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Search for CP violation in the lepton sector. n. Cristina VOLPE (Institut de Physique Nucléaire Orsay, France). CP violation searches with future facilities. CP violation effects in astrophysics and cosmology (BBN). Introduction. Conclusions. OUTLINE. - PowerPoint PPT Presentation
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Cristina VOLPE(Institut de Physique Nucléaire Orsay, France)
Search for CP violationin the lepton sector
CP violation searches with future facilities
Conclusions
CP violation effects in astrophysics and cosmology (BBN)
OUTLINEOUTLINE
Introduction
Major advances in neutrino physics
e
SOURCEL
DETECTOR
e
AN IMPRESSIVE PROGRESS IN THE LAST DECADE in ourknowledge of its properties.
Pontecorvo, 1957
L/E ratio [km/GeV]
1 10 102 103 104
oscillationdecoherencedecay
1.61.41.2
10.80.60.40.2
data
/exp
ecta
tion
?
e cos sin 1
=
-sin cos 2 e
12
flavour basis mass basis
mixing angle
The time evolution is : 2121 sincos veet tiEtiE
e
m2 = m22-m1
2
THEORETICAL DESCRIPTION
THE CP violating phase INTRODUCES A - ASYMMETRY.
3
e
1 12
23
13
3
2
1
1212
1212
1313
1313
2323
2323
100
0
0
0
010
0
0
0
001
cs
sc
ces
esc
cs
sci
ie 1
3
e
The two basis are related by a unitary matrix, called the Maki-Nakagawa-Sakata-Pontecorvo (MNSP) matrix.
ijijc cos ijijs sin
23 1312
THE 3-flavours OSCILLATION PARAMETERS In the case of three families, there are three mass eigenstates (1,2,3) and three flavour eigenstates (e,,).
23
21
22
23
21
22
3,1
2 mmmmmmmi
i Only two m2 are independent.
m212 m32
2
THE key OPEN QUESTIONS
> The mass hierarchy
> The third mixing angle 13
> The neutrino nature
> The Dirac phase
> The absolute mass scale
> The Majorana phases
Double-CHOOZ, Daya-Bay, T2K,..
KATRIN, MARE,…
Gerda, Cuore, Super-Nemo,…
from double-beta decay experiments
supernovae, -factories, double-beta,…
exciting discoveries might be close…
A wealth of experiments are under construction or at a R&D level.
13 – expected sensitivity from currently starting experiments
Discovery potential (90% CL) for sin2 213
from reactors and accelerators
P. Huber, M. Lindner, T. Schwetz, W. Winter, arXiv: 0907.1861
THE VALUE OF 13 CRUCIAL FOR FUTURE STRATEGIES.
CPV sensitivity
sensitivity limits (90% CL) from T2K, NOA and reactors
P. Huber, M. Lindner, T. Schwetz, W. Winter, arXiv: 0907.1861
LONG-TERM expensive PROJECTS might be necessary.
Long-term accelerator projects
> Super-beams - intense conventional beams from muon and pion decay > Beta-beams – intense and pure neutrino beams from boosted accelerated ions
> Neutrino factories – intense neutrino beams from stored muons
THE GOAL : to investigate very small 13 values, the Dirac CP phase and the mass hierarchy.
The beta -beam concept
ions at rest
ions are boosted
6He
6He
neutrino beams
Average neutrino energy : E = 2QFlux emittance : 1/.
No beam associated background (the -beams are produced from primary particles).
Zucchelli, PLB 2002
e6Li 6Li e
Beta-beams = 100
Low-energy = 5 -14
C. Volpe, Journ. Phys. G. 30 (2004), hep-ph/0303222.
Several beta-beam scenarios proposed
P. Zucchelli, Phys. Lett. B 2002
High-energy = 300
J. Burguet-Castell, D. Casper, JJ Gomez-Cadenas, P. Hernandez, F. Sanchez, Nucl. Phys. B695, 217 (2004), hep-ph/0312068.
and very high-energy = 1000
J. Bernabeu, J. Burguet-Castell, C. Espinoza, M. Lindroos, JHEP 0512 (2005) 014, hep-ph/0505054.
Electron-capture
See Volpe, Topical Review on “Beta-beams”, J.Phys.G34, R1 (2007) hep-ph/0605033
CP
THE standard baseline scenario
sourc
e
decayring
6He ,18Ne
PS
SPS
Proton driverSPL
ISOL productionISOL target &ion sourcebeam preparationECR pulsed
Ion accelerationLinac, 0.4 GeV
acceleration atmedium energyRCS, 1.5 GeV Acceleration to final energy
PS and SPS
e
To a far detector
IT REQUIRES THE PRODUCTION AND ACCELERATIONOF VERY INTENSE RADIOACTIVE IONS BEAMS (RIB).
