Solar Luminosity by Neutrinos

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Solar Luminosity by Neutrinos

• Carlos Pena Garay
• IFIC, Valencia

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Solar Neutrinos 40 years of theor. efforts

Cl
Ga
SK, SNO
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Solar Neutrinos 40 years of exp. efforts
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SM n mass, Solar KamLAND exps.
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SSM LMA is the new standard

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Luminosity constraint

If nuclear fusion reactions among light elements
are responsible for solar energy generation and
D and 3He are in local kinetic equilibrium
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(
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pp chain
99,77 p p ? d e ?e
0,23 p e - p ? d ?e
2?10-5
84,7
d p ? 3He ?
13,8
3He 4He ?7Be ?
0,02
13,78
7Be e- ? 7Li ?e
7Be p ? 8B ?
3He3He??2p
7Li p -gt??
3Hep??e?e
pp I
pp III
pp II
hep
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3He production
99,77 p p ? d e ?e
0,23 p e - p ? d ?e
d p ? 3He ?
3p ?3Hegn e(pp,pep)3Mp-M(3He)-ltEngt(pp,pep)
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3He burning
pp I
pp II
3He 4He ?7Be ?
3He3He??2p e332M(3He)-Ma-2Mp
7Be e- ? 7Li ?e
7Li p -gt??
3Hep ?agn e(7Be)MpM(3He)-Ma-ltEngt(7Be)
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Local kinetic equilibrium
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Summary
ltEngt includes corrections -thermal
motion -average ionization states -temperature
profile
Bahcall, PRC (2002)
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CNO cycle
12C p ? 13N g 13N ? 13C e n
e(13N)M(12C)Mp-M(13C)-ltEngt(13N)
13C p ? 14N g 14N p ? 15O g 15O ? 15N
e n 15N p ? 12C a
e(15O)M(13C)3Mp-Ma-M(12C)-ltEngt(15O)
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)
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Neutrino flux determination

Infer flux from measured rate Energy
distribution (lt1, 10000 SSMs) Solar density,
neutrino production distributions Neutrino
parameters (3) Neutrino cross sections ( lt3)
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Neutrino flux determination

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Low Nu experiments Total luminosity

Are nuclear reactions the unique source of power
in the Sun ?
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Conclusions

Luminosity constraint becomes a key test to
accurately probe energy generation of stars.
Test independent (1104) of solar model
details Presently, large uncertainty Needed
7Be, pp(pep), CNO experiments Few percent
accuracy is within reach
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New Physics SM n mass

Solar KamLANDAtmospheric K2K CHOOZ
3 s ranges
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The Neutrino Matrix SM n mass

ALL oscillation neutrino data BUT LSND
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Where are Solar ne ?

As nm and nt indistinguishable in solar
neutrinos experiments