georg raffelt, mpi physics, munich physics colloquium, unsw, sydney, 4 march 2014 neutrinos –...

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


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


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)


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.


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


First Measurement of Solar Neutrinos

600 tons ofPerchloroethylene

Homestake solar neutrino observatory (1967–2002)

Inverse beta decayof chlorine


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”


Cherenkov Effect

Water

Elastic scattering or CC reaction

NeutrinoLight

Light

Cherenkov Ring

Electron or Muon(Charged Particle)


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)


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


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

)


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)


Atmospheric Neutrino Oscillations (1998)

Atmospheric neutrino oscillations show characteristic L/E variation


Long-Baseline (LBL) ExperimentsK2K Experiment(KEK to Kamiokande)measures preciseneutrino oscillationparameters.

Since then other LBLExperiments:• Minos (US)• Opera (Europe)• T2K (Japan)• Nova (US) (construction)


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)


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 ?


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


Neutrino CarabinerNamed for a subatomic particlewith almost zero mass, …

nGreek “nu”Now also in color


“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


KATRIN Ante Portas (25 Nov 2006)


Weighing Neutrinos with the Universe


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


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


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


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)


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!


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


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


Geo NeutrinosExpected Geoneutrino Flux

Reactor Background

KamLAND Scintillator-Detector (1000 t)


Reactor On-Off KamLAND Data

KamLAND Collaboration, arXiv:1303.4667 (2013)

ScintillatorPurification

KamLAND-ZenConstruction

2011 EarthquakeReactors shut down


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!


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)


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?


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


Nucleus of the Active Galaxy NGC 4261


IceCube Neutrino Telescope at the South PoleInstrumentation of 1 km3 antarcticice with 5000 photo multiplierscompleted December 2010


Two High-Energy Events in IceCube

Ernie ~ 1.1 PeV Bert ~ 1.3 PeV


Ernie & Bert and 26 Additional Events in IceCubeSignificance of all 28 events: 4.1s, Background

Ernie & Bert


SN 1006 over Sydney

Supernova Neutrinos


Crab Nebula


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)



Collapse (implosion)ExplosionNewborn Neutron Star

50 km

Proto-Neutron Star

r rnuc = 3 1014 g cm-3

T 30 MeV



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


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


Sanduleak -69 202Sanduleak -69 202

Large Magellanic Cloud Distance 50 kpc (160.000 light years)

Tarantula Nebula

Supernova 1987A23 February 1987


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


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


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


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


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


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


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].


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)


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


Local Group of Galaxies

Current best neutrino detectorssensitive out to few 100 kpc

With megatonne class (30 x SK)60 events from Andromeda


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]


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


First Realistic 3D Simulation (27 Garching Group)

Hanke, Müller, Wongwathanarat, Marek & Janka [arXiv:1303.6269 (26 March 2013)]


Variability seen in Neutrinos (3D Model)

Tamborra, Hanke, Müller, Janka & Raffelt, arXiv:1307.7936See also Lund, Marek, Lunardini, Janka & Raffelt, arXiv:1006.1889


Next Generation Large-Scale Detector Concepts

Memphys

Hyper-K

DUSELLBNE

Megaton-scalewater Cherenkov

5-100 ktonliquid Argon

100 kton scale scintillator

LENAHanoHano


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


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

ic Rays

E

lem

enta

ry P

artic

le P

hysi

cs

georg raffelt, mpi physics, munich physics colloquium, unsw, sydney, 4 march 2014 neutrinos –...

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