Solar Neutrino Observables Sensitive to Matter Effects

We discuss constraints on the coefficient A_{MSW} which is introduced to simulate the effect of weaker or stronger matter potential for electron neutrinos with the current and future solar neutrino data. The currently available solar neutrino data leads to a bound A_{MSW} = 1.47^{-0.42}_{+0.54} (^{-0.82}_{+1.88}) at 1\sigma (3\sigma) CL, which is consistent with the Standard Model prediction A_{MSW} = 1. For weaker matter potential (A_{MSW} 1), the bound is milder and is dominated by the day-night asymmetry of ^8B neutrino flux recently observed by Super-Kamiokande. Among the list of observable of ongoing and future solar neutrino experiments, we find that (1) an improved precision of the day-night asymmetry of ^8B neutrinos, (2) precision measurements of the low energy quasi-monoenergetic neutrinos, and (3) the detection of the upturn of the ^8B neutrino spectrum at low energies, are the best choices to improve the bound on A_{MSW}

Solving the solar neutrino puzzle with KamLAND and solar data

We study what will be learned about the solar neutrino puzzle and solar neutrino oscillations once the data from the KamLAND reactor neutrino experiment (soon to become available) are combined with those from the current solar neutrino experiments, We find that, in agreement with previous estimates, if the solution to the solar neutrino puzzle falls on the LMA region, KamLAND should be able to 'pinpoint' the right solution with unprecedented accuracy after a few years of data taking. Furthermore, the light side ( theta/4) can be separated from the dark side (theta>pi /4) at the 95% confidence level (C.L.) for most of the LMA region allowed by the current data at the 99% C.L., while the addition of the KamLAND data need not improve our ability to limit a sterile component in 'solar' oscillations. If KamLAND does not see an oscillation signal, the solar data would point to the LOW or VAC regions, while the SMA region would still lurk at the two sigma C.L., meaning we would probably have to wait for Borexino data in order to finally piece the solar neutrino puzzle

Four-neutrino oscillations at SNO

We discuss the potential of the Sudbury Neutrino Observatory (SNO) to constrain the four-neutrino mixing schemes favored by the results of all neutrino oscillations experiments. These schemes allow simultaneous transitions of solar {\ensuremath{\nu}}_{e}'s into active {\ensuremath{\nu}}_{\ensuremath{\mu}}'s, {\ensuremath{\nu}}_{\ensuremath{\tau}}'s, and sterile {\ensuremath{\nu}}_{s} controlled by the additional parameter {\mathrm{cos}}^{2}({\ensuremath{\vartheta}}_{23}){\mathrm{cos}}^{2}({\ensuremath{\vartheta}}_{24}) and they contain as limiting cases the pure {\ensuremath{\nu}}_{e}-active and {\ensuremath{\nu}}_{e}-sterile neutrino oscillations. We first obtain the solutions allowed by the existing data in the framework of the BBP00 standard solar model and quantify the corresponding predictions for the charged current and the neutral current to charged current (NC/CC) event ratios at SNO in the different allowed regions as a function of the active-sterile admixture. Our results show that some information on the value of {\mathrm{cos}}^{2}({\ensuremath{\vartheta}}_{23}){\mathrm{cos}}^{2}({\ensuremath{\vartheta}}_{24}) can be obtained by the first SNO measurement of the CC ratio, while considerable improvement on the knowledge of this mixing will be achievable after the measurement of the NC/CC ratio

Final results of Borexino Phase-I on low-energy solar neutrino spectroscopy

Borexino has been running since May 2007 at the Laboratori Nazionali del Gran Sasso laboratory in Italy with the primary goal of detecting solar neutrinos. The detector a large unsegmented liquid scintillator calorimeter characterized by unprecedented low levels of intrinsic radioactivity is optimized for the study of the lower energy part of the spectrum. During Phase-I (2007-2010) Borexino first detected and then precisely measured the flux of the Be-7 solar neutrinos ruled out any significant day-night asymmetry of their interaction rate made the first direct observation of the pep neutrinos and set the tightest upper limit on the flux of solar neutrinos produced in the CNO cycle (carbon nitrogen oxigen) where carbon nitrogen and oxygen serve as catalysts in the fusion process. In this paper we discuss the signal signature and provide a comprehensive description of the backgrounds quantify their event rates describe the methods for their identification selection or subtraction and describe data analysis. Key features are an extensive in situ calibration program using radioactive sources the detailed modeling of the detector response the ability to define an innermost fiducial volume with extremely low background via software cuts and the excellent pulse-shape discrimination capability of the scintillator that allows particle identification. We report a measurement of the annual modulation of the Be-7 neutrino interaction rate. The period the amplitude and the phase of the observed modulation are consistent with the solar origin of these events and the absence of their annual modulation is rejected with higher than 99% C.L. The physics implications of Phase-I results in the context of the neutrino oscillation physics and solar models are presented

