Results 181 to 190 of about 1,157 (218)
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2004
The use of the term atmosphere for the outer layers of a star is not obvious. The atmosphere of a terrestrial planet is easily defined as the gaseous envelope extending from the crust (or ocean) out into free space. For stars, the lower boundary is less easily defined.
Bengt Gustafsson, Susanne Höfner
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The use of the term atmosphere for the outer layers of a star is not obvious. The atmosphere of a terrestrial planet is easily defined as the gaseous envelope extending from the crust (or ocean) out into free space. For stars, the lower boundary is less easily defined.
Bengt Gustafsson, Susanne Höfner
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The Spectra and Atmospheres of Stars
2002Astellar atmosphere is defined as that layer of a star from which electromagnetic radiation can escape; it is thus the “visible” outer part of the star. Its structure is closely connected with the spectra it emits.
Albrecht Unsöld, Bodo Baschek
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On the Atmosphere of a Rotating Star
Publications of the Astronomical Society of Japan, 1966Abstract The condition of radiative equilibrium in the atmosphere of a rotating star is examined. An expression is obtained for the radiation flux in the atmosphere of a rotating star under the assumption of hydrostatic equilibrium for the case in which the centrifugal force has a potential.
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A Neutron Star Atmosphere in the Laboratory with Petawatt Lasers
Astrophysics and Space Science, 2005zbMATH Open Web Interface contents unavailable due to conflicting licenses.
Moon, S. J. +7 more
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Hydrodynamical Model Atmospheres of Metal‐Poor Stars
AIP Conference Proceedings, 2008Standard one‐dimensional (1D) model atmospheres rely on the assumption of radiative equilibrium in the non‐convective part of the stellar photosphere. However, gas‐dynamical effects can lead to dramatic deviations from radiative equilibrium conditions, especially in metal‐poor stellar atmospheres.
Ludwig, Hans-Günter +4 more
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Stars with expanding atmospheres
Vistas in Astronomy, 1956Abstract Most stars are stabilized spheres whose outer strata are nearly quiescent. Those exceptional objects in whose atmospheres outward motions have been observed may be placed in three groups: pulsating stars, stars with occasional outbursts, and stars with a continual outflow of atoms.
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2006
Properties of the thermal radiation emitted by neutron stars (NSs) are determined by thin plasma layers (atmospheres) at their surfaces. The NS atmospheres are very different from those of usual stars due to the immense gravity and huge magnetic fields. Current models of hydrogen NS atmospheres show that the spectra deviate substantially from blackbody
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Properties of the thermal radiation emitted by neutron stars (NSs) are determined by thin plasma layers (atmospheres) at their surfaces. The NS atmospheres are very different from those of usual stars due to the immense gravity and huge magnetic fields. Current models of hydrogen NS atmospheres show that the spectra deviate substantially from blackbody
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Magnetized atoms in star atmospheres
AIP Conference Proceedings, 2000Magnetic white dwarfs possess strong magnetic fields which can vary in the wide range 100 T–105T. Atoms and molecules of their atmospheres which are exposed to such extreme fields severely change their electronic structure and properties. In order to understand the observed spectra of magnetic cosmic objects it is indispensable to perform detailed ...
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On the Stability of the Atmospheres of Helium Stars
Publications of the Astronomical Society of Japan, 1954Abstract On the basis of the hypothesis that the highly luminous peculiar stars are gravitationally contracting after they have exhausted their hydrogen, we consider here the stability of the upper atmosphere, which is assumed to consist of pure helium, against the radiation pressure.
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Atmospheres of Rocky Exoplanets
Annual Review of Astronomy and Astrophysics, 2022Laura Kreidberg, Robin Wordsworth
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