330 n/cm3) Indirect Evidence
AstrophysicalAccelerators
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
Geo Neutrinos: What is it all about?
We know surprisingly little aboutthe Earth’s interior• Deepest drill hole 12 km• Samples of crust for chemical analysis available (e.g. vulcanoes)• Reconstructed density profile from seismic measurements• Heat flux from measured temperature gradient 30-44 TW (Expectation from canonical BSE model 19 TW from crust and mantle, nothing from core)
• Neutrinos escape unscathed• Carry information about chemical composition, radioactive energy production or even a hypothetical reactor in the Earth’s core
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
Geo NeutrinosExpected Geoneutrino Flux
Reactor Background
KamLAND Scintillator-Detector (1000 t)
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
Reactor On-Off KamLAND Data
KamLAND Collaboration, arXiv:1303.4667 (2013)
ScintillatorPurification
KamLAND-ZenConstruction
2011 EarthquakeReactors shut down
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
KamLAND Geo-Neutrino Flux
KamLAND Collaboration, arXiv:1303.4667 (2013)
Geoneutrino events(U/Th = 3.9 fixed)
Separately free fitting:U 116 eventsTh 8 events
Beginning ofneutrino geophysics!
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
Applied Anti-Neutrino Physics (AAP)
Applied Anti-Neutrino Physics (AAP)Annual Conference Series since 2004• Neutrino geophysics• Reactor monitoring (“Neutrinos for Peace”)
• Relatively small detectors can measure nuclear activity without intrusion• Of interest for monitoring by International Atomic Energy Agency (Monitors fissile material in civil nuclear cycles)
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
Cosmic Rays
Air Shower: 1019 eV primary particle 100 billion secondary particles at sea level Victor Hess (1911/12)
100 years later we are still asking
What are the sourcesfor the primarycosmic rays?
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
Neutrino Beams: Heaven and Earth
Target:Protons or Photons
Approx. equal fluxes ofphotons & neutrinos
Equal neutrino fluxesin all flavors due tooscillationsF. Halzen (2002)
𝜋 0
𝜸
𝜋±
𝝁𝝂𝝁
𝒆𝝂𝒆𝝂𝝁
𝝂𝒆𝝂𝝁𝝂𝝉
p
Georg Raffelt, MPI Physics, Munich Colloquium, UNSW, Sydney, 4 March 2014
Nucleus of the Active Galaxy NGC 4261
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
IceCube Neutrino Telescope at the South PoleInstrumentation of 1 km3 antarcticice with 5000 photo multiplierscompleted December 2010
Georg Raffelt, MPI Physics, Munich Colloquium, UNSW, Sydney, 4 March 2014
Two High-Energy Events in IceCube
Ernie ~ 1.1 PeV Bert ~ 1.3 PeV
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
Ernie & Bert and 26 Additional Events in IceCubeSignificance of all 28 events: 4.1s, Background
Ernie & Bert
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
SN 1006 over Sydney
Supernova Neutrinos
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
Crab Nebula
Georg Raffelt, MPI Physics, Munich Colloquium, UNSW, Sydney, 4 March 2014
Stellar Collapse and Supernova Explosion
Hydrogen Burning
Main-sequence star Helium-burning star
HeliumBurning
HydrogenBurning
Onion structure
Degenerate iron core: r 109 g cm-3
T 1010 K MFe 1.5 Msun
RFe 3000 km
Collapse (implosion)
Georg Raffelt, MPI Physics, Munich Colloquium, UNSW, Sydney, 4 March 2014
Stellar Collapse and Supernova Explosion
Collapse (implosion)ExplosionNewborn Neutron Star
50 km
Proto-Neutron Star
r rnuc = 3 1014 g cm-3
T 30 MeV
Georg Raffelt, MPI Physics, Munich Colloquium, UNSW, Sydney, 4 March 2014
Stellar Collapse and Supernova Explosion
Newborn Neutron Star
50 km
Proto-Neutron Star
r rnuc = 3 1014 g cm-3
T 30 MeV
Neutrinocooling bydiffusion
Gravitational binding energy
Eb 3 1053 erg 17% MSUN c2
This shows up as 99% Neutrinos 1% Kinetic energy of explosion 0.01% Photons, outshine host galaxy
Neutrino luminosity
Ln 3 1053 erg / 3 sec 3 1019 LSUN
While it lasts, outshines the entire visible universe
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
Diffuse Supernova Neutrino Background (DSNB)
• A few core collapses per second in the visible universe
• Emitted energy density ~ extra galactic background light ~ 10% of CMB density
• Detectable flux at Earth mostly from redshift
• Confirm star-formation rate
• Nu emission from average core collapse & black-hole formation
• Pushing frontiers of neutrino astronomy to cosmic distances!
