Standard solar model calculation of the neutrino fluxes

2007 ◽  
Vol 168 ◽  
pp. 115-117 ◽  
Author(s):  
A.M. Serenelli
Keyword(s):  
Model Calculation ◽  
Solar Model ◽  
Standard Solar Model ◽  
Neutrino Fluxes

SOLAR MODELS: AN HISTORICAL OVERVIEW

2003 ◽  
Vol 18 (22) ◽  
pp. 3761-3776 ◽  
Author(s):  
JOHN N. BAHCALL
Keyword(s):  
Solar Neutrino ◽  
Neutrino Flux ◽  
New Physics ◽  
Solar Model ◽  
Historical Overview ◽  
Standard Solar Model ◽  
Solar Luminosity ◽  
Consensus View ◽  
Neutrino Fluxes ◽  
Neutrino Experiments

I will summarize in four slides the 40 years of development of the standard solar model that is used to predict solar neutrino fluxes and then describe the current uncertainties in the predictions. I will dispel the misconception that the p-p neutrino flux is determined by the solar luminosity and present a related formula that gives, in terms of the p-p and 7 Be neutrino fluxes, the ratio of the rates of the two primary ways of terminating the p-p fusion chain. I will also attempt to explain why it took so long, about three and a half decades, to reach a consensus view that new physics is being learned from solar neutrino experiments. Finally, I close with a personal confession and some personal remarks.

Perspectives on the Interior of the Sun

2000 ◽  
Vol 179 ◽  
pp. 331-337
Author(s):  
S. M. Chitre
Keyword(s):  
Particle Physics ◽  
Solar Model ◽  
The Sun ◽  
Standard Solar Model ◽  
Physical Conditions ◽  
Viable Solution ◽  
Internal Constitution ◽  
Structure Equations ◽  
Neutrino Fluxes ◽  
Oscillation Frequencies

AbstractThe interior of the Sun is not directly accessible to observations. Nonetheless, it is possible to infer the physical conditions inside the Sun with the help of structure equations governing its equilibrium and with the powerful observational tools provided by the neutrino fluxes and oscillation frequencies. The helioseismic data show that the internal constitution of the Sun can be adequately represented by a standard solar model. It turns out that a cooler solar core is not a viable solution for the measured deficit of neutrino fluxes, and the resolution of the solar neutrino puzzle should be sought in the realm of particle physics.

Making a seismic solar model and an estimate of the neutrino fluxes

1997 ◽  
Vol 181 ◽  
pp. 167-174
Author(s):  
H. Shibahashi ◽  
M. Takata
Keyword(s):  
Sound Speed ◽  
Stellar Structure ◽  
Solar Model ◽  
The Sun ◽  
Speed Profile ◽  
Standard Solar Model ◽  
Sound Speed Profile ◽  
History Of ◽  
Basic Equations ◽  
Neutrino Fluxes

We present a method of making a solar model based on the helioseismic data. We first invert the observed eigenfrequencies to determine the sound speed profile, and then solve the basic equations governing the stellar structure with the imposition of the determined sound-speed profile. This approach is different from that of the standard solar model in the sense that the ‘seismic’ solar model is a snapshot model of the sun constructed without any assumption about the history of the sun. We invert the data obtained at the South Pole by the Bartol/NSO/NASA group along with BISON, HLH, and LOWL data. Finally we estimate the neutrino fluxes of the seismic model.

scholarly journals The Standard Solar Model

1990 ◽  
Vol 121 ◽  
pp. 21-41
Author(s):  
J.N. Bahcall ◽  
M. Cribier
Keyword(s):  
Equation Of State ◽  
Solar Neutrinos ◽  
Solar Model ◽  
Chemical Abundances ◽  
Standard Solar Model ◽  
Cambridge University ◽  
Input Parameters ◽  
Neutrino Astrophysics ◽  
Neutrino Fluxes ◽  
Radiative Opacity

AbstractThe main features of standard solar models, the logic of the calculations, and some of the important results concerning solar neutrinos experiments are given. The input parameters that cause the greatest uncertainties in the calculated neutrino fluxes are the nuclear rection rates, the chemical abundances, the radiative opacity, and the equation of state. This article is based, with permission of the publisher, on Chapters 1 and 4 of Neutrino Astrophysics by J. N. Bahcall, Cambridge University Press (1989).

scholarly journals Theoretical Review of Secular Instabilities in the Sun

1980 ◽  
Vol 5 ◽  
pp. 441-444
Author(s):  
M. Gabriel
Keyword(s):  
Inner Core ◽  
Neutrino Flux ◽  
Radial Oscillation ◽  
Solar Model ◽  
The Sun ◽  
Standard Solar Model ◽  
The Past ◽  
Low Order

In this review we discuss the problems raised by the discovery that the sun was, in the past, unstable towards non-radial oscillations.In 1972, Fowler (1972), in an attempt to explain the low-neutrino flux measured in Davis’ experiment (now 1.6 snu, while the standard solar model predicts 4.4 snu) suggested that the sun could have undergone, some 10 years ago, a change in structure because of sudden mixing of the inner core. During the same year Dilke and Gough (1972) suggested the sun is unstable to low-order gravity modes (g+ modes) of non-radial oscillation and that the mixing is triggered when the amplitude of the oscillation becomes large enough.

scholarly journals Coupling 1D stellar evolution with 3D-hydrodynamical simulations on the fly – I. A new standard solar model

2018 ◽  
Vol 481 (1) ◽  
pp. L35-L39 ◽  
Author(s):  
Andreas Christ Sølvsten Jørgensen ◽  
Jakob Rørsted Mosumgaard ◽  
Achim Weiss ◽  
Víctor Silva Aguirre ◽  
Jørgen Christensen-Dalsgaard
Keyword(s):  
Stellar Evolution ◽  
Solar Model ◽  
Standard Solar Model ◽  
Hydrodynamical Simulations

The Kamiokande Solar Neutrino Experiment

1990 ◽  
Vol 121 ◽  
pp. 179-186 ◽  
Author(s):  
K. S. Hirata ◽  
T. Kajita ◽  
T. Kifune ◽  
K. Kihara ◽  
M. Nakahata ◽  
...  
Keyword(s):  
Solar Neutrino ◽  
Background Level ◽  
Solar Neutrinos ◽  
Solar Model ◽  
Neutrino Experiment ◽  
Standard Solar Model ◽  
Measured Flux ◽  
Analysis Methods ◽  
Time Period ◽  
Solar Neutrino Experiment

AbstractThe observation of 8B solar Neutrinos in the Kamiokande-II detector is presented. Based on 450 days of data in the time period of January 1987 through May 1988, the measured flux obtained with Ee ≥ 9.3 MeV was 0.46 ± 0.13 (stat) ± 0.08 (sys) of the value predicted by the standard solar model. The detector and analysis methods were improved since June 1988 and the background level has been decreased by a factor of about three since then.

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