What Can Solar Neutrinos Tell Us About the Solar Radiative Zone C.P. Burgess wi

What Can Solar Neutrinos Tell Us About the Solar Radiative Zone C.P. Burgess wi www.phwiki.com

What Can Solar Neutrinos Tell Us About the Solar Radiative Zone C.P. Burgess wi

Pechman, Bruce, Fitness and Technology Analyst has reference to this Academic Journal, PHwiki organized this Journal What Can Solar Neutrinos Tell Us About the Solar Radiative Zone C.P. Burgess with N. Dzhalilov, M. Maltoni, T. Rashba, V. Semikoz, M. Tortola in addition to J. Valle hep-ph/0209094 in addition to astro-ph/0304462 Outline Neutrino Oscillations in addition to Fluctuations Neutrino Oscillations Measured Constraining Solar-Medium Fluctuations Observable Fluctuations from Magnetic Fields Helioseismology in addition to Magnetic Fields The Alfvén-wave/g-mode Resonance. Conclusions Outline Neutrino Oscillations in addition to Fluctuations Neutrino Oscillations Measured Constraining Solar-Medium Fluctuations Observable Fluctuations from Magnetic Fields Helioseismology in addition to Magnetic Fields The Alfvén-wave/g-mode Resonance. Conclusions

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Outline Neutrino Oscillations in addition to Fluctuations Neutrino Oscillations Measured Constraining Solar-Medium Fluctuations Observable Fluctuations from Magnetic Fields Helioseismology in addition to Magnetic Fields The Alfvén-wave/g-mode Resonance. Conclusions Outline Neutrino Oscillations in addition to Fluctuations Neutrino Oscillations Measured Constraining Solar-Medium Fluctuations Observable Fluctuations from Magnetic Fields Helioseismology in addition to Magnetic Fields The Alfvén-wave/g-mode Resonance. Conclusions The Sun Dedicated satellite measurements are allowing many of the Sun’s properties to be understood. Most of these are restricted to measurements of the solar surface. GONG

The Solar Interior Solar structure is inferred by modelling, based on bulk properties. Tsurf, L, R Now supplemented by two direct probes: Helioseismology Solar neutrinos GONG Solar Neutrinos Solar neutrinos escape from the solar centre in seconds, have been observed on Earth, in addition to so bring us direct immediate in as long as mation about the deep solar interior. J. Bahcall Solar Neutrino Deficit For decades the disagreement between observations of the solar neutrino flux in addition to solar model predictions has prevented using neutrinos to infer the properties of the deep solar interior. J. Bahcall

Neutrino Oscillations Solar neutrino deficit is now understood as a consequence of neutrinos oscillating while en route from the solar core. SNO After Seasoning with Salt Allowed oscillation parameters after SNO salt Terrestrial Evidence The evidence as long as neutrino oscillations is also now supported by direct terrestrial experiments, which measure disappearance of anti-ne’s from reactors en route to a distant detector. KamL in addition to s

Outline Neutrino Oscillations in addition to Fluctuations Neutrino Oscillations Measured Constraining Solar-Medium Fluctuations Observable Fluctuations from Magnetic Fields Helioseismology in addition to Magnetic Fields The Alfvén-wave/g-mode Resonance. Conclusions What Can We Learn About the Sun The success of the solar model prediction constrains thermal properties deep within the solar core. The 8B flux is sensitive to the temperature at the production point. The efficiency of oscillations also depends on the environment encountered en route. Sensitivity to Solar Fluctuations Resonant neutrino oscillations can be sensitive to fluctuations in the solar environment. Each neutrino is lucky to scatter even once on its way out. Successive neutrinos ‘see’ different solar properties, in addition to so can oscillate more or less efficiently. Jump probability seen by neutrinos behaves as a r in addition to om variable: (‘Generalized Park Formula’) CB & Michaud Loreti, Qian, Fuller & Balantekin Nunokawa, Rossi, Semikoz & Valle

