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2 edition of Sinking satellites and tilting disk galaxies found in the catalog.

Sinking satellites and tilting disk galaxies

Siqin Huang

Sinking satellites and tilting disk galaxies

by Siqin Huang

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  • 17 Currently reading

Published by Graduate Dept. of Astronomy, University of Toronto in Toronto .
Written in English


Edition Notes

Thesis (Ph.D.)--University of Toronto, 1997.

StatementSiqin Huang.
The Physical Object
Pagination115 leaves.
Number of Pages115
ID Numbers
Open LibraryOL17320809M
ISBN 100612279588

We found that galaxies in subhalos with core profiles and high central densities survive for 10 Gyr. The same occurs for galaxies in low density subhalos located far from the host disk influence, whereas satellites in low density DM halos and in tight orbits can eventually be stripped of stars. Density maxima as sites for galaxy formation.- A cross-correlation method to test the dependence of the clustering of galaxies on luminosity.- Constraints on the formation redshift of bright galaxies in biased scenarios.- Biased theories with non-v threshold.- Sinking satellites and disk heating of spiral galaxies

  In order to keep a satellite in orbit, there must be a balance between tidal and Lindblad torques, otherwise the satellite will either break apart or be lost to space permanently. The last boundary for any satellite is the synchronous orbit (a synch), which is the distance where the satellite orbits at the same rate as the rotation of the planet. A) All galaxies contain billions of stars, and all galaxies have spiral shapes. B) All galaxies were born at the same time, and all will die at the same time. C) All galaxies outside the Local Group are moving away from us, and the farther away they are, the faster they're going. D) All galaxies outside the Local Group are orbiting the Local Group.

Minor Mergers: Disk Heating and Aging Although, as discussed in section , there has long been interest in the "sinking satellite" problem, there has been much less simulation work than on mergers between equal mass galaxies. @article{osti_, title = {Testing Lorentz invariance of dark matter with satellite galaxies}, author = {Bettoni, Dario and Nusser, Adi and Blas, Diego and Sibiryakov, Sergey}, abstractNote = {We develop the framework for testing Lorentz invariance in the dark matter sector using galactic dynamics. We consider a Lorentz violating (LV) vector field acting on the dark matter component of a.


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Sinking satellites and tilting disk galaxies by Siqin Huang Download PDF EPUB FB2

Sinking Satellit es and Tilting Disk Galaxies Siclin Huang Doctor of Philosophy. Department of Astronomi. University of Toronto Abstract [ perforni fully self-consistent disk+halo+satellite Y-body simulations to investi- gate the dynamical interaction between a disk galaxy and an infalling by:   We perform fully self-consistent disk+halo+satellite N-body simulations to investigate three different dynamical responses of a disk to an infalling satellite: tilting, warping, and thickening.

Our model is characterized with two cosmologically significant improvements. First, the satellites start at a distance more than three times the radius of the optical : S.

Huang, R. Carlberg. Sinking Satellites and Tilting Disk Galaxies. By Siqin Huang and R. Carlberg. Abstract. The infall of a satellite galaxy onto a galactic disk generally brings in angular momentum that is not aligned with the axis of the disk.

The main dynamical issues addressed are what fraction of the orbital angular momentum of the satellite and the Author: Siqin Huang and R. Carlberg. Sinking Satellites and Tilting Disk Galaxies Huang, Siqin; Carlberg, R. Abstract. The infall of a satellite galaxy onto a galactic disk generally brings in angular momentum that is not aligned with the axis of the disk.

The main dynamical issues addressed are what fraction of the orbital angular momentum of the satellite and the associated Cited by: Sinking satellites and tilting disk galaxies.

By S Huang and R G Carlberg. Abstract. The infall of a satellite galaxy onto a galactic disk generally brings in angular momentum that is not aligned with the axis of the disk.

The main dynamical issues addressed are what fraction of the orbital angular momentum of the satellite and the associated Author: S Huang and R G Carlberg. Abstract. Most large galaxies possess a system of smaller satellite companions, such as the Magellanic Clouds around our own galaxy.

Dynamical friction on the luminous body of the primary galaxy and its dark halo will lead to the decay of satellite orbits and some companions may.

