Nuclear Relativistic Astrophysics 1
A.Y. 2021/2022
Learning objectives
The course introduces the students to the principles of stellar physics, both at the microscopic and macroscopic levels. The topics cover the thermodinamical properties of stellar matter, the equilibrium and stability of self-gravitating objects, the production and transport of energy in stars. In this module, the general theory is applied to the the behaviour of classical stars.
Expected learning outcomes
At the end of the course, the student should know the following topics:
· Equation of state of matter at the different temperatures and densities found in stars
· Gravitational virial theorem and its application to stellar equilibrium and evolution
· Theory of politropes and Eddington's standard model
· Thermonuclear reaction in the various evolutionary phases
· Energy transport (conduction, convection and radiative transport)
· Random walk and diffusion applied to stellar atmospheres (Eddington's atmosphere, color temperature)
· Equations of stellar structure and theory of principal sequence (homology)
· Equation of state of matter at the different temperatures and densities found in stars
· Gravitational virial theorem and its application to stellar equilibrium and evolution
· Theory of politropes and Eddington's standard model
· Thermonuclear reaction in the various evolutionary phases
· Energy transport (conduction, convection and radiative transport)
· Random walk and diffusion applied to stellar atmospheres (Eddington's atmosphere, color temperature)
· Equations of stellar structure and theory of principal sequence (homology)
Lesson period: First semester
Assessment methods: Esame
Assessment result: voto verbalizzato in trentesimi
Single course
This course cannot be attended as a single course. Please check our list of single courses to find the ones available for enrolment.
Course syllabus and organization
Single session
Lesson period
First semester
Lectures will be transmitted in streaming on the virtual class of the department having the same name than the real room where the lecture is taught.
Course syllabus
Introduction to the course - Stellar evolution and formation of compact objects: temperature and density regimes.
Equation of state of stellar matter: EOS of perfect gases (classical, Fermi, Bose) in the non-relativistic and relativistic regime - Electrostatic corrections and effects of beta decay - EOS of dense matter below and above neutron drip - Exotic forms of matter.
Stellar structure and evolution: Hydrostatic equilibrium and the viral theorem -Gravitational contraction and stellar evolution - Thermonuclear reactions inside stars - Adiabatic index, stability and polytropes - Energy transport: conduction, radiative diffusion and convection - Diffusion and random-walk - Equations of stellar structure and standard model for radiative stars.
Equation of state of stellar matter: EOS of perfect gases (classical, Fermi, Bose) in the non-relativistic and relativistic regime - Electrostatic corrections and effects of beta decay - EOS of dense matter below and above neutron drip - Exotic forms of matter.
Stellar structure and evolution: Hydrostatic equilibrium and the viral theorem -Gravitational contraction and stellar evolution - Thermonuclear reactions inside stars - Adiabatic index, stability and polytropes - Energy transport: conduction, radiative diffusion and convection - Diffusion and random-walk - Equations of stellar structure and standard model for radiative stars.
Prerequisites for admission
A basic knowledge of classical physics, quantum mechanics and special relativity is required, but the different topics will be presented consistently during the course.
Teaching methods
Attendance strongly recommended.
Traditional front lectures.
Traditional front lectures.
Teaching Resources
- A.C. Phillips: The Physics of Stars (Wiley Interscience, 1999)
- D. Prialnik: An Introduction to the Theory of Stellar Structure and Evolution (Cambridge University Press, 2000)
- S.L. Shapiro and S.A. Teukolsky: Black Holes, White Dwarfs, and Neutron Stars: the Physics of Compact Objects (Wiley Interscience, 1983)
- D.D. Clayton: Principles of Stellar Evolution and Nucleosynthesis (The University of Chicago Press, 1983)
- D. Prialnik: An Introduction to the Theory of Stellar Structure and Evolution (Cambridge University Press, 2000)
- S.L. Shapiro and S.A. Teukolsky: Black Holes, White Dwarfs, and Neutron Stars: the Physics of Compact Objects (Wiley Interscience, 1983)
- D.D. Clayton: Principles of Stellar Evolution and Nucleosynthesis (The University of Chicago Press, 1983)
Assessment methods and Criteria
The exam consists of an oral discussion of about one hour about the topics presented during the course. The student is tested on both the theory explained and its quantitative application to simple cases.
FIS/05 - ASTRONOMY AND ASTROPHYSICS - University credits: 6
Lessons: 42 hours
Professor:
Pizzochero Pierre Massimo