Beacom & Vagins, PRL 93:171101,2004
Window of opportunity betweenreactor and atmospheric bkg
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
Sanduleak -69 202Sanduleak -69 202
Large Magellanic Cloud Distance 50 kpc (160.000 light years)
Tarantula Nebula
Supernova 1987A23 February 1987
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
Neutrino Signal of Supernova 1987AKamiokande-II (Japan)Water Cherenkov detector2140 tonsClock uncertainty 1 min
Irvine-Michigan-Brookhaven (US)Water Cherenkov detector6800 tonsClock uncertainty 50 ms
Baksan Scintillator Telescope(Soviet Union), 200 tonsRandom event cluster 0.7/dayClock uncertainty +2/-54 s
Within clock uncertainties,all signals are contemporaneous
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
Do Neutrinos Gravitate?
Early light curve of SN 1987A
• Neutrinos arrived several hours before photons as expected• Transit time for and same ( yr) within a few hours
Shapiro time delay for particlesmoving in a gravitational potential
For trip from LMC to us, depending on galactic model,
–5 months
Neutrinos and photons respond togravity the same to within
1–
Longo, PRL 60:173, 1988Krauss & Tremaine, PRL 60:176, 1988
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
Supernova 1987A Energy-Loss Argument
SN 1987A neutrino signal
Late-time signal most sensitive observable
Emission of very weakly interactingparticles would “steal” energy from theneutrino burst and shorten it.(Early neutrino burst powered by accretion, not sensitive to volume energy loss.)
Neutrino diffusion
Neutrinosphere
Volume emission of new particles
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
Flavor Oscillations in Core-Collapse Supernovae
Neutrinosphere
MSW region
Neutrino flux
Flavor eigenstates arepropagation eigenstates
Neutrino-neutrinorefraction causesa flavor instability,flavor exchangebetween differentparts of spectrum
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
Neutrino Oscillations in Matter
3700 citations
Lincoln Wolfenstein
Neutrinos in a medium suffer flavor-dependentrefraction
f
Zn n n n
W
f
Typical density of Earth: 5 g/cm3
Δ𝑉 weak≈ 2×10−13 eV=0.2 peV
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
Flavor-Off-Diagonal Refractive Index2-flavor neutrino evolution as an effective 2-level problem
i𝜕𝜕𝑡 (𝜈𝑒
𝜈𝜇)=𝐻 (𝜈𝑒
𝜈𝜇)
𝐻=𝑀 2
2𝐸+√2𝐺F(𝑁𝑒−
𝑁𝑛
20
0 −𝑁 𝑛
2)+√2𝐺F ( 𝑁𝜈𝑒
𝑁⟨ 𝜈𝑒|𝜈 𝜇⟩
𝑁 ⟨ 𝜈𝜇|𝜈𝑒 ⟩ 𝑁𝜈𝜇)
Effective mixing Hamiltonian
Mass term inflavor basis:causes vacuumoscillations
Wolfenstein’s weakpotential, causes MSW “resonant” conversiontogether with vacuumterm
Flavor-off-diagonal potential,caused by flavor oscillations.(J.Pantaleone, PLB 287:128,1992)
Flavor oscillations feed back on the Hamiltonian: Nonlinear effects!
