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