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Interstellar dust grains are responsible for modifying the spectral energy distribution (SED) of galaxies, both absorbing starlight at UV and optical wavelengths and con-verting this energy into ther...
Energy loss through optically thin radiative cooling plays an important part in the evolution of astrophysical gas dynamics and should therefore be considered a necessary element in any numerical simu...
A one-dimensional method for reconstructing the structure of prestellar and proto-stellar clouds is presented. The method is based on radiative transfer computations and a comparison of theoretical an...
Radiative transfer equation in plane parallel geometry and Kompaneets equa-tion is solved simultaneously to obtain theoretical spectrum of 1-125 KeV photon energy range. Diffuse radiation field is cal...
We study radiative activity of magnetic white dwarf undergoing torsional vibrations about axis of its own dipole magnetic moment under the action of Lorentz restoring force. It is shown that pulsating...
Elements heavier than hydrogen or helium that are present in the atmospheres of white dwarfs with effective temperatures lower than 25,000 K, are believed to be the result of accretion. By measuring t...
We investigated the radiative emission of different types of solar features in the spectral range of the Ca II K line. We analyzed full-disk 2k x 2k observations from the PSPT Precision Solar Photom...
Sph and radiative cooling     Sph  radiative cooling       2009/6/17
Sph and radiative cooling。
SPH with radiative transfer:method and applications。
A Model for the Cross Section of a Turbulent, Radiative Jetor Wake。
Decompressive quasi shocks in radiative plasmas。

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