Erratum: “Modeling Eclipses in the Classical Nova V Persei: The Role of the Accretion Disk Rim” (ApJ, 644, 1104 [2006])

2006 ◽  
Vol 653 (2) ◽  
pp. 1586-1586
Author(s):  
A. W. Shafter ◽  
K. A. Misselt
Keyword(s):  
Accretion Disk ◽  
Classical Nova

scholarly journals Modeling Eclipses in the Classical Nova V Persei: The Role of the Accretion Disk Rim

2006 ◽  
Vol 644 (2) ◽  
pp. 1104-1117 ◽  
Author(s):  
A. W. Shafter ◽  
K. A. Misselt
Keyword(s):  
Accretion Disk ◽  
Classical Nova

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

scholarly journals Complex long-term activity of the post-nova X Serpentis

2018 ◽  
Vol 614 ◽  
pp. A141 ◽  
Author(s):  
V. Šimon
Keyword(s):  
Accretion Disk ◽  
Mass Transfer Rate ◽  
Complex Activity ◽  
Viscous Instability ◽  
Classical Nova ◽  
The Individual ◽  
Instability Regime ◽  
Nova Outbursts ◽  
Nova Outburst

Aims. X Ser is a cataclysmic variable (CV) which erupted as a classical nova in 1903. In this work we use over 100 years of photometry to characterize the long-term light curve of X Ser, with the aim of interpreting the post-nova activity in X Ser in the context of behaviors in other old novae. Methods. This analysis of its long-term optical activity uses the data from the Digital Access to a Sky Century @ Harvard (DASCH), AAVSO, and Catalina Real-time Transient Survey databases, supplemented by the data of other authors. Results. We show that X Ser displays a strong complex activity with the characteristics of various CV types after the return to quiescence from its classical nova outburst. Both nova-like and dwarf nova (DN) features are present. The decaying branches of the individual post-nova outbursts display large mutual similarities and obey the Bailey law for outbursts of DNe. These outbursts of X Ser constitute a uniform group (inside-out outbursts), and their decaying branches can be explained by propagation of cooling front through the accretion disk. In the interpretation, X Ser rapidly transitioned to a thermal-viscous instability regime of the disk, initially only intermittently. The occurrence of the DN outbursts shortly after the end of the nova outburst suggests that the mass transfer rate into the disk was usually not sufficiently high to prevent a thermal-viscous instability of this post-nova. The very long orbital period, and hence large accretion disk of X Ser can contribute to this.

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.

scholarly journals THE ROLE OF THE ACCRETION DISK, DUST, AND JETS IN THE IR EMISSION OF LOW-LUMINOSITY ACTIVE GALACTIC NUCLEI

2013 ◽  
Vol 777 (2) ◽  
pp. 164 ◽  
Author(s):  
R. E. Mason ◽  
C. Ramos Almeida ◽  
N. A. Levenson ◽  
R. Nemmen ◽  
A. Alonso-Herrero
Keyword(s):  
Active Galactic Nuclei ◽  
Accretion Disk ◽  
Galactic Nuclei ◽  
Ir Emission
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