Dynamical Properties of Collisionless Star Streams
arXiv:1412.2405 · doi:10.1088/0004-637X/800/2/133
Abstract
A sufficiently extended satellite in the tidal field of a host galaxy loses mass to create nearly symmetric leading and trailing tidal streams. We study the case in which tidal heating drives mass loss from a low mass satellite. The stream effectively has two dynamical components, a common angular momentum core superposed with episodic pulses with a broader angular momentum distribution. The pulses appear as spurs on the stream, oscillating above and below the stream centerline, stretching and blurring in configuration space as they move away from the cluster. Low orbital eccentricity streams are smoother and have less differential motion than high eccentricity streams. The tail of a high eccentricity stream can develop a fan of particles which wraps around at apocenter in a shell feature. We show that scaling the essentially stationary action-angle variables with the cube root of the satellite mass allows a low mass satellite stream to accurately predict the features in the stream from a satellite a thousand times more massive. As a practical astrophysical application, we demonstrate that narrow gaps in a moderate eccentricity stream, such as GD-1, blur out to 50\% contrast over approximately 6 radial periods. A high eccentricity stream, such as Pal~5, will blur small gaps in only radial 2 orbits as can be understood from the much larger dispersion of angular momentum in the stream.
arXiv commentApJ accepted
References in corpus (30)
- The cosmological simulation code GADGET-2
- The Aquarius Project: the subhalos of galactic halos
- Formation and evolution of galaxy dark matter halos and their substructure
- Building up the Stellar Halo of the Galaxy
- A 2MASS All-Sky View of the Sagittarius Dwarf Galaxy: IV. Modeling the Sagittarius Tidal Tails
- The extended tails of Palomar 5: A ten degree arc of globular cluster tidal debris
- Fossil Signatures of Ancient Accretion Events in the Halo
- A Prescription for Building the Milky Way's Halo from Disrupted Satellites
- Phase-space structure in the local dark matter distribution and its signature in direct detection experiments
- Clumpy Streams from Clumpy Halos: Detecting Missing Satellites with Cold Stellar Structures
- Modeling the disruption of the globular cluster Pal5 by Galactic tides
- Tidal Tails of Star Clusters
- More on the structure of tidal tails
- On the Orbits of Infalling Satellite Halos
- Dark Matter Sub-Halo Counts via Star Stream Crossings
- On the structure of tidal tails
- Dynamical modeling of tidal streams
- Using Tidal Tails to Probe Dark Matter Halos
- Stream-orbit misalignment I: The dangers of orbit-fitting
- The mechanics of tidal streams
- The geometry of phase mixing
- Milky Way Mass and Potential Recovery Using Tidal Streams in a Realistic Halo
- Stellar Streams as Probes of Dark Halo Mass and Morphology: A Bayesian Reconstruction
- Disassembling the Galaxy with angle-action coordinates
- An Orbit Fit for the Grillmair Dionatos Cold Stellar Stream
- Using gaps in N-body tidal streams to probe missing satellites
- Actions, angles and frequencies for numerically integrated orbits
- Fitting orbits to tidal streams
- Development of multiple tidal tails around globular clusters and dwarf satellite galaxies
- Enhancements to velocity-dependent dark matter interactions from tidal streams and shells in the Andromeda galaxy