8.7 GeV
93 GeVLss = 2.5 km
EURISOL
EURISOL Design Study (FP6 2005-2009) -> Conceptual Report
P. Zucchelli, Phys. Lett. B (2002)B. Autin et al. , J. Phys. G 29 (2003) 1785.
130 km
CERN
FREJUS
e
Frejus Underground Laboratory
60 m
MEGATONDETECTOR
65 m
MULTIPURPOSE DETECTORCP violation, (relic) supernova neutrinos and proton decay.
MULTIPURPOSE DETECTORCP violation, (relic) supernova neutrinos and proton decay.
THE SEARCH for CP and T violation:
CP T
(with Beta-beams) (conventional beams)
e (+) e (+)
e (-) e (-)Three technologies under study(water Cherenkov, scintillator,liquid argon) LAGUNA Design Study (2008-10)
Three technologies under study(water Cherenkov, scintillator,liquid argon) LAGUNA Design Study (2008-10)
THE standard baseline scenario
Sensitivity to 13 and CP violation
Campagne, Maltoni, Mezzetto, Schwetz, JHEP 0704:003 (2007). hep-ph/0603172
After 10 years running (5+5, or 2+8) with 440 kton detector,
5.8 (2.2) 10 18 6He (18Ne)/s, = 100
THE BETA-BEAM PROJECT IS A COMPETITIVE option.
Comparison with other facilities
ISSstudy
-beam
1
1
0.6
0.2
10-5 10-4 10-3 sin2213
Fract
ion
of
International Scoping Study Physics Working Group, arXiv: 0710.4947 .
close detector
PS
SPS
EURISOL
storage ring
BASELINE-nucleus cross sections(detector’s response,r-process, 2decay)
fundamental interactions studies (Weinberg angle, CVC test, )
PHYSICS POTENTIAL
astrophysical applications
PHYSICS STUDIED WITHIN THE EURISOL DS (FP6, 2005-2009)
CP violation effects in astrophysicsand cosmology (BBN epoch)
Core-collapse supernova neutrinos
E. Akhmedov, C.Lunardini & A.Smirnov, Nucl.Phys.B643 (2002) 339.
J Kneller and G.C. McLaughlin, arXiv:0904.3823.
A. B. Balantekin, J. Gava, C. Volpe, PLB662, 396 (2008), arXiv:0710.3112.
J. Gava, C. Volpe, Phys. Rev. D78, 083007(2008), arXiv:0807.3418.
Solar neutrinosH.Minakata and S. Watanabe, Phys. Lett. B 468, 256 (1999).
Walter Winter, Phys. Rev. D 74, 033015 (2006).
UHE neutrinos
Cosmological neutrinosJ. Gava, C. Volpe, Nucl. Phys. B (2010), arXiv:09…
NS
e
Core-collapse supernovae (SN)
99 % of the energy is emitted as neutrinos of all flavours in a short burst of about 10 s.
A possible site for thenucleosynthesis of the heavy elements, but present calculations fail to reproduce the observed abundances.
Neutrino oscillations have a significant impactIn supernovae:a fast developing field at present(shock wave effects, turbulence, the interaction)
THERE CAN BE CP-VIOLATION EFFECTS IN SUPERNOVAE.
In the Standard Model loop corrections for the v interaction with matter should be included.
Conditions for CP effects in supernovae
Beyond the Standard Model mightintroduce differences in the and interaction wiht matter (Flavor Changing Neutral Currents, …).
at the neutrinosphere
The propagation Hamiltonian does not factorize any more !
AND also
A. B. Balantekin, J. Gava, C. Volpe, PLB662, 396 (2008), arXiv:0710.3112
We have demonstrated under which conditions there can be CP violating effects in supernovae.
J. Gava, C. Volpe, Phys. Rev. D78, 083007(2008), arXiv:0807.3418.
More realistic case !
EFFECTS OF 5-10 % ON THE ELECTRON NEUTRINO FLUXES
in the SUPERNOVA.
- interaction and 1-loop
Standard MSW, tree level
Inverted hierarchy and small
Numerical results : effects on the flux ratios
J. Gava, C. Volpe, Phys. Rev. D78, 083007(2008), arXiv:0807.3418.
200 Km in the star
e (
= 1
80°)
/ e
( =
0°)
The electron fraction is n/p ratio:a key parameter for the nucleosynthesisof heavy elements (r-process).
VERY SMALL EFFECTS ON THE ELECTRON FRACTION.
Numerical results : effects on Ye
Ye (
= 1
80°)
/Ye (
= 0
°)
A. B. Balantekin, J. Gava, C. Volpe, PLB662, 396 (2008), arXiv:0710.3112
More to come ……..
