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  2. Codes for electromagnetic scattering by spheres - Wikipedia

    en.wikipedia.org/wiki/Codes_for_electromagnetic...

    py_gmm G. Pellegrini [20] Python + Fortran A Python + Fortran 90 implementation of the Generalized Multiparticle Mie method, especially suited for plasmonics and near field computation. 2017 CELES A. Egel, L. Pattelli and G. Mazzamuto [21] MATLAB + CUDA Running on NVIDIA GPUs, with high performance for many spheres. 2020 QPMS M. Nečada [22] C ...

  3. Modified Newtonian dynamics - Wikipedia

    en.wikipedia.org/wiki/Modified_Newtonian_dynamics

    Here F N is the Newtonian force, m is the object's (gravitational) mass, a is its acceleration, μ (x) is an as-yet unspecified function (called the interpolating function), and a 0 is a new fundamental constant which marks the transition between the Newtonian and deep-MOND regimes. Agreement with Newtonian mechanics requires

  4. List of open-source software for mathematics - Wikipedia

    en.wikipedia.org/wiki/List_of_open-source...

    An unpublished computational program written in Pascal called Abra inspired this open-source software. Abra was originally designed for physicists to compute problems present in quantum mechanics. Kespers Peeters then decided to write a similar program in C computing language rather than Pascal, which he renamed Cadabra. However, Cadabra has ...

  5. Standard gravitational parameter - Wikipedia

    en.wikipedia.org/wiki/Standard_gravitational...

    the vector r is the position of one body relative to the other; r, v, and in the case of an elliptic orbit, the semi-major axis a, are defined accordingly (hence r is the distance) μ = Gm 1 + Gm 2 = μ 1 + μ 2, where m 1 and m 2 are the masses of the two bodies. Then: for circular orbits, rv 2 = r 3 ω 2 = 4π 2 r 3 /T 2 = μ

  6. Two-body problem in general relativity - Wikipedia

    en.wikipedia.org/wiki/Two-body_problem_in...

    In the spherical-coordinates example above, there are no cross-terms; the only nonzero metric tensor components are g rr = 1, g θθ = r 2 and g φφ = r 2 sin 2 θ. In his special theory of relativity, Albert Einstein showed that the distance ds between two spatial points is not constant, but depends on the motion of the observer.

  7. Gyromagnetic ratio - Wikipedia

    en.wikipedia.org/wiki/Gyromagnetic_ratio

    Here, ⁠ 1 / 2 ⁠ σ μν and F μν stand for the Lorentz group generators in the Dirac space, and the electromagnetic tensor respectively, while A μ is the electromagnetic four-potential. An example for such a particle [9] is the spin ⁠ 1 / 2 ⁠ companion to spin ⁠ 3 / 2 ⁠ in the D (½,1) ⊕ D (1,½) representation space of the ...

  8. Generalized estimating equation - Wikipedia

    en.wikipedia.org/wiki/Generalized_estimating...

    Download QR code; Print/export ... (GMM). [9] This relationship is ... Comparisons among software packages for the analysis of binary correlated data ...

  9. Gravitational energy - Wikipedia

    en.wikipedia.org/wiki/Gravitational_energy

    For two pairwise interacting point particles, the gravitational potential energy is the work that an outside agent must do in order to quasi-statically bring the masses together (which is therefore, exactly opposite the work done by the gravitational field on the masses): = = where is the displacement vector of the mass, is gravitational force acting on it and denotes scalar product.