Solar Models: Current Epoch and Time Dependences, Neutrinos, and Helioseismological Properties

Bahcall, John N.; Pinsonneault, Marc H.; Basu, Sarbani

doi:10.1086/321493

Cited by 944 publications

(1,347 citation statements)

References 96 publications

Supporting

Mentioning

1,241

Contrasting

Unclassified

Order By: Relevance

“…In the capture rate calculations we also need the density profile of the Earth and the Sun and the chemical composition as a function of radius. For the Sun we use the solar model BP2000 [81], complemented with the estimates of the mass fractions of the heavier elements from [82]. For the Earth, we use the density profile of [83] with the compositions given in [84] (see [54] for a table of these).…”

Section: Neutrinos From the Sun And Earthmentioning

confidence: 99%

DarkSUSY: computing supersymmetric dark matter properties numerically

Gondolo

Edsjö

Ullio

et al. 2004

J. Cosmol. Astropart. Phys.

910

1,059

View full text Add to dashboard Cite

The question of the nature of the dark matter in the Universe remains one of the most outstanding unsolved problems in basic science. One of the best motivated particle physics candidates is the lightest supersymmetric particle, assumed to be the lightest neutralino -a linear combination of the supersymmetric partners of the photon, the Z boson and neutral scalar Higgs particles. Here we describe DarkSUSY, a publicly-available advanced numerical package for neutralino dark matter calculations. In DarkSUSY one can compute the neutralino density in the Universe today using precision methods which include resonances, pair production thresholds and coannihilations. Masses and mixings of supersymmetric particles can be computed within DarkSUSY or with the help of external programs such as FeynHiggs, ISASUGRA and SUSPECT. Accelerator bounds can be checked to identify viable dark matter candidates. DarkSUSY also computes a large variety of astrophysical signals from neutralino dark matter, such as direct detection in low-background counting experiments and indirect detection through antiprotons, antideuterons, gamma-rays and positrons from the Galactic halo or high-energy neutrinos from the center of the Earth or of the Sun. Here we describe the physics behind the package. A detailed manual will be provided with the computer package.

show abstract

Section: Neutrinos From the Sun And Earthmentioning

confidence: 99%

DarkSUSY: computing supersymmetric dark matter properties numerically

Gondolo

Edsjö

Ullio

et al. 2004

J. Cosmol. Astropart. Phys.

910

1,059

View full text Add to dashboard Cite

show abstract

“…The strategies corresponding to panels (b) and (c) include the theoretical uncertainty in the 8 B neutrino flux, but differ in how they treat the total rate measured in the Super-Kamiokande experiment. The input data used in constructing figure 1 include the neutrino fluxes and uncertainties predicted by the BP00 solar model [8] and the total measured CC and NC event rates from the SNO experiment [1], the SNO day-night asymmetry [2], the Chlorine [10] and Gallium (averaged) [6,11,12,13] event rates, as well as the zenith angle-recoil energy spectrum data presented by Super-Kamiokande [14]. The rates from the GALLEX/GNO and SAGE experiments have been averaged to provide a unique data point (72.4 ± 4.7 SNU).…”

Section: Global Oscillation Solutionsmentioning

confidence: 99%

“…We also include the recently reported SAGE [6] data for 11 years of observation and the zenith angle-recoil energy spectrum data presented by the Super-Kamiokande collaboration after 1496 days of observations [7] . Where required, we use the predicted fluxes and their errors from the BP00 standard solar model [8].…”

Section: Introductionmentioning

confidence: 99%

“…To assess the robustness of the global oscillation solutions, compare this figure with figure 1a or 3b. The input data used in constructing figure 4 include the SNO day-night spectrum [2], the Chlorine [10] and Gallium (averaged) [6,11,12,13] event rates, as well as the zenith angle-recoil energy spectrum data presented by Super-Kamiokande [14] and the neutrino fluxes and uncertainties predicted by the standard solar model [8] except for the 8 B flux (which is treated as a free parameter). The rates from the GALLEX/GNO and SAGE experiments have been averaged to provide a unique data point (72.4 ± 4.7 SNU).…”

mentioning

confidence: 99%

See 1 more Smart Citation

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

Bahcall¹,

González-García²,

Peña-Garay³

2002

J. High Energy Phys.

126

121

View full text Add to dashboard Cite

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). 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. We have performed global analyses using the full SNO day-night energy spectrum and, alternatively, using just the SNO NC and CC rates and the 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 2.5σ, SMA is now excluded at 3.7σ or 4.7σ depending upon analysis strategy, and pure sterile oscillations are excluded at more than 4.7σ. Small mixing angles are "out" (pure sterile is "way out"); MSW with large mixing angles is definitely "in." Vacuum oscillations are allowed at 3σ, but not at 2σ. Precise maximal mixing is excluded at 3.2σ for MSW solutions and at more than 2.8σ 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 that are inferred from the measurements and the predicted values for future solar neutrino observables, we have carried out calculations using a variety of strategies for analyzing the SNO and other experimental data.

show abstract

“…In this section, we present the predicted solar neutrino fluxes (table 1) and their uncertainties (table 2) that were computed with the BP00 solar model [12], with and without taking account of a recent precise measurement of the production cross section that leads to the emission of 8 B neutrinos. Both the solar neutrino fluxes and their uncertainties are used in calculations of the allowed regions for neutrino oscillation parameters.…”

Section: Bp00 + New 8 Bmentioning

confidence: 99%

Robust signatures of solar neutrino oscillation solutions

Bahcall

González-García

Peña-Garay

2002

J. High Energy Phys.

View full text Add to dashboard Cite

With the goal of identifying signatures that select specific neutrino oscillation parameters, we test the robustness of global oscillation solutions that fit all the available solar and reactor experimental data. We use three global analysis strategies previously applied by different authors and also determine the sensitivity of the oscillation solutions to the critical nuclear fusion cross section, S 17 (0), for the production of 8 B. Our standard results make use of the precise new measurement of S 17 (0) by Junghans et al. The globally favored solutions are, in order of goodness of fit: LMA(the only solution at 2σ), LOW, and VAC. The NC to CC ratio for SNO is predicted by the standard global analysis to be 3.45 +0.70 −0.54 (1σ) which is separated from the no-oscillation value of 1.0 by much more than the expected experimental error. The predicted range of the day-night difference in CC rates is 8.3 +5.0 −5.6 (1σ)%. A measurement by SNO of either a NC to CC ratio > 3.3 or a day-night difference > 10%, would favor a small region of the currently allowed LMA neutrino parameter space. The global oscillation solution predicts a 7 Be neutrino-electron scattering rate in BOREXINO and KamLAND in the range 0.65 +0.04 −0.03 (1σ) of the BP00 standard solar model rate, a prediction which can be used to test both the solar model and the neutrino oscillation theory. Only the LOW solution predicts a large day-night effect(≤ 42%, 3σ) in BOREXINO and KamLAND. For the reactor KamLAND experiment, the LMA solution predicts a charged current rate relative to the standard model of 0.44 +0.22 −0.07 (1σ), E threshold = 1.22 MeV. We have also evaluated the effects of including preliminary Super-Kamiokande data for 1496 days of observations.

show abstract

Solar Models: Current Epoch and Time Dependences, Neutrinos, and Helioseismological Properties

Cited by 944 publications

References 96 publications

DarkSUSY: computing supersymmetric dark matter properties numerically

DarkSUSY: computing supersymmetric dark matter properties numerically

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

Robust signatures of solar neutrino oscillation solutions

Contact Info

Product

Resources

About