Only Fluctuations at Resonance Count Oscillations are only sensitive to fluctuations which satisfy two criteria at resonance: Their correlation length must be comparable to the neutrino oscillation length. Their amplitude must be at least a few percent of the background values. No known sources of solar oscillations seem to have the required properties. CB, Bamert & Michaud Pre-Salt Sensitivities Better knowledge of neutrino oscillation parameters allows better sensitivity to solar properties. Fluctuations generically imply both a reduced transition rate in addition to a distortion of the energy spectrum. CB, Dzhalilov, Maltoni, Rashba, Semikoz, Tortola in addition to Valle Pre-Salt Sensitivities Better knowledge of neutrino oscillation parameters allows better sensitivity to solar properties. Fluctuations generically imply both a reduced transition rate in addition to a distortion of the energy spectrum. CB, ND, MM, TR, VS, MT in addition to JV Balantekin et al, Guzzo et al

Pre-Salt Sensitivities Better knowledge of neutrino oscillation parameters allows better sensitivity to solar properties. Fluctuations generically imply both a reduced transition rate in addition to a distortion of the energy spectrum. CB, Dzhalilov, Maltoni, Rashba, Semikoz, Tortola in addition to Valle after SNO salt tan2q = 0.43 Dm2 = 6.9 × 10-5 eV2 Current Noise Exclusions Amplitude/Correlation-Length Exclusion with in addition to without floating oscillation parameters tan2q = 0.43 Dm2 = 6.9 × 10-5 eV2 Sensitivity vs Experiment Type Relative Chi-Squared vs Noise Amplitude

Sensitivity of Oscillation Parameters Fits to oscillation parameters with in addition to without noise. (Black lines indicate same results without KamLAND) Sensitivity of Oscillation Parameters Fits to oscillation parameters with in addition to without noise. (Black lines indicate same results without KamLAND) with in addition to without SNO salt Outline Neutrino Oscillations in addition to Fluctuations Neutrino Oscillations Measured Constraining Solar-Medium Fluctuations Observable Fluctuations from Magnetic Fields Helioseismology in addition to Magnetic Fields The Alfvén-wave/g-mode Resonance. Conclusions

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Helioseismology The solar interior supports numerous kinds of oscillations, whose motion on the solar surface can be detected. Comparison of frequency in addition to observed wavepattern with solar model predictions constrains the properties of the model as a function of depth below the surface. GONG l = 1, m = 1 l = 36, m = 24 Helioseismic Waves Observed Wave patterns are observable by measuring Doppler shifts as a function of position on the solar surface. Thous in addition to s of normal modes have been detected in this way. GONG Two Kinds of Waves Several kinds of waves are possible. For p-modes pressure is the restoring as long as ce. Higher frequency, closer to solar surface. For g-modes buoyancy is the restoring as long as ce. Lower frequency, confined to radiative zone.

Physical Properties vs Depth Successful comparison between predicted in addition to measured normal mode frequencies gives cs, r as functions of depth. Can ‘see’ bottom of Convective Zone. Accuracy has been sufficient to correct errors in opacity codes. GONG Physical Properties vs Depth Although helioseismology constrains deviations from solar models at better than the percent level, it cannot resolve fluctuations with small spatial sizes. Must deconvolve spherical harmonics given only half of the Sun in addition to experimental noise. Christensen-Dalsgaard Turck-Chieze et al The Sun’s Magnetic Fields Studies of the solar surface in addition to corona also provide in as long as mation about the Sun’s magnetic field. Dynamic, changing fields believed responsible as long as sunspots, solar cycle, hot corona etc.

Summary Solar neutrino physics is entering a mature phase where neutrinos can be used to probe the deep solar interior. Probes both the neutrino production point in addition to the intervening neutrino oscillation history. Solar fluctuations at the position of the resonant neutrino oscillations can be observable if their amplitude is a few percent in addition to their correlation length is a few hundred km. Sensitive to scales much shorter than helioseismology. Under favourable circumstances, radiative zone magnetic fields may produce such fluctuations in the solar density due to a resonance between Alfvén waves in addition to helioseismic g-modes.

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