Results 271 to 280 of about 35,614 (300)

Black hole jets on the scale of the Cosmic Web

Oei MS, Hardcastle MJ, Timmerman R, Gast AR, Botteon A, Rodriguez AC, Stern D, Rivera GC, Weeren RJv, Röttgering HJ, Intema HT, de Gasperin F, Djorgovski S.   +12 more
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Accretion disks in stellar X-ray sources

Space Science Reviews, 1982
openaire   +3 more sources

Accretion disk dynamics, photoionized plasmas, and stellar opacities

Physics of Plasmas, 2009
We present a brief review on the atomic kinetics, modeling and interpretation of astrophysical observations, and laboratory astrophysics experiments. The emphasis is on benchmarking of opacity calculations relevant for solar structure models, photoionized plasmas research, the magnetohydrodynamic numerical simulation of accretion disk dynamics, and a ...
R. C. Mancini, J. E. Bailey, J. F. Hawley, T. Kallman, M. Witthoeft, S. J. Rose, H. Takabe   +6 more
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Accretion Disks in Compact Stellar Systems

1993
Disk instabilities in stellar accretion disks, J. Cannizzo and F. Meyer angular momentum transport in low mass accretion disks, E.T. Vishniac emission lines from accretion disks, E.L. Robinson eclipse mapping of accretion disks, K. Horne disk atmospheres, G. Shaviv discs and magnetospheres, A. King winds and boundary layers in accretion disks, J.
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Heating mechanisms in accretion disks around young stellar objects

Proceedings of the International Astronomical Union, 2018
AbstractAccretion disks are observed around young stellar objects such as T Tauri stars. In order to complete the star formation, particles in the disk need to loose angular momentum in order to be accreted into the central object. The magneto-rotational instability (MRI) is probably the mechanism responsible for a magneto-hydrodynamic (MHD) turbulence
Natália F.S. Andrade, Rafael Rechiche de Campos, Vera Jatenco-Pereira   +2 more
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Alfvén Waves in Dusty Proto-Stellar Accretion Disks

2012
The magneto-rotational instability (MRI) is believed to be the mechanism responsible for a magneto-hydrodynamic (MHD) turbulence that could lead to the accretion observed in proto-stellar accretion disks. A minimum amount of ionization in this medium is necessary for the MRI to take place.
Aline de Almeida Vidotto, Vera Jatenco-Pereira   +1 more
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The development of large-scale instability in Keplerian stellar accretion disks

Astronomy Reports, 2012
Our previous studies of large-scale vortical flows arising in shear flows of stellar accretion disks with Keplerian azimuthal velocity distributions as a result of the development of small perturbations are continued. The development of large-scale instability in an accretion disk is investigated via mathematical modeling.
A. Yu. Lugovskii, V. M. Chechetkin
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Stellar mass black holes accretion disks in the low-hard state

AIP Conference Proceedings, 2010
The geometry of the accretion flow in the low‐hard state (LHS) remains uncertain. A cool accretion disk is usually invoked in all interpretations, however the extent of its inner radius differs significantly between them. Either the geometrically thin disk in the LHS extends close to the innermost stable circular orbit or is truncated far from the ...
R. C. Reis, A. C. Fabian, J. M. Miller, A. Comastri, L. Angelini, M. Cappi   +5 more
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Ejection of substellar objects from accretion disks through stellar encounters

2015
Stars often form in dense cluster environments, in which encounters between young stars are likely. If such an encounter happens while one of the stars has an extended disk that is gravitationally unstable, fragments formed within the disk can be ejected via multi-body gravitational interaction.
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