𝝂Z
n n
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
Collective Supernova Nu Oscillations since 2006Two seminal papers in 2006 triggered a torrent of activitiesDuan, Fuller, Qian, astro-ph/0511275, Duan et al. astro-ph/0606616Balantekin, Gava & Volpe [0710.3112]. Balantekin & Pehlivan [astro-ph/0607527]. Blennow, Mirizzi & Serpico [0810.2297]. Cherry, Fuller, Carlson, Duan & Qian [1006.2175, 1108.4064]. Cherry, Wu, Fuller, Carlson, Duan & Qian [1109.5195]. Cherry, Carlson, Friedland, Fuller & Vlasenko [1203.1607]. Chakraborty, Choubey, Dasgupta & Kar [0805.3131]. Chakraborty, Fischer, Mirizzi, Saviano, Tomàs [1104.4031, 1105.1130]. Choubey, Dasgupta, Dighe & Mirizzi [1008.0308]. Dasgupta & Dighe [0712.3798]. Dasgupta, Dighe & Mirizzi [0802.1481]. Dasgupta, Dighe, Raffelt & Smirnov [0904.3542]. Dasgupta, Dighe, Mirizzi & Raffelt [0801.1660, 0805.3300]. Dasgupta, Mirizzi, Tamborra & Tomàs [1002.2943]. Dasgupta, Raffelt & Tamborra [1001.5396]. Dasgupta, O'Connor & Ott [1106.1167]. Duan [1309.7377]. Duan, Fuller, Carlson & Qian [astro-ph/0608050, 0703776, 0707.0290, 0710.1271]. Duan, Fuller & Qian [0706.4293, 0801.1363, 0808.2046, 1001.2799]. Duan, Fuller & Carlson [0803.3650]. Duan & Kneller [0904.0974]. Duan & Friedland [1006.2359]. Duan, Friedland, McLaughlin & Surman [1012.0532]. Esteban-Pretel, Mirizzi, Pastor, Tomàs, Raffelt, Serpico & Sigl [0807.0659]. Esteban-Pretel, Pastor, Tomàs, Raffelt & Sigl [0706.2498, 0712.1137]. Fogli, Lisi, Marrone & Mirizzi [0707.1998]. Fogli, Lisi, Marrone & Tamborra [0812.3031]. Friedland [1001.0996]. Gava & Jean-Louis [0907.3947]. Gava & Volpe [0807.3418]. Galais, Kneller & Volpe [1102.1471]. Galais & Volpe [1103.5302]. Gava, Kneller, Volpe & McLaughlin [0902.0317]. Hannestad, Raffelt, Sigl & Wong [astro-ph/0608695]. Wei Liao [0904.0075, 0904.2855]. Lunardini, Müller & Janka [0712.3000]. Mirizzi [1308.5255, 1308.1402]. Mirizzi, Pozzorini, Raffelt & Serpico [0907.3674]. Mirizzi & Serpico [1111.4483]. Mirizzi & Tomàs [1012.1339]. Pehlivan, Balantekin, Kajino & Yoshida [1105.1182]. Pejcha, Dasgupta & Thompson [1106.5718]. Raffelt [0810.1407, 1103.2891]. Raffelt, Sarikas & Seixas [1305.7140]. Raffelt & Seixas [1307.7625]. Raffelt & Sigl [hep-ph/0701182]. Raffelt & Smirnov [0705.1830, 0709.4641]. Raffelt & Tamborra [1006.0002]. Sawyer [hep-ph/0408265, 0503013, 0803.4319, 1011.4585]. Sarikas, Raffelt, Hüdepohl & Janka [1109.3601]. Sarikas, Tamborra, Raffelt, Hüdepohl & Janka [1204.0971]. Saviano, Chakraborty, Fischer, Mirizzi [1203.1484]. Väänänen & Volpe [1306.6372]. Volpe, Väänänen & Espinoza [1302.2374]. Vlasenko, Fuller Cirigliano [1309.2628]. Wu & Qian [1105.2068].