CP effects in the early Universe (BBN) A vaste literature exist on the possibility of a non-zeroneutrino degeneracy parameter (neutrino asymmetry)…. If equilibration holds current bound on all flavours is: -0.044<<0.070 Serpico and Raffelt PRD 71 (2005) 127301
We have established the conditions to have CP effects on parameters : the muon and tau have to differ.
We have performed numerical calculations of the evolution ofthe degeneracy parameters at BBN epoch including the neutrinomixing, the coupling to matter and the interaction.
Our calculations follow others, e.g. Dolgov et al, Nucl. Phys. B 632 (2002) 363,
Abazajian, Beacom, Bell, PRD 66 (2002) 013008, Mangano et al, Nucl. Phys. B 729 (2005) 221,
Pastor, Pinto and Raffelt, PRL 102 (2009) 241302
Are there any CP violation effects on the neutrino degeneracyparameters? J. Gava, C. Volpe, Nucl. Phys. B 837 (2010) 50, arXiv:1002.0981.
CP effects in the early Universe (BBN) BUT our calculations include for the first time a non-zero CP violating Dirac phase in the neutrino evolution :
WE have found CP EFFECTS UP TO 1% on e, a few 10-3 on the He4 abundance.
J. Gava, C. Volpe, Nucl. Phys. B 837 (2010) 50, arXiv:1002.0981.
Conclusions
13 sets the strategy for CP violation searches.
Beta-beams and super-beams are a very competitive option if the third neutrino mixing angle is close tothe present Chooz limit.
CP violation effects in dense media -- core-collapse supernovae and Early Universe --We have determined the conditions to have CP effects (e.g. FCNC) and performed the first calculations ofits impact on the neutrino fluxes and nucleosynthesis.
Danke.
Thank you!
Merci.
Grazie.
Sensitivity to 13 and CP violation
Mezzetto 2005
Campagne, Maltoni, Mezzetto, Schwetz, JHEP 0704:003 (2007). hep-ph/0603172
After 10 years running (5+5, or 2+8) with 440 kton detector,
5.8 (2.2) 10 18 6He (18Ne)/s, = 100
Among the fundamental implications…
The solar neutrino deficit problem is clarified.
We understand the energy production in stars.
Neutrinos are massive particles, contrary to whatwas believed for decades.
The origin of neutrino mass and its smallnessneeds to be understood.
It opens a new possibility to understand the matter versus anti-matter asymmetry in the Universe.
A key step for one of the major open questions in modern cosmology.
Neutrino propagation in media
There are also shock wave effects. These engender multiple resonances and phase effects.
Neutrino-neutrino interaction is important. A more complex problem : the neutrino evolution equations are non-linear.
IMPRESSIVE PROGRESS IN THE LAST FEW YEARS !
V() GF e.
e
e e
e
W
The Mikheev-Smirnov-Wolfenstein (MSW) effect (’78, ’86) : neutrino coupling with matter induces a resonant flavour conversion.
the beautiful explanation of the « solar neutrino deficit » problem !
E=20 MeV
t=1st=1.5s
Turbulence effects arejust being considered.
A lot of work still needs to be done …
A NEW UNDERSTANDING OF PROPAGATION IN SN :
See the review from Duan and Kneller, arXiv:0904.0974
Synergy with athmospherics
Helps identify the mass hierarchy and the octant degeneracy.
Campagne, Maltoni, Mezzetto, Schwetz, JHEP 0704:003 (2007). hep-ph/0603172
First proposed in : . Hubert, Maltoni, Schwetz, Phys. Rev. D 71, 053006 (2005). hep-ph/0501037.
Neutrino propagation in SN
Temporally evolving density profiles with shock waves have to be included :These engender multiple resonances and phase effects.
Neutrino-neutrino interaction is important : Collective phenomena emerge.
IMPRESSIVE PROGRESS IN THE LAST FEW YEARS !
A NEW UNDERSTANDING OF PROPAGATION :
See the review from Duan and Kneller, arXiv:0904.0974
Turbulence effects, studies still at its beginning.
interactioneffects
shock waveseffects
The neutrino evolution equations in matter are
with
factorizes out easily and gives:
vacuum term
CP violation and core-collapse SNA. B. Balantekin, J. Gava, C. Volpe, PLB662, 396 (2008), arXiv:0710.3112
We have demonstrated under which conditions there can be CP violating effects in supernovae. Here the main steps :
matterterm
the T23 basis
The electron neutrino survival probability does not depend on .
This leads to the two following relations:
Evolution operator in the T23 basis
CP violation and core-collapse SN
J. Gava, C. Volpe, Phys. Rev. D78, 083007(2008), arXiv:0807.3418.
We have demonstrated that these relations also hold when the interaction is included.