Results 121 to 130 of about 2,917 (170)
Feller processes: the next generation in modeling. Brownian motion, Lévy processes and beyond. [PDF]
PLoS One, 2010 Böttcher B.
europepmc +1 more source
Corrugated Waveguide and Directional Coupler for CW 250-GHz Gyrotron DNP Experiments. [PDF]
IEEE Trans Microw Theory Tech, 2005 Woskov PP +4 more
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Monte Carlo estimation of the electric field in stellarators. [PDF]
Proc Natl Acad Sci U S A, 1986 Bauer F +3 more
europepmc +1 more source
Magnetofluid-dynamic spectrum and low shear stability. [PDF]
Proc Natl Acad Sci U S A, 1973 Grad H.
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A method of computational magnetohydrodynamics defining stable Scyllac equilibria. [PDF]
Proc Natl Acad Sci U S A, 1977 Betancourt O, Garabedian P.
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Some of the next articles are maybe not open access.
Neutrino Theory of Stellar Collapse
Physical Review, 1941At the very high temperatures and densities which must exist in the interior of contracting stars during the later stages of their evolution, one must expect a special type of nuclear processes accompanied by the emission of a large number of neutrinos.
Gamow, G., Schoenberg, M.
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Astrophysics and Space Science, 1997
The author surveys the basic theory of stellar winds with momentum input due to a force or with energy input. Five laws of stellar winds are formulated, and different wind mechanisms, line-driven model and dust-driven models are discussed.
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The author surveys the basic theory of stellar winds with momentum input due to a force or with energy input. Five laws of stellar winds are formulated, and different wind mechanisms, line-driven model and dust-driven models are discussed.
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Journal of Geophysical Research: Space Physics, 1980
The theory of stellar winds as given by the equations of classical fluid dynamics is considered. The equations of momentum and energy describing a steady, spherically symmetric, heat‐conducting, viscous stellar wind are cast in a dimensionless form which involves a thermal conduction parameter E and a viscosity parameter γ.
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The theory of stellar winds as given by the equations of classical fluid dynamics is considered. The equations of momentum and energy describing a steady, spherically symmetric, heat‐conducting, viscous stellar wind are cast in a dimensionless form which involves a thermal conduction parameter E and a viscosity parameter γ.
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Fusion Technology, 2000
A very important field of stellarator theory is based on the kinetic equations. This paper reviews the kinetic equations and the reduction of the phase-space dimension by averaging of the fastest t...
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A very important field of stellarator theory is based on the kinetic equations. This paper reviews the kinetic equations and the reduction of the phase-space dimension by averaging of the fastest t...
openaire +2 more sources