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
Operational Detectors for Supernova Neutrinos
Super-K (104)KamLAND (400)
MiniBooNE(200)
In brackets eventsfor a “fiducial SN”at distance 10 kpc
LVD (400)Borexino (100)
IceCube (106)
Baksan (100)
HALO (tens)
Daya Bay (100)
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
SuperNova Early Warning System (SNEWS)
http://snews.bnl.gov
Early light curve of SN 1987A
CoincidenceServer @ BNL
Super-K
Alert
Borexino
LVD
IceCube• Neutrinos arrive several hours before photons• Can alert astronomers several hours in advance
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
Local Group of Galaxies
Current best neutrino detectorssensitive out to few 100 kpc
With megatonne class (30 x SK)60 events from Andromeda
Georg Raffelt, MPI Physics, Munich Colloquium, UNSW, Sydney, 4 March 2014
The Red Supergiant Betelgeuse (Alpha Orionis)First resolvedimage of a starother than Sun
Distance(Hipparcos)130 pc (425 lyr)
If Betelgeuse goes Supernova:• 6 107 neutrino events in Super-Kamiokande• 2.4 103 neutrons /day from Si burning phase (few days warning!), need neutron tagging [Odrzywolek, Misiaszek & Kutschera, astro-ph/0311012]
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
IceCube as a Supernova Neutrino Detector
Pryor, Roos & Webster, ApJ 329:355, 1988. Halzen, Jacobsen & Zas, astro-ph/9512080.Demirörs, Ribordy & Salathe, arXiv:1106.1937.
• Each optical module (OM) picks up Cherenkov light from its neighborhood• 300 Cherenkov photons per OM from SN at 10 kpc, bkgd rate in one OM < 300 Hz• SN appears as “correlated noise” in 5000 OMs• Significant energy information from time-correlated hits
SN signal at 10 kpc10.8 Msun simulationof Basel group[arXiv:0908.1871]
Accretion
Cooling
Georg Raffelt, MPI Physics, Munich Colloquium, UNSW, Sydney, 4 March 2014
First Realistic 3D Simulation (27 Garching Group)
Hanke, Müller, Wongwathanarat, Marek & Janka [arXiv:1303.6269 (26 March 2013)]
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
Variability seen in Neutrinos (3D Model)
Tamborra, Hanke, Müller, Janka & Raffelt, arXiv:1307.7936See also Lund, Marek, Lunardini, Janka & Raffelt, arXiv:1006.1889
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
Next Generation Large-Scale Detector Concepts
Memphys
Hyper-K
DUSELLBNE
Megaton-scalewater Cherenkov
5-100 ktonliquid Argon
100 kton scale scintillator
LENAHanoHano
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
LENA: From Dream to Reality
50 ktScintillator
Juno (formerly Daya Bay II), Collaboration formed (2014)20 kt scintillator detectorHierarchy determination with reactor neutrinosAlso good for low-energy neutrino astronomy
Georg Raffelt, MPI Physics, Munich Physics Colloquium, UNSW, Sydney, 4 March 2014
SummaryUnderstanding neutrino internal properties — a mature field• Neutrino mixing parameters: Matrix well known from astro and lab evidence• New experiments for missing parameters in the making• Absolute masses yet to be determined (KATRIN, cosmology)• Majorana nature yet to be found (neutrino-less double beta expts)
Neutrinos as astrophysical messengers — a field in its infancy• Detailed measurement of solar nus (ca 60,000 events in Super-K) • First geo-neutrinos (ca 116 events in KamLAND)• SN 1987A (ca 20 events)• First high-E events in IceCube (Ernie, Bert, and 26 others)
- More statistics needed in all of these areas: bigger/better detectors planned or discussed- Waiting for next nearby supernova
Neutrinos at the center
nn Astrophysics & Cosmology
Cosm
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