Nuclear Relativistic Astrophysics 1
A.Y. 2024/2025
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: Second semester
Assessment methods: Esame
Assessment result: voto verbalizzato in trentesimi
Single course
This course can be attended as a single course.
Course syllabus and organization
Single session
Responsible
Lesson period
Second semester
Course syllabus
Introduction to the course - Typical density and temperature conditions in compact stars - Limits of applicability of classical physics in compact stars. Equation of state of stellar matter: overview of thermodynamics and statistical mechanics - Perfect gas and degenerate Fermi gas: non-relativistic, ultrarelativistic and general case. Equation of state of dense matter: the NN interaction problem and phenomenological potentials - Hydrostatic equilibrium of a non-relativistic and ultrarelativistic gas - Adiabatic index and instability of self-gravitating bodies - Polytropes: Lane-Emden equations, masses and radii - The equations of stellar structure.
Overview of General Relativity, TOV equations of stellar structure in relativity.
Predictions using polytropic theory - Chandrasekhar limiting mass for white dwarfs and discussion of limit mass problem for neutron stars, dependence on equation of state.
Supernova explosions: Introduction and phenomenology.
Advanced equation-of-state models, exotic matter at high densities.
Classical and relativistic rotating stars - comparison with the Black Hole case. Kerr metric and slow rotation approximation.
Magnetic fields in neutron stars - rotating dipole model and magnetohydrodynamic models. Superfluids and superconductors in neutron stars.
Heat equation and cooling of compact stars - neutrino emission.
Introduction to gravitational waves and emission mechanisms - chirps from the coalescence of compact objects and continuous waves from neutron stars.
Overview of General Relativity, TOV equations of stellar structure in relativity.
Predictions using polytropic theory - Chandrasekhar limiting mass for white dwarfs and discussion of limit mass problem for neutron stars, dependence on equation of state.
Supernova explosions: Introduction and phenomenology.
Advanced equation-of-state models, exotic matter at high densities.
Classical and relativistic rotating stars - comparison with the Black Hole case. Kerr metric and slow rotation approximation.
Magnetic fields in neutron stars - rotating dipole model and magnetohydrodynamic models. Superfluids and superconductors in neutron stars.
Heat equation and cooling of compact stars - neutrino emission.
Introduction to gravitational waves and emission mechanisms - chirps from the coalescence of compact objects and continuous waves from neutron stars.
Prerequisites for admission
No prior knowledge is required, other than a basic understanding of classical physics, quantum mechanics and special relativity. The various topics will be introduced sequentially and in a consistent manner during the course itself.
Teaching methods
Attendance:
Strongly recommended
Delivery method:
Traditional
Strongly recommended
Delivery method:
Traditional
Teaching Resources
S.L. Shapiro and S.A. Teukolsky: Black Holes, White Dwarfs, and Neutron Stars: the Physics of Compact Objects (Wiley Interscience, 1983)
Glendenning: Compact Stars: Nuclear Physics, Particle Physics and General Relativity (Springer Astronomy and Astrophysics Library, 2012)
Weinberg: Gravitation and cosmology: principles and applications of the general theory of relativity (Wiley, 1972)
Misner, Thorne & Wheeler: Gravitation (W.H. Freeman Princeton University Press, 1973)
Silbar & Reddy: Neutron Stars for Undergraduates, Am.J.Phys. 72 (2004) 892-905, arXiv:nucl-
th/0309041
Tassoul: Theory of rotating stars (Princeton University Press, 1978).
Haensel, Potekhin & Yakovlev: Neutron Stars 1: Equation of State and Structure (Springer Astrophysics and Space Science Library, 2006)
Glendenning: Compact Stars: Nuclear Physics, Particle Physics and General Relativity (Springer Astronomy and Astrophysics Library, 2012)
Weinberg: Gravitation and cosmology: principles and applications of the general theory of relativity (Wiley, 1972)
Misner, Thorne & Wheeler: Gravitation (W.H. Freeman Princeton University Press, 1973)
Silbar & Reddy: Neutron Stars for Undergraduates, Am.J.Phys. 72 (2004) 892-905, arXiv:nucl-
th/0309041
Tassoul: Theory of rotating stars (Princeton University Press, 1978).
Haensel, Potekhin & Yakovlev: Neutron Stars 1: Equation of State and Structure (Springer Astrophysics and Space Science Library, 2006)
Assessment methods and Criteria
The exam consists of an oral discussion, lasting approximately one hour, on the topics covered in the course. Both theoretical notions and their quantitative application to simple cases will be tested.
FIS/05 - ASTRONOMY AND ASTROPHYSICS - University credits: 6
Lessons: 42 hours
Professor:
Haskell Brynmor
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