Results 181 to 190 of about 762 (219)

Revisiting the Surface Brightness Profile of the Stellar Disk with the Statistical Mechanics of the Self-Gravitating System with the Central Body. [PDF]

Entropy (Basel)
Kang DB.
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A direct black-hole mass measurement in a little red dot at high redshift. [PDF]

Nature
Juodžbalis I, Marconcini C, D'Eugenio F, Maiolino R, Marconi A, Übler H, Scholtz J, Ji X, Jones GC, Perna M, Arribas S, Bennett JS, Bromm V, Bunker AJ, Carniani S, Charlot S, Cresci G, Dayal P, Egami E, Fabian A, Inayoshi K, Isobe Y, Ivey LR, Koudmani S, Laporte N, Liu B, Lyu J, Mazzolari G, Monty S, Parlanti E, Pérez-González PG, Robertson B, Schneider R, Sijacki D, Tacchella S, Trinca A, Valiante R, Volonteri M, Witstok J, Zhang S.   +39 more
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Electromotive field in space and astrophysical plasmas. [PDF]

Rev Mod Plasma Phys
Bourdin PA, Narita Y.
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Synchronous motion of the Easter mantle plume and the East Pacific Rise. [PDF]

Nat Commun
O'Connor JM, Regelous M, Haase KM, Hemond C, Koppers AAP, Miggins DP, Heaton DE.   +6 more
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Turbulence in Accretion Disks

Astrophysics and Space Science, 2004
zbMATH Open Web Interface contents unavailable due to conflicting licenses.
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Accretion Disks

2000
Derivations are made for the mass and the mass-turnover time scale of an accretion disk as a function of the accretion rate, the observed disk radius, the non-viscous disk radius, and two parameters. These parameters depend on the effectiveness of viscosity and tidal angular momentum loss. Application is made to DQ Herculis.
Sparks, Warren M., Kutter, G.Siegfried
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On disk accretion

Astrophysics and Space Science, 1983
A simple but sufficiently accurate method for calculating an accretion disk structure is developed. The detailed analysis of the accretion disk is fulfilled by using this method. The effect of turbulent heat transfer on the disk structure is taken into account along with the effect of radiative transfer.
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Slender Fluxtubes in Accretion Disks

Space Science Reviews, 1994
Some of the aspects of the dynamics of slender magnetic fluxtubes in a differentially rotating thin accretion disk are considered. The effect of Coriolis- and buoyancy forces on the added mass, and of radiation pressure are considered. The results are applied to a linear stability analysis for a circular fluxtube in the equatorial plane of the disk.
G. P. Schramkowski, A. Achterberg
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Periodic Orbits and Accretion Disks

Celestial Mechanics and Dynamical Astronomy, 1997
The motion of a small particle in a binary system where the radiation pressure is not negligible is considered. The photogravitational three-body problem is used as a model of formation of a disc by accretion. The author generalizes the method of \textit{Paczyńsky} [Astrophys. J.
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Counterrotating Galaxies and Accretion Disks

Annals of the New York Academy of Sciences, 1998
ABSTRACT:Theoretical interest in astrophysical disks with counterrotating components of stars and/or gas has been stimulated by recently discovered counterrotating spiral and S0 galaxies. A variety of physical processes can occur in counterrotating disks.
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