February 23, 2005 Neutrino Telescopes, Venice
Comparing Solar and KamLAND DataComparing Solar and KamLAND Data
Carlos Pena Garay
IAS, Princeton
~
Solar vs KamLAND DataSolar vs KamLAND Data
Solar vs KamLAND : Solar vs KamLAND : mm22 & &
MSW adiabatic vs Vacuum Osc.MSW adiabatic vs Vacuum Osc.
2
22
m
EnG eF
134cos) (
134cos
2cos
134cos
0.1
0.2
0.3
0.4
0.5
0.6
0.7
0.8
0.9
1
2 3 4 5 6 7 8
"pee_kland.txt"
Km 180LMeV )8.1 ,2.2 ,3.3(B)Be,(pp, 87 critE
Solar & KamLAND : Solar & KamLAND : mm22 & &
25221 eV10 ) 3.09.7( m
05.004.012
2 38.0tan
choozatm132 )3( 04.0sin
KamLAND in rescue of Solar KamLAND in rescue of Solar
Bahcall, Gonzalez-Garcia, PG
How well do we know solar neutrino fluxes from neutrino data + luminosity constraint?
Main effect due to KamLAND data : Improved m2
KamLAND in rescue of Solar KamLAND in rescue of Solar
Bahcall, Gonzalez-Garcia, PG
How well do we know solar neutrino fluxes from neutrino data + luminosity constraint?
Main effect due to KamLAND data: Improved m2
Low Nu experiments : Low Nu experiments : Total luminosityTotal luminosity
2.00.3-,, 1.4L/L SunvSun
02.0990.L/L ,, SunvSun
7Be,pp
Bahcall, PG, JHEP (2003)
Solar + KamLAND neutrino data:
How well do (will) we know solar neutrino fluxes ?
Solar in rescue of KamLAND Solar in rescue of KamLAND
Main effect due to Solar data : Improved 12
- Amplitude of the Energy dependent signature
- Bounds on other sources : geoneutrinos, supernovae
Fiorentini Ianni et al, in progress
KamLAND + Solar : Determining KamLAND + Solar : Determining MSWMSW
22113
20F m vscos)(nG2E2 re
Matter effects in KamLAND : negligible ( <0.5% rate )m2 determined by KamLAND in osc. phase
Matter effects in the Sun:- r0 bounded : present : 8B production < 0.23 RSUN
future : 0.05 RSUN : pep/low 8B
- If GF is replaced by A GF : A=1 within 2 A=0
rejected >6
Do we have other (practical) ways to measure MSW ?
Fogli et al
PG
KamLAND + Solar : Beyond KamLAND + Solar : Beyond MSWMSW
22113
20F m vscos)(nG2E2 re
Several speculative proposals: Better fits, new allowed regions, bounds on new physics,…
- Non-Standard Interactions- Sterile Neutrinos - CPT violation- Mass Varying Neutrinos- …
Huber
Non-standard Non-standard interactions (Majorana) interactions (Majorana)Small flavor diagonal and flavor changingfermi interactions (~0.1GF ) with quarks
LMA with modifiedmatter effects
))((v))(( 424RRR
tR qqMqHLLHqM
Berezhiani, Rossi (2002)
What’s new :
Lower region 221m
Sensitivity in KamLAND reactor
Sensitivity in low energysolar neutrino experiments
Friedland, Lunardini, PG (2004)
Davidson et al (2002)
Non-standard Non-standard interactions (Dirac) interactions (Dirac)Small flavor diagonal and flavor changingfermi interactions (~0.1GF ) with quarks
LMA with modifiedmatter effects
))(())(( 22
22RRE
mRRRR qqMqqM
What’s new :
Lower region 221m
Sensitivity in KamLAND reactor
Sensitivity in low energysolar neutrino experiments
Friedland, Lunardini, PG (2004)
Davidson et al (2002)
Sterile neutrinosSterile neutrinos
Bahcall, Gonzalez-Garcia, P-G, PRC66, 2002
221
241
2 )35.0( 09.0sin mm
How do solar data constraint oscillations to sterile ?
sae sin cos vvv
Solar & KamLAND : Solar & KamLAND : Not assuming CPT conservationNot assuming CPT conservation
KamLAND best fit points which fit Solar & KamLAND data
De Gouvea, PG
CPT boundsCPT bounds
eV10510| )K(- )(K| -10-1800 Kmmm
Lorentz invariance + Hermiticity of the Hamiltonian + locality leads to CPT theorem in relativistic local QFT
20202 eV 25.0| )K(- )(K|or mm
What about
2422 eV 101.1| )(- )(| mmDe Gouvea, PG (2004)Murayama (2003)
Summary Summary
1. Solar & KamLAND : 2 independent sources ( and ) lead to LMA
2. a) KamLAND lead to solar improved flux determinations : CNO luminosity, total luminosity2. b) Solar data lead to improved extraction of other sources
3. Goal : Determining MSW- solar tomography- Search for exotics : NSI, sterile, CPT, MVNs, …
The brightest neutrino sourceThe brightest neutrino source
SK, SNOClGa