Solar Models With Accretion. I. Application To The Solar Abundance Problem

We generate new standard solar models using newly analyzed nuclear fusion cross sections and present results for helioseismic quantities and solar neutrino fluxes. The status of the solar abundance problem is discussed. We investigate whether nonstandard solar models with accretion from the protoplanetary disk might alleviate this problem. We examine a broad range of models, analyzing metal-enriched and metal-depleted accretion and three scenarios for the timing of accretion. Only partial solutions are found. For metal-rich accreted material (Z ac gsim 0.018) there exist combinations of accreted mass and metallicity that bring the depth of the convective zone into agreement with the helioseismic value. For the surface helium abundance, the helioseismic value is reproduced if metal-poor or metal-free accretion is assumed (Z ac lsim 0.09). In both cases a few percent of the solar mass must be accreted. Precise values depend on when accretion takes place. We do not find a simultaneous solution to both problems but speculate that changing the hydrogen-to-helium mass ratio in the accreted material may lead to more satisfactory solutions. We also show that, with current data, solar neutrinos are already a very competitive source of information about the solar core and can help constraining possible accretion histories. Even without helioseismic constraints, solar neutrinos rule out the possibility that more than 0.02 M ☉ from the protoplanetary disk were accreted after the Sun settled on the main sequence. Finally, we discuss how measurements of neutrinos from the CN cycle could shed light on the interaction between the early Sun and its protoplanetary disk

Precision Measurement of the (7)Be Solar Neutrino Interaction Rate in Borexino

A direct measurement of the 0.862 MeV 7Be solar neutrino interaction rate performed with the Borexino detector at the Laboratori Nazionali del Gran Sasso yields 46.0±1.5stat+1.6−1.5syst counts/day/(100 tons). Our result is the first direct measurement of a sub-MeV solar neutrino rate with an accuracy better than 5%. The hypothesis of no oscillation for 7Be solar neutrinos is rejected at 4.9σ C.L. Using the latest Standard Solar Model (SSM) flux predictions, the result leads directly to a precise determination of the survival probability for solar νe's in vacuum, and permits us to probe with unprecedented sensitivity the transition between the matter-enhanced and vacuum-dominated neutrino oscillation regimes characteristic of the MSW-LMA solution to the solar neutrino problem

Solar and atmospheric four-neutrino oscillations

We present an analysis of the neutrino oscillation solutions of the solar and atmospheric neutrino problems in the framework of four-neutrino mixing where a sterile neutrino is added to the three standard ones and the mass spectra presents two separated doublets. Such scenarios allow for simultaneous transitions of solar $\nu_e$, as well as atmospheric $\nu_\mu$, into active and sterile neutrinos controlled by the additional mixing angles $\vartheta_{23}$ and $\vartheta_{24}$, and they contain as limiting cases the pure solar $\nu_e$-active and $\nu_e$-sterile neutrino oscillations, and the pure atmospheric $\nu_\mu\to\nu_s$ and $\nu_\mu\to\nu_\tau$ oscillations, respectively. We evaluate the allowed active-sterile admixture in both solar and atmospheric oscillations from the combined analysis. Our results show that, although the Super-Kamiokande data disfavour both the pure $\nu_\mu\to\nu_s$ atmospheric channel and the pure $\nu_e\to\nu_s$ solar channel, the result from the combined analysis still favours close-to-pure active and sterile oscillations and disfavours oscillations into a near-maximal active-sterile admixture

Four-neutrino oscillations and the solar neutrino problem

We perform a fit of solar neutrino data in the framework of the two four-neutrino schemes that are compatible with the results of all neutrino oscillation experiments. These schemes allow simultaneous transitions of solar v(e)'s into active v(mu)'s, v(tau)'s and sterile v(s). The data imply that the SMA solution is valid for any combination of v(e) --> active and v(e) --> sterile transitions, whereas the LMA, LOW and VO solutions disappear when v(e) --> v(s) transitions are dominant

Zenith angle distributions at Super-Kamiokande and SNO and the solution of the solar neutrino problem

We have performed a detailed study of the zenith angle dependence of the regeneration factor and distributions of events at SNO and SK for different solutions of the solar neutrino problem. In particular, we discuss the oscillatory behavior and the synchronization effect in the distribution for the LMA solution, the parametric peak for the LOW solution, etc. A physical interpretation of the effects is given. We suggest a new binning of events which emphasizes the distinctive features of the zenith angle distributions for the different solutions. We also find the correlations between the integrated day-night asymmetry and the rates of events in different zenith angle bins. The study of these correlations strengthens the identification power of the analysis

Before and After: How has the SNO NC measurement changed things?

We present "Before and After" global oscillation solutions, as well as predicted "Before and After" values and ranges for ten future solar neutrino observables (for BOREXINO, KamLAND, SNO, and a generic p-p neutrino detector). We have performed global analyses using the full SNO day-night energy spectrum and, alternatively, just the SNO CC and NC rates and the day-night asymmetry.The ``Before'' case includes all solar neutrino data (and some theoretical improvements) available prior to April 20, 2002 and the ``After'' case includes, in addition, the new SNO data on the CC, NC, and day-night asymmetry. The LMA solution is the only currently allowed MSW oscillation solution at ~99% CL. The LOW solution is allowed only at more than 2.5 sigma, SMA at 3.7 sigma or 4.7 sigma (depending upon analysis strategy), and pure sterile oscillations at 4.7sigma. Small mixing angles are ``out''(pure sterile is ``way out''); MSW with large mixing angles is definitely ``in''. Vacuum oscillations are allowed at 3 sigma, but not a 2 sigma. Precise maximal mixing is excluded at 3.2 sigma for MSW solutions and at 2.8 sigma for vacuum solutions. Most of the predicted values for future observables for the BOREXINO, KamLAND, and future SNO measurements are changed only by minor amounts by the inclusion of the recent SNO data. In order to test the robustness of the allowed neutrino oscillation regions and the predictions for future observables, we have carried out calculations using a variety of strategies to analyze the SNO and other solar neutrino data.Comment: Added global analysis with full SNO day-night energy spectrum. Results essentially unchange