Comparison of Gamow-Teller strength in<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mmultiscripts><mml:mrow><mml:mi mathvariant="normal">Ar</mml:mi></mml:mrow><mml:mprescripts /><mml:mrow /><mml:mrow><mml:mn>37</mml:mn></mml:mrow><mml:mrow /><mml:mrow /></mml:mmultiscripts></mml:mrow></mml:math>and<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mmultiscripts><mml:mrow><mml:mi mathvariant="normal">K</mml:mi></mml:mrow><mml:m

Aufderheide, Maurice B.; Bloom, S.D.; Resler, D.A.; Goodman, C.D.

doi:10.1103/physrevc.49.678

Cited by 27 publications

(15 citation statements)

References 19 publications

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“…For the 8 B-neutrino absorption cross section on 37 C1, we use the recent determination by Aufderheide et al (1994) of cr( 8 B) = ( 1.11± 0.08) X 10~4 2 cm 2 (3 or uncertainty), which is in good agreement with the Bahcall and Holstein (1986) value (adopted by Bahcall and Ulrich, 1988) of cr( 8 B) = (1.06±0.10)X10~4 2 cm 2 . The slightly greater accuracy of the Aufderheide et al value is the result of improved measurements of the /3-decay strengths in the decay of 37 Ca.…”

Section: F Neutrino Interaction Cross Sectionsmentioning

confidence: 67%

Solar models with helium and heavy-element diffusion

1995

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Helium and heavy-element diffusion are both included in precise calculations of solar models. In addition, improvements in the input data for solar interior models are described for nuclear reaction rates, the solar luminosity, the solar age, heavy-element abundances, radiative opacities, helium and metal diffusion rates, and neutrino interaction cross sections. The effects on the neutrino fluxes of each change in the input physics are evaluated separately by constructing a series of solar models with one additional improvement added at each stage. The effective 1 cr uncertainties in the individual input quantities are estimated and used to evaluate the uncertainties in the calculated neutrino fluxes and the calculated event rates for solar neutrino experiments. The calculated neutrino event rates, including all of the improvements, are 9.3* J'\ SNU for the 37 C1 experiment and 137*7 SNU for the 71 Ga experiments. The calculated flux of 7 Be neutrinos is 5.1 (1.00ig;Sf)X10 9 cm -2 s _1 and the flux of 8 B neutrinos is 6.6(1.00^) X 10 6 cm -2 s _1 . The primordial' helium abundance found for this model is Y=0.278. The present-day surface abundance of the model is Y s = 0.247, in agreement with the helioseismological measurement of 7^ = 0.242±0.003 determined by Hernandez and Christensen-Dalsgaard (1994). The computed depth of the convective zone is R -0.712R 0 , in agreement with the observed value determined from /?-mode oscillation data of R = 0.713±0.003/?© found by Christensen-Dalsgaard et al. (1991). Although the present results increase the predicted event rate in the four operating solar neutrino experiments by almost l

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Section: F Neutrino Interaction Cross Sectionsmentioning

confidence: 67%

Solar models with helium and heavy-element diffusion

1995

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“…All, except the 8 B neutrinos , lead only to the ground state of 37 Ar whereas 8 B is also populating excited states including the isotopic analogue state. The cross section for the reaction (88) averaged over the 8 B spectrum has been measured recently to be [209,210] 1.14 ± 0.11 · 10 −42 cm 2…”

Section: The Chlorine-experimentsmentioning

confidence: 99%

On the physics of massive neutrinos

1998

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Massive neutrinos open up the possibility for a variety of new physical phenomena. Among them are oscillations and double beta decay. Furthermore they influence several fields from particle physics to cosmology. In this article the concept of massive neutrinos is given and the current status of experimental research is extensively reviewed. This includes astrophysical studies of solar, supernova and very high energy neutrinos. Future perspectives are also outlined.Comment: 86 pages, 50 figures (large file 8MB!!). To appear in Physics Report

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“…When averaging the pp and pep components to get p, we use the relative weights of the RSM; similarly for 13 N and 15 O to get CNO. All data from[24] but for σ Cl,B from[165]. The main characteristic of each neutrino experiment: type, detection reaction, energy threshold E th , experimental results with statistical and systematical errors.…”

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confidence: 99%

Solar neutrinos: beyond standard solar models

et al. 1997

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After a short survey of the physics of solar neutrinos, giving an overview of hydrogen burning reactions, predictions of standard solar models and results of solar neutrino experiments, we discuss the solar-model-independent indications in favour of non-standard neutrino properties. The experimental results look to be in contradiction with each other, even disregarding some experiment: unless electron neutrinos disappear in their trip from the sun to the earth, the fluxes of intermediate energy neutrinos (those from 7 Be electron capture and from the CNO cycle) result to be unphysically negative, or anyway extremely reduced with respect to standard solar model predictions. Next we review extensively non-standard solar models built as attempts to solve the solar neutrino puzzle. The dependence of the central solar temperature on chemical composition, opacity, age and on the values of the astrophysical S-factors for hydrogen-burning reactions is carefully investigated. Also, possible modifications of the branching among the various pp-chains in view of nuclear physics uncertainties are examined. Assuming standard neutrinos, all solar models examined fail in reconciling theory with experiments, even when the physical and chemical inputs are radically changed with respect to present knowledge and even if some of the experimental results are discarded.

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Comparison of Gamow-Teller strength inAr37andK

Cited by 27 publications

References 19 publications

Solar models with helium and heavy-element diffusion

Solar models with helium and heavy-element diffusion

On the physics of massive neutrinos

Solar neutrinos: beyond standard solar models

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