Investigating a self-consistent galactic potential with central mass concentration

1993 ◽  
pp. 385-386 ◽  
Author(s):  
H. Hasan ◽  
J. A. Sellwood ◽  
C. A. Norman
Keyword(s):  
Mass Concentration ◽  
Central Mass ◽  
Self Consistent ◽  
Galactic Potential

scholarly journals Investigating a self-consistent galactic potential with central mass

1993 ◽  
Vol 153 ◽  
pp. 385-386
Author(s):  
H. Hasan ◽  
J. A. Sellwood ◽  
C. A. Norman
Keyword(s):  
Mass Concentration ◽  
Central Mass ◽  
Self Consistent ◽  
Galactic Potential

The evolution of a barred galactic potential containing a central mass concentration is examined by means of a self-consistent 2-D N-body simulation. It is found that the bar weakens as the central mass grows and eventually dissolves, in agreement with earlier orbital studies of this problem.

scholarly journals Instabilities of Uniformly Rotating Disks

1996 ◽  
Vol 169 ◽  
pp. 349-350 ◽  
Author(s):  
P. Vauterin ◽  
H. Dejonghe
Keyword(s):  
Distribution Function ◽  
Differential Rotation ◽  
Mass Concentration ◽  
Expansion Method ◽  
Rotating Disks ◽  
Central Mass ◽  
Reasonable Approximation ◽  
Central Regions ◽  
Series Expansion Method

We explore a series expansion method to calculate the instabilities and the structure of the perturbations for a variety of uniformly rotating finite stellar disks. This survey focuses on the role of the distribution function in stability analyses. Although the potential does not show differential rotation, it will in many cases be a reasonable approximation for the disk in the central regions of galaxies without massive central mass concentration.

scholarly journals 9.14. A simple mass estimate for central black holes in cuspy galaxies

1998 ◽  
Vol 184 ◽  
pp. 409-410
Author(s):  
S. de Rijcke ◽  
V. de Bruyne ◽  
H. Dejonghe ◽  
A. Mathieu
Keyword(s):  
Mass Concentration ◽  
Velocity Dispersion ◽  
Minor Axis ◽  
Minimum Mass ◽  
Central Mass ◽  
Central Regions ◽  
Monotonically Decreasing Function ◽  
Mass Estimate ◽  
Current Mass ◽  
Simple Mass

We argue that the velocity dispersion of the stars is likely a monotonically decreasing function of radius along the minor axis in the central regions of cuspy galaxies. We show that then a central mass concentration (a black hole) must be present and calculate its minimum mass, M⊙. This lower bound is relevant and entirely consistent with current mass estimates.

Dynamical evidence for a central mass concentration in the galaxy M87

1978 ◽  
Vol 221 ◽  
pp. 731 ◽  
Author(s):  
W. L. W. Sargent ◽  
P. J. Young ◽  
C. R. Lynds ◽  
A. Boksenberg ◽  
K. Shortridge ◽  
...  
Keyword(s):  
Mass Concentration ◽  
Central Mass ◽  
The Galaxy

scholarly journals Orbits in a Stäckel Approximation

1999 ◽  
Vol 172 ◽  
pp. 395-396
Author(s):  
V. De Bruyne ◽  
F. Leeuwin ◽  
H. Dejonghe
Keyword(s):  
Black Hole ◽  
Numerical Integration ◽  
Mass Concentration ◽  
Good Representation ◽  
Central Mass ◽  
Good Basis ◽  
The Third ◽  
Integrable Potential ◽  
Building Models ◽  
The Family

Because of their analytical simplicity and regularity, Stäckel potentials are attractive tools for modelling galaxies. The third integral I3 is explicitly known in a Stäckel potential, and can be used as an approximation to the effective third integral, in order to construct three-integral models (cf. Dejonghe, et al., 1996, A&A 306, 363).Moreover, Stäckel potentials turn out to yield good global descriptions for either axisymmetric or triaxial systems without central mass concentration (de Zeeuw 1985, MNRAS 216, 273, de Zeeuw & Lynden-Bell 1985, MNRAS 215, 713), and even for some systems with a black hole included (Sridhar & Touma 1997, MNRAS 292, 657).One long-standing concern though, is that Stäckel potentials form only a very small subspace in the family of all potentials. The main orbit families found by numerical integration in general triaxial potentials are present in a Stäckel potential (Schwarzschild 1981, ApJ 232, 236, de Zeeuw 1985, MNRAS 216, 273), but there is obviously no place in an integrable potential for smaller orbital families or stochastic orbits. However, since regular orbits are the rule rather than the exception, a potential which yields a good representation of those orbits is certainly a good basis for building models.

scholarly journals EFFECT OF CENTRAL MASS CONCENTRATION ON THE FORMATION OF NUCLEAR SPIRALS IN BARRED GALAXIES

2009 ◽  
Vol 693 (1) ◽  
pp. 586-596 ◽  
Author(s):  
Parijat Thakur ◽  
H. B. Ann ◽  
Ing-Guey Jiang
Keyword(s):  
Mass Concentration ◽  
Central Mass ◽  
Barred Galaxies

scholarly journals Luminosity Distribution in CD Clusters

1994 ◽  
Vol 161 ◽  
pp. 629-631
Author(s):  
F.W. Baier
Keyword(s):  
Galaxy Clusters ◽  
Mass Distribution ◽  
Mass Concentration ◽  
Central Mass ◽  
Cooling Flows ◽  
Galaxy Distribution ◽  
Cd Galaxies ◽  
Cluster Properties ◽  
General Cluster

The ratio of contributions from cannibalism and from cooling flows to the final cD galaxies in diverse clusters seems to be different. It should be determined by some general cluster properties as for instance the central mass concentration. Assuming that mass distribution is tantamount to luminosity distribution we have analyzed the question of possible luminosity segregation in the radial galaxy distribution of galaxy clusters (Baier & Schmidt 1992; Baier & MacGillivray 1994).

The Formation of Red Giants

1992 ◽  
Vol 10 (2) ◽  
pp. 125-127 ◽  
Author(s):  
Cheryl Frost ◽  
John C. Lattanzio
Keyword(s):  
Mass Concentration ◽  
Red Giants ◽  
Central Mass ◽  
Primary Agent

AbstractThe astrophysical literature contains many discussions on exactly which changes in a star’s structure are responsible for the extremely large radii found after core hydrogen exhaustion. Different authors favour different mechanisms. Unfortunately none of the proposals are easily verified nor are they easily disproven. In this paper we examine the suggestion that it is the increased central mass concentration (i.e., the growth of the hydrogen exhausted core) which is the primary agent responsible for envelope growth.

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