Connection between the Accretion Disk and Superluminal Radio Jets and the Role of the Radio Plateau State in GRS 1915+105

2006 ◽  
Vol 646 (1) ◽  
pp. 385-393 ◽  
Author(s):  
J. S. Yadav
Keyword(s):  
Accretion Disk ◽  
Radio Jets ◽  
Plateau State

scholarly journals Symmetric Parsec-Scale Radio Jets in NGC 4261

1998 ◽  
Vol 164 ◽  
pp. 63-64
Author(s):  
Dayton L. Jones ◽  
Ann E. Wehrle
Keyword(s):  
Accretion Disk ◽  
Rotation Axis ◽  
Position Angle ◽  
Narrow Gap ◽  
Apparent Rotation ◽  
Radio Jets

AbstractVLBA observations of NGC 4261 (3C 270) reveal highly symmetric radio structures at both 1.6 and 8.4 GHz. There is little evidence for free-free absorption in the inner few pc, despite the fact that HST imaging shows this galaxy to contain a nearly edge-on disk of gas and dust in its nucleus. However, at our highest resolution we find a narrow gap in emission just east of the radio core which we interpret as evidence for a small (sub-parsec) nearly edge-on accretion disk which is obscuring the base of the counterjet. The position angle of the pc-scale radio axis agrees with the position angle of the VLA-scale jets, which differs from the apparent rotation axis of the nuclear disk seen by HST.

Going with the Flow: Can the Base of Jets Subsume the Role of Compact Accretion Disk Coronae?

2005 ◽  
Vol 635 (2) ◽  
pp. 1203-1216 ◽  
Author(s):  
Sera Markoff ◽  
Michael A. Nowak ◽  
Jorn Wilms
Keyword(s):  
Accretion Disk

The Role of the Outer Boundary Condition in Accretion Disk Models: Theory and Application

2000 ◽  
Vol 537 (1) ◽  
pp. 236-244 ◽  
Author(s):  
Feng Yuan ◽  
Qiuhe Peng ◽  
Ju‐fu Lu ◽  
Jianmin Wang
Keyword(s):  
Boundary Condition ◽  
Accretion Disk ◽  
Outer Boundary

scholarly journals The Role of Opacities in Accretion Disks

1995 ◽  
Vol 10 ◽  
pp. 597-598
Author(s):  
R. Wehrse
Keyword(s):  
Angular Momentum ◽  
Neutron Star ◽  
Potential Energy ◽  
Accretion Disk ◽  
Accretion Disks ◽  
Heat Generation ◽  
White Dwarf ◽  
Young Stellar Object ◽  
Central Object

An accretion disk is formed when matter with angular momentum is flowing on a gravitating object (as e.g. a white dwarf, a neutron star, a young stellar object, or a black bole). It radiates because the transport of angular momentum (required for the matter to reach the central object) necessarily implies the conversion of potential energy into a form of energy that corresponds to higher entropy. Many aspects of the physics (as e.g. the mechanism for the heat generation) are not yet well understood but they are presently one of the centers of astronomical interest (see e.g. the books by Frank, King, and Raine, 1992, or by Wheeler, 1993).

Role of general relativity in accretion disk dynamics

Pramana ◽  
1991 ◽  
Vol 36 (5) ◽  
pp. 445-488 ◽  
Author(s):  
A R Prasanna
Keyword(s):  
General Relativity ◽  
Accretion Disk

On the heterogeneous appearance of Saturn's rings at high optical resolution

1984 ◽  
Vol 75 ◽  
pp. 691
Author(s):  
A.F. Cook ◽  
F.A. Franklin ◽  
E.M. Shoemaker ◽  
R.J. Terrile
Keyword(s):  
Uniform Distribution ◽  
Accretion Disk ◽  
Optical Resolution ◽  
Large Impact ◽  
Small Satellites ◽  
Saturn’S Rings ◽  
Break Up ◽  
Saturn's Rings

Shoemaker and Terrile have shown that several small satellites can be the parents of Saturn's rings and have suggested these as the origin of the broad systematic differences in the photometric properties of the rings. Dramatic variations on the smallest scales appear in the images obtained from Voyager. The variations of the surface of Enceladus suggest the importance of differentiation of satellites heated by tidal action maintained by resonances, as pointed out by C.M. Yoder. Subsequent break-up of such satellites, either under a large impact or under increasing tidal action of Saturn as its mass increased, would have yielded a mixture of different crustal and interior materials with different spectra of sizes and masses. We shall discuss the possible role of radial differentiation of particles in terms of their masses initiated by the combined activity of instabilities discussed long ago by Maxwell and by Cook and Franklin with those proposed recently by Ward and by Lin and Bodenheimer. In this way, we may reach an explanation of variations on the smallest scales. Comparison will be made with the expected behaviour of a primary accretion disk composed of a uniform distribution of material.

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