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\@writefile{toc}{\contentsline {section}{\numberline {2}Solar Neutrino and Recent Reactor Neutrinos Experiments}{2}}
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\@writefile{lof}{\contentsline {figure}{\numberline {1}{\ignorespaces Flux of solar $\nu _{\mu }$ or $\nu _{\tau }$ {\it  vs.} flux of $\nu _e$ deduced from the three neutrino reactions in SNO. The diagonal bands show the total $^{8}$B flux as predicted by the Standard Solar Model \nobreakspace  {}\cite  {bib:bpb} (dashed lines) and that measured with the NC reaction (solid band). The intercepts of these bands with the axes represent the $\pm 1\sigma $ errors. The bands intersect at the fit values for $\phi _{e}$ and $\phi _{\mu \tau }$, indicating that the combined flux results are consistent with flavor transformation.}}{2}}
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\@writefile{lof}{\contentsline {figure}{\numberline {2}{\ignorespaces A global analysis of the solar neutrino experiments presented in the text. Only the LMA solution remains as a viable solution to this group of experiments. This figure is courtesy of H. Murayama. }}{2}}
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\@writefile{lof}{\contentsline {figure}{\numberline {3}{\ignorespaces Excluded regions of neutrino oscillation parameters for the rate analysis and allowed regions for the combined rate and shape analysis from KamLAND at 95\% C.L.The 95\% C.L. allowed region of the Large Mixing Angle solution of solar neutrino experiments is shown. The thick dot indicates the best fit to the KamLAND data in the physical region: $\qopname  \relax o{sin}^2 2\theta = 1.0$ and $\Delta m^2 = 6.9 \times 10^{-5}$eV$^2$. All regions look identical under $\theta \leftrightarrow (\pi /2-\theta )$ except for the solar neutrino experiment determined LMA region. }}{3}}
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\@writefile{lof}{\contentsline {figure}{\numberline {4}{\ignorespaces Subdominate oscillation patterns characteristic of $\theta _{13}$ terms superimposed on the dominate $\theta _{12}$ neutrino suppression. Figure courtesy of K. Heeger.}}{4}}
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\@writefile{lof}{\contentsline {figure}{\numberline {5}{\ignorespaces Revised analysis of Super-K's 1489 day data set including fully contained and partially contained events, upward going muons, and multi-ring events. Improving the Monte Carlo simulations, event reconstruction and using updated flux calculations resulted in a slight lowering of the preferred value for $\Delta $m$^{2}$ that is consistent with early determinations but affects a number of experiments probing this region of parameter space. }}{4}}
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\@writefile{lof}{\contentsline {figure}{\numberline {6}{\ignorespaces The recent K2K analysis overlayed with Super-K atmospheric neutrino analysis both reported at this conference. }}{5}}
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\@writefile{toc}{\contentsline {subsection}{\numberline {5.1}NEMO}{7}}
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\@writefile{lof}{\contentsline {figure}{\numberline {7}{\ignorespaces This figure, courtesy of H. Murayama, indicates the different experimental signatures for neutrino oscillations: the solar and reactor neutrino region, atmospheric neutrino experiments and recent long base line accelerator experiments, and finally the LSND results. Limits for other oscillation modes are also presented. The region labeled LMA is the preferred region obtained by a global analysis of all solar radiochemical experiments, Super-K, and SNO. }}{8}}
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