Transcript Solar Neutrinos, Neutrino Cross Sections, and NUSEL Developments A.B. Balantekin

Solar Neutrinos, Neutrino
Cross Sections, and NUSEL
Developments
A.B. Balantekin
ORNL SNS Workshop
August 28, 2003
Puzzles where neutrinos may
play a role
• What is the Dark Matter made of?
• What is Dark Energy?
• How much neutrinos contribute and why?
(what is  ?)
• What happened to all the anti-matter?
Solar Energy Generation
4 p  alpha particle + 2 positrons + 26.7
MeV
97% is emitted as photons, 3% as
neutrinos
Where does the Energy of the Sun
come from?
• 1854 von Helmholtz
gravitational
• 1920 Eddington
nuclear fusion “We do
not argue with the critic who
urges that the stars are not
hot enough for this process;
we tell him to go and find a
hotter place.”
• 1938 Bethe and
Critchfield
p+p2H +e++e
• 1946 Pontecorvo the
idea of using chlorine
as detector
• 1964 Davis chlorine
detector at
Homestake Bahcall
Standard Solar Model
“..to see into the interior
of a star and thus verify
directly the hypothesis of
nuclear energy
generation..”
Neutrinos from the Sun
Neutrinos from the Sun
The Homestake Experiment
2002
Nobel
Prize in
Physics
Sudbury Neutrino
Observatory
SNO
e + d  p + p + e-
CC
e + e  e + e
ES
x + d  x + p + n
NC
Results from SNO
Fluxes (106 cm-2s-1)
•e :
1.76(11)
•, :
3.41(66)
•TOTAL:5.09(64)
•SSM :5.05
Physics Potential of Solar
Neutrino Experiments
• Neutrino Physics - Neutrino masses and
mixings, A.B. Balantekin and H. Yuksel, JPG
29, 665 (2003) (hep-ph/0301072).
• Solar Physics - Solar temperature and
density. A.B. Balantekin and H. Yuksel, PRD
68, 013006 (2003) (hep-ph/0303169).
• Nuclear Physics - Axial two-body current.
A.B. Balantekin and H. Yuksel, (hepph/0307227).
A global analysis of the solar neutrino data
Balantekin & Yuksel
hep-ph/0301072
KamLAND
e + p  n + e+
Solar + KamLAND Global
Analysis
3 parameter
Global Fits to
Solar
Neutrino
Experiments
And KamLAND
for different
values of 13
Balantekin
and Yuksel,
hepph/0301072
Effective Field Theories
Goal: to integrate the undesired degrees of
freedom

But
~ 
Hence introduce counter-terms consistent with the
symmetries of the theory to cancel the infinities.
EFT applied to neutrino capture
• Deuteron break-up :
e + d  e- + p + p
x + d  x + p + n
3S  3S transition dominates and one only
1
0
needs the coefficient of the two-body
counter term, L1A. (Butler and Chen)

