The modern study of the dynamics of stellar systems requires the use of high-performance computers. Indeed, an accurate modelization of the structure and evolution of self-gravitating systems like planetary systems, open clusters, globular clusters and galaxies imply the evaluation of body-body interaction over the whole size of the structure, a task that is computationally very expensive, in p...

We propose a mathematical scheme to classify the eigenmodes of linear adiabatic oscillations of spherically symmetric stars, with fully taking account of the perturbation to the gravitational potential. The scheme allows us to allocate a unique and continuous integral index (the radial order) to each eigenmode with a positive squared eigenfrequency of any stellar structure, which is invariant a...

The modern study of the dynamics of stellar systems requires the use of high-performance computers. Indeed, an accurate modelization of the structure and evolution of self-gravitating systems like planetary systems, open clusters, globular clusters and galaxies imply the evaluation of body-body interaction over the whole size of the structure, a task that is computationally very expensive, in p...

We study the relations between stellar mass, star formation history, size and internal structure for a complete sample of 80,000 galaxies drawn from the Sloan Digital Sky Survey. We show that low-redshift galaxies divide into two distinct families at a stellar mass of 3×10M⊙. Lower mass galaxies have young stellar populations, star formation histories characterized by recent bursts, low surface...