Nightside clouds and disequilibrium chemistry on the hot Jupiter WASP-43b. [PDF]
Bell TJ +82 more
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A hot white dwarf merger remnant revealed by an ultraviolet detection of carbon. [PDF]
Sahu S +9 more
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Infrared radiative transfer dataset: Comparisons of HITRAN2020, HITRAN2016, and MT_CKD versions 3.2 & 4.1.1 across five model atmospheres. [PDF]
Gava MLLM, Costa SMS, Sena CAP.
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Comprehensive analysis of disruption mitigation methods using gas and pellet-like injections in ITER-like Tokamaks. [PDF]
Sizyuk V, Hassanein A.
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Accreting White Dwarfs: An Unreview. [PDF]
Scaringi S, Knigge C, de Martino D.
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Opacity and radiative power losses calculations
High Energy Density Physics, 2009In this contribution we present results on opacity and radiative power losses in laser-produced plasmas. We focus our attention on the inner shell transition array 1s-2p in an aluminum plasma. At high densities, electron, Doppler and ion Stark broadening play a role in line merging.
D Benredjem, A Calisti, C Mossé
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Calculations of the radiative opacity of laser-produced plasmas
Journal of Physics B: Atomic, Molecular and Optical Physics, 1992The author presents a model for the calculation of the radiative opacity of high-power laser-produced plasmas in local thermodynamic equilibrium (LTE). The model uses detailed configuration accounting in an open shell for both the line and photoelectric absorption.
S J Rose
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The Effect of Degeneracy on the Scattering Contribution to the Radiative Opacity
Astrophysical Journal, 1995The effect of partial free electron degeneracy on the scattering contribution to the radiative opacity is of interest in calculations of the structure and evolution of stars, particularly the Sun, where the plasma at the Sun's center is partially degenerate and scattering is a major contribution to the opacity.
S J Rose
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Opacity Project data on CD for mean opacities and radiative accelerations
Monthly Notices of the Royal Astronomical Society: Letters, 2005M J Seaton
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Radiative opacities for stellar envelopes
Physica Scripta, 1995Recent advances in the field of opacity calculations for stellar envelopes are summarized. The methods used and the results obtained in the last decade by two independent groups are discussed briefly. Some of the important effects of the new data on astrophysical studies are outlined.
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