D1 Knowledge and understanding of stellar structure, basic reactions of stellar nucleosynthesis, evolution of stars and stellar populations in galaxies.
D2 Knowledge and understanding of some basic exercises on stellar structure and resolution of some simple models of chemical evolution.
D3 Making judgments in understanding when the approximations and the models introduced in the course can be used.

D4 Ability to describe the phenomena described in the course in a clear and precise way, preferably with an appropriate scientific language.

D5 Studying the course also develops those learning skills that will allow students to continue studying mostly autonomously thanks to books on stellar physics or scientific articles on the same topic.

Knowledge of basic principles of Physics (classical mechanics, electromagnetism, nuclear e quantum physics)

Equations of the stellar structure.
Stellar nucleosynthesis.
Primordial Nucleosynthesis.
Stellar evolution in the HR diagram.
Supernovae and stellar remnants: white dwarfs, neutron stars and black holes.
Cosmic abundances.
Chemical evolution of stellar populations in galaxies.

Lecture Notes of F. Matteucci "Introduzione all'evoluzione di stelle e galassie",

"Evolution of stars and stellar populations", M. Salaris & S. Cassisi, 2005
John Wiley & Sons, Ltd

Capitolo I-VII R.G. Tayler, 1994, ``The Stars. Their Structure and Evolution''
Cambridge University Press

"The Physics of Stars" A.C. Phillips, Wiley, Publisher

"The Chemical Evolution of the Galaxy", F. Matteucci, Monograph Kluwer Academic Publisher,
second edition 2003

"Chemical Evolution of galaxies", F. Matteucci, Monograph, Springer-Verlag

Equations of the stellar structure; equation of hydrostatic equilibrium, equation of continuity, equation of state (perfect gas, degenerate gas, and photon gas), equation of energetic transport
(radiative and convective), equation of energy production. Computation of the opacity and average molecular weight. Polytropic models of stellar evolution. Equation of Boltzmann and equation Saha. Stellar nucleosynthesis: main fusion reactions in stars and reaction of neutron capture. Primordial nucleosynthesis. Stellar remnants: white dwarfs, neutron stars and black holes.
Supernovae classification and theories on supernovae of type I and type II. Novae.

Stellar evolution in the Hertzsprung-Russel diagram. Stellar evolution with mass loss.

Cosmic abundances
Chemical evolution of stellar populations in galaxies
Numerical models of chemical evolution.
Applications and comparison with observations: our Galaxy and external galaxies.

Theoretical lectures using blackboard and projected slides. Possible seminars of experts

Any changes to the methods described herein, which may be needed to ensure the application of security protocols linked to any emergency situations will be communicated in the website of the Department of the Course and MOODLE.

The exams may be held in Italian or English, at the student's choice. The verification methods will be explained by the teacher to the students during the presentation of the course in the first lesson; in any case they consist of an oral exam with 3-4 questions covering the program.
During the exam, the student’s knowledge and understanding of stellar structure, basic stellar nucleosynthesis reactions, stellar evolution, and stellar populations in galaxies will be evaluated; as well as their understanding and ability to solve basic exercises on stellar structure and chemical evolution, and their independent judgment in recognizing when the introduced approximations and models can be applied.

Communication skills and the ability to describe one's knowledge and reasoning will also be assessed.
To pass the exam (18/30), the student must demonstrate sufficient knowledge of the topics.
To obtain the maximum grade (30/30 cum laude), the student must demonstrate excellent knowledge of all the topics covered in the course; correctly answer all questions and autonomously connect the various topics.