scholarly journals Measurement of neutrino flux from the primary proton–proton fusion process in the Sun with Borexino detector

2016 ◽  
Vol 47 (6) ◽  
pp. 995-1002 ◽  
Author(s):  
O. Yu. Smirnov ◽  
M. Agostini ◽  
S. Appel ◽  
G. Bellini ◽  
J. Benziger ◽  
...  
Keyword(s):  
Neutrino Flux ◽  
Fusion Process ◽  
Primary Proton ◽  
The Sun ◽  
Proton Proton ◽  
Proton Fusion ◽  
Borexino Detector

scholarly journals Low-energy (anti)neutrino physics with Borexino: Neutrinos from the primary proton-proton fusion process in the Sun

2015 ◽  
Vol 265-266 ◽  
pp. 87-92 ◽  
Author(s):  
P. Mosteiro ◽  
G. Bellini ◽  
J. Benziger ◽  
D. Bick ◽  
G. Bonfini ◽  
...  
Keyword(s):  
Neutrino Physics ◽  
Low Energy ◽  
Fusion Process ◽  
Primary Proton ◽  
The Sun ◽  
Proton Proton ◽  
Proton Fusion

Fusion in the Sun

2018 ◽  
Author(s):  
E. L. Wolf
Keyword(s):  
Kinetic Energy ◽  
Power Density ◽  
Dense Plasma ◽  
Alpha Particles ◽  
The Sun ◽  
Proton Proton ◽  
Atomic Nuclei ◽  
Proton Fusion ◽  
Schrödinger's Equation ◽  
Simplified Formula

Protons in the Sun’s core are a dense plasma allowing fusion events where two protons initially join to produce a deuteron. Eventually this leads to alpha particles, the mass-four nucleus of helium, releasing kinetic energy. Schrodinger’s equation allows particles to penetrate classically forbidden Coulomb barriers with small but important probabilities. The approximation known as Wentzel–Kramers–Brillouin (WKB) is used by Gamow to predict the rate of proton–proton fusion in the Sun, shown to be in agreement with measurements. A simplified formula is given for the power density due to fusion in the plasma constituting the Sun’s core. The properties of atomic nuclei are briefly summarized.

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 Complex-energy analysis of proton-proton fusion

2019 ◽  
Vol 100 (3) ◽  
Author(s):  
David Gaspard ◽  
Jean-Marc Sparenberg ◽  
Quentin Wenda ◽  
Daniel Baye
Keyword(s):  
Energy Analysis ◽  
Complex Energy ◽  
Proton Proton ◽  
Proton Fusion

scholarly journals Solar Neutrino Projects

1990 ◽  
Vol 121 ◽  
pp. 157-169
Author(s):  
M. Spiro ◽  
D. Vignaud
Keyword(s):  
Heavy Water ◽  
Solar Neutrino ◽  
Neutrino Oscillations ◽  
Neutrino Flux ◽  
The Sun ◽  
Solar Neutrino Problem ◽  
Wide Range ◽  
Different Sources

AbstractAn overview of the solar neutrino projects is given, with an emphasis on the complementarity of the different experiments (gallium, indium, heavy water,...) to solve the solar neutrino problem that was raised by the chlorine and the Kamiokande results. The separation of the different sources of neutrinos in the Sun would contribute significantly to the astrophysical understanding of the Sun. Some of the planned experiments could be able to pinpoint neutrino oscillations (within a wide range of parameters) almost independently of solar models. Projects which are particularly sensitive to a variation of the neutrino flux with time are also discussed.

ON THE COHERENCE CONDITION FOR RESONANT SPIN-FLAVOR PRECESSION OF MAJORANA SOLAR NEUTRINOS

1992 ◽  
Vol 07 (06) ◽  
pp. 1309-1314
Author(s):  
RAUL HORVAT
Keyword(s):  
Solar Neutrino ◽  
Neutrino Flux ◽  
Majorana Neutrino ◽  
Solar Neutrinos ◽  
Sunspot Activity ◽  
The Sun ◽  
Solar Neutrino Problem ◽  
Mass Eigenstates ◽  
Flavor Changing ◽  
Solar Neutrino Flux

One of the most attractive solutions to the solar-neutrino problem (including an anticorrelation of the solar-neutrino flux with sunspot activity) incorporates a Majorana neutrino having a flavor-changing transition moment as large as (0.1–1)×10−10 Bohr magnetons. This solution is compatible with all known laboratory, astrophysical and cosmological bounds. Here we show the consistency of the solution with the coherence condition for effective-mass eigenstates inside the sun.

On the investigation of the internal structure of the sun by means of neutrino radiation studies

1968 ◽  
Vol 46 (10) ◽  
pp. S491-S493
Author(s):  
V. A. Dergachov ◽  
G. E. Kocharov
Keyword(s):  
Energy Spectrum ◽  
Experimental Determination ◽  
Internal Structure ◽  
Solar Neutrino ◽  
Gravitational Constant ◽  
Neutrino Flux ◽  
The Sun ◽  
Neutrino Radiation ◽  
Solar Neutrino Flux

We consider the possibilities of investigating the internal structure of the sun using the energy spectrum and the intensity of its neutrino radiation. The experimental determination of the solar neutrino flux will permit us to obtain values for some parameters which are important for the theory of the internal structure of the sun (e.g. the time for evolution and the concentrations of various isotopes in the interior). It is also possible to decide whether or not the gravitational constant varies with time.

ON THE PRODUCTION OF HIGH-ENERGY NEUTRINOS IN GAMMA-RAY BURSTS

2014 ◽  
Vol 28 ◽  
pp. 1460207
Author(s):  
MATIAS M. REYNOSO
Keyword(s):  
Energy Loss ◽  
Gamma Ray ◽  
Neutrino Flux ◽  
High Energy ◽  
Gamma Ray Bursts ◽  
Proton Proton ◽  
Preliminary Results ◽  
Acceleration Zone ◽  
High Energy Neutrinos

We present preliminary results of a model with two zones in order to study the production of high energy neutrinos at the prompt phase of gamma-ray bursts (GRB). We consider an acceleration zone, where protons and electrons are injected and accelerated, being subject to synchrotron, proton-proton, and proton-gamma cooling. We also assume that they can escape from this zone at a certain rate. The produced pions and the decaying muons are also subject to energy loss and gain processes within the acceleration zone, and the escaping ones are re-injected in a second zone where acceleration no longer operates. We compute the neutrino output expected from both of these zones using typical GRB parameters, and integrate in the redshift to obtain a diffuse neutrino flux which can be different from the expected within one-zone models.

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