Stellar Dynamics

Challenging stellar dynamical problems, such as the study of gravothermal oscillations in star clusters, have in the past initiated the very successful building of GRAPE special purpose computers. It is discussed, that present day tasks such as the formation and evolution of galactic nuclei with one or more massive black holes and the coupled stellar and gas dynamical processes in

An improved transformation of the full width at half maxima (FWHM) of the [O III] 5007 line in AGNs to the stellar velocity dispersion, sigma, of the host galaxy is given. This significantly reduces the systematic errors in using the [O III] FWHM as a proxy for sigma. AGN black hole masses, M, estimated using the Dibai single epoch spectrum method, are combined with the new estimates of sigma to give a revised AGN M-sigma relationship extending up to high masses. This shows that the masses of the most massive black holes are systematically higher than predicted by extrapolation of M \propto sigma^4 to high masses. This supports recent suggestions that stellar dynamical masses of the most massive black holes have been systematically underestimated. The steepening of the M-sigma relationship is consistent with the absence of very high sigma galaxies in the local universe and with the curvature of the Faber-Jackson relationship. There appears to be significantly less intrinsic scatter ...

This paper investigates spheroidal galaxies comprising a self-interacting dark matter (SIDM) halo plus de Vaucouleurs stellar distribution. These are coupled only via their shared gravitational field, which is computed consistently from the density profiles. Assuming conservation of mass, momentum and angular momentum, perturbation analyses reveal the galaxy's response to radial disturbance. The modes depend on fundamental dark matter properties, the stellar mass, and the halo's mass and radius. The coupling of stars and dark matter stabilizes some haloes that would be unstable as one-fluid models. However the centrally densest haloes are unstable, causing radial flows of SIDM and stars (sometimes in opposite directions). Depending on the dark microphysics, some highly diffuse haloes are also unstable. Unstable galaxies might shed their outskirts or collapse. Observed elliptical galaxies appear to exist in the safe domain. Halo pulsations are possible. The innermost node of SIDM waves may occur within 10 half-light radii. Induced stellar ripples may also occur at detectable radii if higher overtones are excited. If any SIDM exists, observational skotoseismology of galaxies could probe dark matter (DM) physics, measure the sizes of specific systems, and perhaps help explain peculiar objects (e.g. some shell galaxies, and the growth of red nuggets).

A new empirical formulae is given for estimating the masses of black holes in AGNs from the H beta velocity dispersion and the continuum luminosity at 5100 Angstroms. It is calibrated to reverberation-mapping and stellar-dynamical estimates of black hole masses. The resulting mass estimates are as accurate as reverberation-mapping and stellar-dynamical estimates. The new mass estimates show that there is very little scatter in the M_{bh} - L_{bulge} relationship for high-luminosity galaxies, and that the scatter increases substantially in lower-mass galaxies.

Abstract.  In this article are the 5 tables for calculating the average translational velocities of all milisecond pulsars and others fast spinning bodies and shift the center of gravity due to the rotation.  Corrections theory ideal spining circle for real  bodies. Extreme values for neutron stars. Summary values  for neutron stars. A new perspective on neutronization and nuclear fusion.  Consent theory with the real Universe. From well-functioning theory for milisecond pulsars are derived estimates for raelisation new mode of transport on the principle rotation.  CNN's Larry King covered the news story in the days following the incident, and according to Steve Allen, a private pilot who witnessed the UFO, the object was travelling at a high rate of speed which supposedly reached 3,000 feet in the air.  3000 ft/s (910 m/s) velocity .

For radius UFO  r= 20m,  the estimate revolutions per second is 18 207  rps 

for  real  UFO

Keywords: stars: kinematics, pulsars: general,  stellar dynamics,  , stars: neutron, 
PACS number:  97.60.Gb, 97.60.Jd,

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The long-term evolution of massive black hole binaries at the centers of galaxies is studied in a variety of physical regimes, with the aim of resolving the '' final parsec problem,'' ie, how black hole binaries manage to shrink to separations at which emission ...

The stability of the 2:3 mean motion resonance with Neptune is systematically explored and compared to the observed resonant population. It is shown that orbits with small and moderate amplitudes of the resonant angle are stable over the age of the Solar System. The observed resonant population is distributed within the stability limits. There exists an interval of large resonant amplitudes, where orbits are marginally unstable. Resonant objects starting in this interval may leave the resonance by slow increase of their resonant amplitudes on a time scale of several billion years. These objects eventually attain Neptune-crossing trajectories and contribute to the flux of Jupiter-family comets. The number of objects leaking from the 2:3 resonance per time interval is calibrated by the number of objects needed to keep the Jupiter-family comets population in steady state. This allows us to compute the upper limit of the number of resonant objects with cometary size. The effects of collisions and mutual gravitational scattering are discussed in this context.