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Dynamics of the Milky Way: Tidal Streams and Extended by Jason Sanders

By Jason Sanders

This paintings offers a examine of tools valuable for modeling and figuring out dynamical structures within the Galaxy. A common coordinate method for the learn of dynamical platforms is the angle-action coordinate approach. New tools for the approximation of the action-angle variables in most cases potentials are offered and mentioned. those new instruments are utilized to the development of dynamical types for 2 of the Galaxy’s elements: tidal streams and the Galactic disc. Tidal streams are remnants of tidally stripped satellites within the Milky approach that have the consequences of the massive scale constitution of the Galactic gravitational power, whereas the Galactic disc offers insights into the character of the Galaxy close to the sunlight. acceptable action-based types are awarded and mentioned for those elements, and prolonged to incorporate extra 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

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The Geneva-Copenhagen Survey (GCS) (Nordström et al. 2004) is a sample of 16682 nearby F and G stars, and is perhaps the best data set with full 6D phase-space information. It provides us with a platform to motivate a discussion of errors involved in a practical calculation. The GCS has been analysed by many authors and specifically looked at in angle-action space by Sellwood (2010) and McMillan (2011b). From the table produced by Holmberg et al. (2009), we select the 13,518 objects that have full 6D phase-space information.

The minimum and maximum τ edges are distinguished by inspecting the sign of τ¨ . For all realistic potentials every orbit crosses the z = 0 plane so we set ν− = c2 . 3. We can now find a best-fitting Stäckel potential over this region. Using Eq. 19) we tabulate f (λ) and f (ν) for 40 points in (λ− , λ+ ) and (ν− , ν+ ) respectively so that we may interpolate these smooth functions. Any call outside the ranges is calculated fully using Eq. 19) with a full re-computation of χ(τ ¯ ). 4. With the best fit potential now calculated, we find I3 using Eq.

The black lines are the equipotential contours of McMillan’s bestfitting Milky Way potential. The red lines show the lines of constant λ and ν that define the region over which the potential is fitted shown in Fig. 2. 8 kpc. Also shown in the figure are the curves defining the fit region and equipotential contours for McMillan’s best-fitting potential. The residuals in the fitted potential over the fitting region defined in Fig. 2 are plotted in Fig. 3. 2 % of the maximum difference in the potential across the fitting region.

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