Galactic dynamics

J. Binney and S. Tremaine, Galactic Dynamics, Princeton University Press 1987, 2008, is another classic text, recommended for background reading on Galactic aspects of abundances. 

Binney, J. Tremaine, S. 1987, 2008, Galactic Dynamics, Princeton Princeton University Press. 

CELESTIAL MECHANICS is the study of dynamics in gravitational fields of cosmic bodies. In recent years, this has come to include gravitational statistical mechanics, galactic dynamics, nonlinear stability theory and chaos. 

Supernova explosions produce spherical shock waves with stellar remnants. The shock wave propagates into interstellar space and dynamically interacts with the ambient interstellar clouds. Yusef-Zadeh et al. [48] reported that shock-excited OH maser emission outlined the galactic center supernova remnant. Aschenbach et al. [49] suggested tliat the X-ray emission associated with the ejected objects was produced by shock heating of the ambient medimn resulting Ifom supersonic motion of the objects. 

In the picture the expectation fines are shown with an inclusion of the dynamical evolution. I.e. here NSs movements in the Galactic potential are accurately calculated. To plot them we use the same model of progenitor distribution and SN rate as in (Popov et al. 2003). At birth NSs obtain kick velocities in accordance with Arzoumanian et al. (2002) model, and move in the galactic potential. 

Ptuskin, V.S. (2001). Propagation, confinement models, and large-scale dynamical effects of galactic cosmic rays , Space. Sci. Rev. 99, 281... 

Abstract We map and study the dynamics of the Milky Way s spiral arms in our vicinity, using the birth place of open clusters. Since these objects are located in the galactic plane and are born primarily in the arms, they are an excellent tool for analyzing the dynamics of the spiral structure. Using their birth place, we find evidence for multiple spiral patterns with different speeds. The Carina arm appears now to be a superposition of both. The results are important for proper modeling of cosmic ray diffusion in our galactic vicinity. 

Recent chemo-dynamical simulations for one instantaneous starburst also suggest the possibiliy of galactic winds and that these winds are metal enriched (MacLow Ferrara 1999 Recchi et al. 2001). 

Purely chemical models (no dynamics) have been computed by several authors by varying the number of bursts, the time of occurrence of bursts, tburst, the star formation efficiency, the type of galactic wind, the IMF and the nucleosynthesis prescriptions (Marconi et al. 1994 Kunth et al.1995 Bradamante et al.1998). The main conclusions of these papers can be summarized as follows ... 

Figure 10. Chemo-dynamical simulation of an instantaneous starburst from Recchi et al. (2001). The development of a galactic wind is evident along the z-axis, since the assumed configuration is flattened.The age of the burst is indicated in Myr.

Cincotta, P. M. and Simo, C. (2000). Simple tools to study global dynamics in non-axisymmetric galactic potentials - I. Astron. and Astroph. suppl., 147 205-228. 

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