Dissipative phenomena in extended-bodies interactions I: Methods Dwarf galaxies of the Local Group and their synthetic CMDs

Abstract

Dissipative phenomena occurring during the orbital evolution of a dwarf satellite galaxy around a host galaxy may leave signatures in the star formation activity and signatures in the colour magnitude diagram of the galaxy stellar content. Our goal is to reach a simple and qualitative description of the these complicated phenomena. We develop an analytical and numerical technique able to study ram pressure, Kelvin-Helmholtz instability, Rayleigh-Taylor and tidal forces acting on the star formation processes in molecular clouds. We consider it together with synthetic colour magnitude diagrams techniques. We developed a method to investigate the connections existing between gas consumption processes and star formation processes in the context of the two extended-body interaction with special attention to the dwarf galaxies dynamical regime.

Accepted on A&A

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Cited by in corpus (7)

• Three-dimensional hydrodynamical simulations of the supernovae-driven gas loss in the dwarf spheroidal galaxy Ursa Minor
• Theory of stellar convection: Removing the Mixing-Length Parameter
• Spiral arm kinematics for Milky Way stellar populations
• GalMod: a Galactic synthesis population model
• Theory of Stellar Population Synthesis with an application to N-Body simulations
• Theory of stellar convection II: first stellar models
• Environmental effects on star formation in dwarf galaxies and star clusters