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Tidal tails of dwarf galaxies on different orbits around the Milky Way | | Ewa L. Lokas
; Grzegorz Gajda
; Stelios Kazantzidis
; | | Date: |
12 Feb 2013 | | Abstract: | We present a phenomenological description of the properties of tidal tails
forming around dwarf galaxies orbiting the Milky Way. For this purpose we use
collisionless N-body simulations of dwarfs initially composed of a disk
embedded in an NFW dark matter halo. The dwarfs are placed on seven orbits
around the Milky Way-like host, differing in size and eccentricity, and their
evolution is followed for 10 Gyr. In addition to the well-studied morphological
and dynamical transformation of the dwarf’s main body, the tidal stripping
causes them to lose a substantial fraction of mass both in dark matter and
stars which form pronounced tidal tails. We focus on the properties of the
stellar component of the tidal tails thus formed. We first discuss the break
radii in the stellar density profile defining the transition to tidal tails as
the radii where the profile is steepest and relate them to the classically
defined tidal radii. We then calculate the relative density and velocity of the
tails at a few break radii as a function of the orbital phase. Next, we measure
the orientation of the tails with respect to an observer placed at the centre
of the Milky Way. The tails are perpendicular to this line of sight only for a
short period of time near the pericentre. For most of the time the angles
between the tails and this line of sight are low, with orbit-averaged medians
below 30 degrees for all, even the almost circular orbit. The median angle is
typically lower while the maximum relative density higher for more eccentric
orbits. The combined effects of relative density and orientation of the tails
suggest that they should be easiest to detect for dwarf galaxies soon after
their pericentre passage. | | Source: | arXiv, 1302.2744 | | Services: | Forum | Review | PDF | Favorites | |
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