By Jason Sanders
This paintings provides a research of equipment helpful for modeling and knowing dynamical platforms within the Galaxy. A typical coordinate process for the research of dynamical platforms is the angle-action coordinate method. New equipment for the approximation of the action-angle variables typically potentials are awarded and mentioned. those new instruments are utilized to the development of dynamical versions for 2 of the Galaxy’s elements: tidal streams and the Galactic disc. Tidal streams are remnants of tidally stripped satellites within the Milky manner that have the consequences of the massive scale constitution of the Galactic gravitational strength, whereas the Galactic disc presents insights into the character of the Galaxy close to the sunlight. acceptable action-based types are awarded and mentioned for those parts, and prolonged to incorporate additional info similar to the metallicity of stars.
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Extra info for Dynamics of the Milky Way: Tidal Streams and Extended Distribution Functions for the Galactic Disc
We present a discussion of the dependence of these results on the progenitor mass, and demonstrate that the misalignment is mass-independent for the range of masses of observed streams. Hence, orbit-fitting does not yield better constraints on the potential if one uses 14 1 Introduction narrower, lower-mass streams. The work in this chapter is based on that published by Sanders and Binney (2013a). 5 Stream Modelling in Angle-Frequency Space In Chap. 6, we present new techniques for constraining the Galactic potential using tidal streams, which crucially do not rely on the assumption that a stream delineates an orbit.
The method recovers the generating function that maps an analytic phase-space torus to the torus to which the orbit is confined, by simultaneously solving the constraints provided by each time step. 7 Overview of Thesis 13 recovering the actions and frequencies of tori in a triaxial Stäckel potential, and use it to investigate the structure of orbits in a triaxial potential that has been fitted to our Galaxy’s Sagittarius stream. We show how the method operates when working with near-resonant and chaotic orbits.
However, the discussion in Eyre and Binney (2011) was limited to potentials that have separable Hamilton-Jacobi equations (Stäckel potentials, of which spherical potentials are limiting cases) for which the angle-action coordinates are numerically tractable. 6 Tidal Streams 11 The angle-action approach allows for a clearer understanding of the structure of streams, as well as presenting a route to improving the modelling of the streams in order to constrain the potential. This approach more correctly models the formation and dynamics of the stream.
Dynamics of the Milky Way: Tidal Streams and Extended Distribution Functions for the Galactic Disc by Jason Sanders