Results 241 to 250 of about 435,520 (296)
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2001
The quest to learn the internal structure and dynamics of the Sun is motivated by several issues. For most people the most obvious is the desire to understand the source of energy for the Earth, which is essential for the maintenance of life. Astronomers are interested in the Sun because it is an example of a typical main-sequence star that can be ...
Douglas O. Gough, Philip H. Scherrer
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The quest to learn the internal structure and dynamics of the Sun is motivated by several issues. For most people the most obvious is the desire to understand the source of energy for the Earth, which is essential for the maintenance of life. Astronomers are interested in the Sun because it is an example of a typical main-sequence star that can be ...
Douglas O. Gough, Philip H. Scherrer
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2019
Neutrinos allow us to look into the interior of the Sun, in particular by observing the neutrino fluxes that come from the Sun’s core, which yield stringent tests whether we understand the nuclear physics and calculate the correct temperatures and densities in solar or stellar cores.
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Neutrinos allow us to look into the interior of the Sun, in particular by observing the neutrino fluxes that come from the Sun’s core, which yield stringent tests whether we understand the nuclear physics and calculate the correct temperatures and densities in solar or stellar cores.
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AIP Conference Proceedings, 2007
The equations of stellar structure and evolution need to be solved to model the interior of the Sun. Modelling the Sun is, however, slightly more complicated than modelling other stars since we have more observational constraints for the Sun than for other stars. In this article we discuss the basics of modelling the interior structure of the Sun.
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The equations of stellar structure and evolution need to be solved to model the interior of the Sun. Modelling the Sun is, however, slightly more complicated than modelling other stars since we have more observational constraints for the Sun than for other stars. In this article we discuss the basics of modelling the interior structure of the Sun.
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Advances in Space Research, 1991
Abstract Solar oscillation frequencies have become an important tool to obtain detailed information about the solar interior. The physical nature of the oscillations is well understood: the modes observed so far are standing acoustic waves (or p modes).
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Abstract Solar oscillation frequencies have become an important tool to obtain detailed information about the solar interior. The physical nature of the oscillations is well understood: the modes observed so far are standing acoustic waves (or p modes).
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1991
The interior properties of four solar models from the recent astrophysical literature are presented. The first three are standard solar models, each with somewhat different input physics. The fourth is an unconventional model designed to address the solar neutrino problem, with reduced central opacity to simulate the effects of weakly interacting ...
Guzik, J. A., Lebreton, Y.
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The interior properties of four solar models from the recent astrophysical literature are presented. The first three are standard solar models, each with somewhat different input physics. The fourth is an unconventional model designed to address the solar neutrino problem, with reduced central opacity to simulate the effects of weakly interacting ...
Guzik, J. A., Lebreton, Y.
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Solar neutrinos and nuclear reactions in the solar interior
2018We discuss the results of Homestake and Kamioka experiments, showing that - if the results of these experiments are taken at their face values - one way to save "conventional neutrinos" is to look for a nuclear solution decreasing both 7Be and 8B neutrino fluxes with respect to the predictions of the standard solar models.
Castellani V +2 more
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Present problems of the solar interior
Solar Physics, 1985The standard model of solar evolution is reviewed and a number of problems highlighted. A fundamental question is whether there is any mixing of matter in the central regions, since such mixing could radically alter the model of the present Sun and modify our understanding of the evolution of other stars.
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Solar interior structure and luminosity variations
Solar Physics, 1981The assumptions of standard solar evolution theory are mentioned briefly, and the principle conclusions drawn from them are described. The result is a rationalization of the present luminosity and radius of the Sun. Because there is some uncertainty about the interior composition of the Sun, a range of models is apparently acceptable.
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Helioseismology and the solar interior dynamics
Journal of Astrophysics and Astronomy, 2000AbstractThe inversion of helioseismic modes leads to the sound velocity inside the Sun with a precision of about 0.1 per cent. Comparisons of solar models with the “seismic sun” represent powerful tools to test the physics: depth of the convection zone, equation of state, opacities, element diffusion processes and mixing inside the radiative zone.
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Rapid Rotation of the Solar Interior
Science, 1967A model proposed for the sun apparently can account for the maintenance of photospheric rotation against deceleration by the solar wind. The rotational period is about half a day near the top of the radiative mass, and 1.6 times shorter at the center.
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