Found 42 talks archived in The Galaxy
2- More on isochrones
- bolometric corrections and Teff-color relations
- populating isochrones, and the IMF
- simulating star clusters
- simulating apparent and detached binaries
- simulating interacting binaries
2- Stellar orbits and dynamical models
- orbits in various potentials, Jeans Thm, DF models, Schwarzschild, M2M
2- The thin disk.
- observational issues with the star formation history and the dynamical evolution of the thin disk.
- continuing gas accretion
- theoretical ideas about the formation and evolution of the thin disk.
2- Poisson solvers
- fixed and adaptive grids
1- Overview of the structure of our Galaxy in the context of other galaxies
- the basic components
- dark matter properties
- general ideas about galaxy assembly
1- The basics
- overview of stellar evolution as a function of mass and metallicity
- from evolutionary tracks to isochrones
- quick overview of chemical changes at the stellar surface
1- Fundamental stellar dynamics
- relaxation, collisionless dynamics
- distribution functions, Jeans eqs, etc.
1- The use and abuse of N-body codes
- relaxation in spheres and disks, collective enhancement
- code structure, block time steps
In the past few years, a series of discoveries have been made of objects which appear to be accreting stellar mass black holes in globular clusters -- both in the Milky Way and in other nearby galaxies. I will discuss why the theoretical work which suggested that such objects would be unlikely to exist, the observations showing they do exist, some of the unusual aspects of some of the individual sources, and the new theoretical framework for producing them.
Among the different effects of secular evolution of galaxies we find how bars influence enormously their host galaxies. For many years now, it is known how the evolution of bars will produce different boxy/peanut and X-shape bulges. In this context our Milky Way is an example of a boxy bulge, and we will present a self consistent N-body simulation of a barred galaxy that will be compared with some of the Milky Way available data. We will compare the model in terms of morphology and structure, kinematics and finally metallicity gradients.
- Deciphering the Milky Way: dark and visible matter at home and at the edge of the UniverseDr. Elena D’OnghiaTuesday July 17, 2018 - 12:30 (Aula)
- COLLOQUIA: Chemical evolution in the Milky-Way and its satellites: an observational perspectiveVanessa HillWednesday July 18, 2018 - 10:30 (Aula)