
Course unit
ASTROPHYSICS 2
SCM0014352, A.A. 2017/18
Information concerning the students who enrolled in A.Y. 2015/16
ECTS: details
Type 
ScientificDisciplinary Sector 
Credits allocated 
Core courses 
FIS/05 
Astronomy and Astrophysics 
6.0 
Mode of delivery (when and how)
Period 
Second semester 
Year 
3rd Year 
Teaching method 
frontal 
Organisation of didactics
Type of hours 
Credits 
Hours of teaching 
Hours of Individual study 
Shifts 
Lecture 
6.0 
48 
102.0 
No turn 
Start of activities 
26/02/2018 
End of activities 
01/06/2018 
Examination board
Examination board not defined
Prerequisites:

Elements of plane trigonometry, derivatives, integrals, basic knowledge of physics relating to previous courses.
Preparatory courses: Astronomy I (two years) and Astronomy II (model A, third year). 
Target skills and knowledge:

This course aims at providing the students with the fundamental elements of the structure and evolution of stars, from their birth to their final stages. 
Examination methods:

Oral/written examination on all topics covered during the course. 
Assessment criteria:

Assessment of understanding and mastery of the topics. 
Course unit contents:

1. Introduction and overview.
Observational constraints, the HR diagram, massluminosity and massradius relations, stellar populations and abundances.
2. Hydrostatics, energetics and timescales.
Derivation of three of the structure equations (mass, momentum and energy conservation). Hydrostatic and thermal equilibrium. Derivation of the virial theorem and its consequences for stellar evolution. Derivation of the characteristic timescales of stellar evolution.
3. Equation of state (EoS).
Local Thermodynamical equilibrium. General derivation of n, U, P from statistical mechanics. Limiting cases: ideal gas, degeneracy. Mixture of gas and radiation. Adiabatic processes. Ionization (Saha equation, consequences for thermodynamic properties).
4. Energy transport in stellar interiors.
The 4th equation of stellar structure: the energy transport equation.
Diffusion approximation for radiation transport. The radiative temperature gradient . Opacity. Eddington luminosity. Convection: Derivation of stability criteria (Schwarzschild, Ledoux) .Convective energy transport: orderofmagnitude derivation. Mixinglength theory.
5.Nuclear reactions.
Nuclear energy generation (binding energy). Derivation of thermonuclear reaction rates (cross sections, tunnel effect, Gamow peak). Temperature dependence of reaction rates .Nuclear burning cycles: Hburning by ppchain and CNOcycle. He burning by 3alpha and alpha+C reactions. Advanced burning reactions.
6. Stellar evolution equations.
Overview, time/space derivatives, limiting cases. Boundary conditions and their effect on stellar structure. How to obtain solutions.
7. Simple stellar models.
Polytropic models.Homology relations: principles, derivations, application to contraction and the main sequence. Stability of stars: derivation of simplified criteria for dynamical and secular stability.
8. Schematic evolution from the virial theorem (VT).
Evolution of the stellar centre combining the VT and the EoS: evolution tracks in terms of (P,rho) and (T,rho). Evolution towards degeneracy or not. The Chandrasekhar mass, lowmass vs massive stars . Critical ignition masses, brown dwarfs, nuclear burning cycles.
9. Detailed evolution: towards and on the main sequence.
Simple derivation of Hayashi line, preMS evolution tracks properties of the ZAMS: ML and MR relations, occurrence of convection zones evolution across the MS band: structural changes, lowmass vs highmass, effects of overshooting.
10. PostMS evolution.
The SchoenbergChandrasekhar limit, the mirror principle. Hshell burning: Hertzsprunggap, red giant branch, first dredgeup. Heburning: horizontal branch, loops, Cepheids. RGB mass loss.
11. Late evolution of low and intermediatemass stars.
The Asymptotic Giant Branch: thermal pulses, 2nd/3rd dredgeup, mass loss, nucleosynthesis. White dwarfs: structure, nonideal effects, derivation of simple cooling theory.
12. PreSN evolution of massive stars.
Importance of mass loss across the HRD (O stars, RSG, LBV and WR stars). Modern evolution tracks. Advanced evolution of the core: nuclear burning cycles and neutrino losses, acceleration of core evolution. PreSN structure
13. Explosions and remnants of massive stars.
Evolution of the core towards collapse: Fedisintegration, electron captures, role of neutrinos supernovae. Observed properties and relation to massive star evolution. Limiting masses for neutron star and black hole formation, dependence on mass loss and metallicity. 
Planned learning activities and teaching methods:

Lectures, with use of both classical methodology (lectures at the blackboard) that the media (slides, movies, applets, webinterfaces for the onthefly generation of stellar models). 
Additional notes about suggested reading:

Slides and other material available in electronic format to the students. 
Textbooks (and optional supplementary readings) 

M. Salaris & S. Cassisi, Evolution of Stars and Stellar Populations. : John Wiley & Sons, 2005. Testo consigliato, non obbligatorio. Puo' essere consultato presso l'ufficio del docente.

C.J. Hansen, S.D. Kawaler & V. Trimble, Stellar Interiors. : SpringerVerlag, 2004. Testo consigliato, non obbligatorio. Puo' essere consultato presso l'ufficio del docente.

R. Kippenhahn & A. Weigert, Stellar Structure and Evolution. : SpringerVerlag, 1990. Testo consigliato, non obbligatorio. Puo' essere consultato presso l'ufficio del docente.

D. Prialnik, An Introduction to the Theory of Stellar Structure and Evolution. : Cambridge University Press, 2009. Testo consigliato, non obbligatorio. Puo' essere consultato presso l'ufficio del docente.


