Seismological challenges for stellar structure

Variational Principles for Stellar Structure

The four equations of stellar structure are reformulated as two alternate pairs of variational principles. Different thermodynamic representations lead to the same hydromechanical equations, but the thermal equations require, not the entropy, but the temperature as the thermal field variable. Our treatment emphasizes the hydrostatic energy and the entropy production rate of luminosity produced ...

On a stellar structure for a stellar manifold

It is well known that a compact two dimensional surface is homeomorphic to a polygon with the edges identified in pairs. This paper not only presents a new proof of this statement but also generalizes it for any connected n-dimensional stellar manifold with a finite number of vertices.

Stellar Evolutionary Models: challenges from observations of stellar systems

We briefly review some constraints† for stellar models in various mass regimes and evolutionary stages as provided by observational data from spectroscopy to multi-wavelenghts photometry. The accuracy of present generation of stellar models can be significantly improved only through an extensive comparison between theory and observations.

Stellar Structure and Evolution

Models of Stellar Structure for Asteroseismology

Among the problems still open in the study of stellar structure, we discuss in particular some issues related to the study of convection. We have recently built up complete stellar models, adopting a consistent formulation of convection both in the non gray atmosphere and in the interior, to be used for non adiabatic pulsational analysis, and discuss in some details two problems which have been...