We have carried out a set of self-consistent N-body simulations to study the interaction between disc galaxies and merging satellites with the aim of determining the disc kinematical changes induced by such events.

We explore a region of the. CiteSeerX - Document Details (Isaac Councill, Lee Giles, Pradeep Teregowda): We have carried out a set of self-consistent N-body simulations to study the interaction between disc galaxies and merging satellites with the aim of determining the disc kinematical changes induced by such events.

We explore a region of the parameter space embracing satellites with different masses and internal. and satellite galaxies, of our numerical methods, and of the parameters of the set of simulations we have carried out.

Section 3 studies how the disc is heated and thickened by infalling satellites and a comparison with TO’s results is given in section 4. We discuss the tilting and warping of the disc resulting from such events in section 5.

CiteSeerX - Document Details (Isaac Councill, Lee Giles, Pradeep Teregowda): The present work represents an attempt to understand the ‘rules of behavior ’ of observed warps in the HI disks of spiral galaxies found by Briggs ().

In contrast with most earlier theoretical work, the present study investigates different initial value problems of a warped disk in an oblate (or prolate) halo. Over a Hubble time, the disk of a spiral galaxy and its system of satellites can be severely altered by the action of dynamical friction.

Satellites sink rapidly to the center of the disk when their orbits bring them within the optical radius.

Those satellites in direct orbits with orbital planes close to that of the disk. Sinking Satellites and the Heating of Galaxy Discs The former tend to heat the stellar disc while the latter primarily produce a coherent tilt.

Thus, disc galaxies may accrete quite massive. We numerically solve the equations for $\Theta_j$ for four different types of initial conditions: (1) warp excitation by a passing satellite, (2) excitation by a sinking compact minor satellite, (3) warp evolution due toa tilted halo potential, and (4) warp evolution resulting from an initially tilted disk.

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Elliptical Galaxies: Detailed Structure, Scaling Relations and Formation: Bender, Ralf; Saglia, Roberto P. The Central Structure of Elliptical Galaxies and the Stellar-Dynamical Search for Supermassive Black Holes: Kormendy, John: NICMOS Images of the Cores of the Radio Galaxies M84 and NGC Quillen, A.

Books. Publishing Support In particular, the interaction of a stellar disk with visible dwarf satellite galaxies has been suggested as a way to excite structures in galactic previously ignored, such as the tidal disruption of the satellite as it approaches the host galaxy and the tilting of the disk plane due to the gravitational torque.

Sinking satellites and tilting disk galaxies / Siqin Huang; Photometric properties of low-redshift galaxy clusters / Omar Lopez-Cruz Abstract. UofT Astronomy and Astrophysics Theses List. Compiled by Lee Robbins [email protected]   A dissipating disk does a better job of keeping Uranus tilted, but 45º is not even half of the tilt seen today.

Model 3 is the same as model 2, but Uranus grows in mass as material from the disk falls onto it, shown in Figure 4. Here the obliquity (top panel) reaches a maximum of about 70º and settles to 60º once the disk is gone.

b/a of disk galaxies approximate the inclination of disk fracDevdisk galaxies F comp = fracDeV F deV + (1 - fracDeV) F exp ~40% of galaxies are spiral AGNs hosted by disk galaxies BPT diagram ~30% of AGNs hosted by spirals N AGN,spiral =32, Disk height.

Disk ellipticity. Scientists in the late twentieth century are not the first to view galaxy formation as a phenomenon worthy of explanation in terms of the known laws of physics.

Already in Kant regarded the problem as essentially solved. In his Univerlal Natural Hutory and Theory 0/ the H eaven$ he wrote; "If. Multi-scale interaction between the LMC, the Galactic halo, and the disk is examined with N-body simulations, and precise amplitudes of the Galactic warp excitation are Galactic models are constructed most realistically to satisfy available observational constraints on the local circular velocity, the mass, surface density and thickness of the disk, the mass and size of the bulge.

For almost two decades the properties of ‘dwarf’ galaxies have challenged the cold dark matter (CDM) model of galaxy formation observed dwarf galaxies consist of a rotating stellar disk.The Large-Scale Structure of the Universe (Review of a book by P.J.E. Peebles). Physics To 8, 62 ().

White, S.D.M. and J. Negroponte: The Gravitational Evolution of Structure in a .