p + p  d + e + e+
”Calibrating the Sun”
Balantekin and Yuksel, 2003
Balantekin and Yuksel, 2003
Balantekin and Yuksel, 2003
National Underground Science and
Engineering Laboratory
Science Underground
•
•
•
•
•
•
Solar Neutrinos
Double -decay
Dark Matter
Nucleon Decay
Atmospheric neutrinos
Long-baseline neutrino
oscillation experiments
•
•
•
•
Supernova ’s
Nuclear astrophysics
Geoscience
Materials Development
and Technology
• Monitoring nuclear
tests.
• Microbiology
Where do we stand?
A perspective
Fundamental discoveries are recently
made
• SNO, 2002: Discovery of the non-electron neutrino
component of the solar flux ( neutrino oscillations);
measurement of the total solar neutrino flux.
• SuperK, 1998:Discovery of atmospheric neutrino flux
variations ( neutrino oscillations).
• Baksan, Kamioka, IMB, 1987: Detection of neutrinos from
Supernova 1987A (neutrino flux consistent with neutron star
binding energy, cooling time is near that expected).
• Irvine, 1987: Detection of two-neutrino double-beta decay.
• MSW, 1986: Recognition that matter enhances neutrino
oscillations.
..that broadly impact physics,
astronomy, and cosmology
• Massive neutrinos: Beyond the Standard Model of
elementary particles.
• Neutrino mixing angles are close to maximal: Impacts on
leptogenesis; explosion mechanism and nucleosynthesis in
core-collapse supernovae.
• Total solar neutrino flux is measured: The theory of main
sequence stellar evolution is verified.
• Direct neutrino mass measurements:
Neutrino component of dark matter.
Sloan DDS analysis requires a knowledge of neutrino mass
at ≈ 0.3 eV
Neutrino Astrophysics and
Cosmology
Open questions in neutrino
physics
• What is the absolute scale of neutrino masses?
Direct mass measurements.
• Why are the mixing angles so large? What is 13?
Is CP violated in the neutrino sector? Is this the
origin of the CP violation needed to explain the
baryon asymmetry of the universe?
Real-time solar neutrino experiments, very-long
baseline experiments.
• Do sterile neutrinos exist?
Open questions…
• What is the behavior of neutrinos under
charge-conjugation (Dirac vs. Majorana)?
Is neutrino its own antiparticle?
Double beta decay experiments
• What is the role of neutrinos in corecollapse supernovae?
SN neutrino detectors, MiniBooNE
• Is CPT violated?
Open questions…
• Can we do astrophysics with neutrinos?
Measure solar properties? Learn about the
interior of the supernovae?
Neutrino-nucleus crosssections
• A rich physics program, only - C is reasonably
well-known.
• Detector response 16O, Ga, Mo, Xe, Pb
• Input into supernova modeling, Fe peak
• Fundamental physics, strangeness content of the
proton
• Tests of effective field theories, e + d  p + p
(related to p + p  d + e “calibrating the Sun”)
Direct Measurements of the
Neutrino Mass
KATRIN
proposal
Double Beta Decay
• Probes the charge-conjugation properties
of neutrino:
(A,Z)  (A,Z+2) + e+ + e- + e + e
Is lepton number-violating:
mMaj =  i Uei2 mi
Muon flux vs overburden
6
10
5
Proposed NUSL Homestake
Current Laboratories
WIPP
Soudan
Muon Intensity, m-2
y
-1
Why go
deep?
10
Kamioka
10
4
Gran Sasso
10
3
10
2
Homestake
(Chlorine)
Baksan
Mont Blanc
Sudbury
NUSL - Homestake
10
1
5
6
7
8 9
10
3
2
3
4
5
6
7
8 9
10
Depth, meters water equivalent
4
Depth
requirements
are driven by
improvements
in
experimental
sensitivity
NUSL Overview (cross-section)
Yates Shaft and Complex
Science Operations
Ross Shaft and Complex
Mining and Operations
Oro Hondo
Exhaust
Ellison Exhaust
No.5 Shaft
Air Intake
No. 3 Shaft
No. 4 Shaft
No. 6
Shaft
Service Shaft
4850’
4850’
6200’
No. 7 Shaft
6800’
Proposed
Yates
Shaft Ext.
7400’
8000’
7400’ Laboratory Area
Neutrinos in Cosmology
•  = 1 (Inflation)
• Primordial
neutrinos as one
component of the
dark matter :
• 3H beta decay 
0.003 closure≤  ≤
0.20 closure
Neutrinos from corecollapse supernovae
• Mprog ≥ 8 MSun
• E ≈ 1053 ergs ≈ 1059 MeV
• 99% of the energy is carried away by
neutrinos and antineutrinos with 10 ≤
E ≤ 30 MeV
• 1059 Neutrinos!
Why do we have a baryon excess over
antibaryons in the Universe?
Baryogenesis conditions (Sakharov):
1. Baryon number non-conservation
2. CP-violation
3. Non-equilibrium conditions
Is the CP-violation necessary for this hidden
in the neutrino sector?
CP-violation in neutrino
oscillations
Very Long Baseline
Experiments
SNS and NUSEL are
complementary
playing a leading role in nuclear
astrophysics