Physics of Stars
Faculteit  Science and Engineering 
Jaar  2019/20 
Vakcode  STFVSE5 
Vaknaam  Physics of Stars 
Niveau(s)  bachelor 
Voertaal  Engels 
Periode  semester II b 
ECTS  5 
Rooster  rooster.rug.nl 
Uitgebreide vaknaam  Physics of Stars  
Leerdoelen  At the end of the course, the student is able to: 1. Outline and explain the basic properties and physics of stars. Understand the electromagnetic spectrum, Black Body radiation, luminosity, effective temperature, flux and magnitudes, the Boltzmann and Saha equations, the spectral classification of stars, the HerzsprungRussel diagram. 2. Understand the concepts of hydrostatic equilibrium, the Virial Theorem, the Jean's criterion, freefall times and preMainSequence evolution. 3. Understand the concepts of radiative opacities, matterradiation interactions, different types of radiative opacities, specific intensities and radiative moments, the Radiative Transfer equation, Local Thermodynamic Equilibrium, the general solution of the RT equation, radiative equilibrium,radiative transfer at large optical depths, the Rosseland mean opacity. 4. Understand the radiative acceleration of matter, radiation pressure, the temperature profile in a Grey Atmosphere, line opacities (natural, Doppler and pressure broadening), Stimulated emission and Masers, Equivalent Widths, the formation of weak lines, Curve of Growth, atmospheric modelling. 5. Understand and apply the four equations of stellar structure, monochromatic radiative flux in stellar interiors, conduction, the general concept of convection, the Schwarzschild criterion for convection. Understand polytropic models, tthe structure of the Sun, the equations of state (ideal gas, degeneracy, radiation pressure). 6. Understand generalities and basic physics concerning nuclear fusion, the protonproton chains, CNO cycles, the lifetime on the Main Sequence, the Helium burning phase. Describe evolutionary tracks in the HRdiagram and the underlying physical principles at the root cause of evolution. Understand the differences and underlying physics for the evolution of lowmass, solarmass and massive stars. 7. Describe and explain the origin and nature of stellar remnants, White Dwarfs, neutron stars, pulsars and black holes. 

Omschrijving  The student will learn the basic properties and physics of stars, the basics of the star formation process, radiative transfer and plasma opacity, and the structure of stellar atmospheres and techniques to model them. The course introduces the equations of stellar structure and the concepts of convection, nuclear fusion and stellar evolution. It explains the HR diagram and discusses stellar remnants and the basics of star formation.  
Uren per week  
Onderwijsvorm 
Hoorcollege (LC), Opdracht (ASM), Practisch werk (PRC), Werkcollege (T)
(LC 30, T 24, ASM 12, 32 PRC, self study 42) 

Toetsvorm 
Opdracht (AST), Practisch werk (PR), Schriftelijk tentamen (WE), Tussentoets (IT)
(60% WE, 10 IT, 20% PR, 10% AST) 

Vaksoort  bachelor  
Coördinator  prof. dr. E. Tolstoy  
Docent(en)  prof. dr. E. Tolstoy  
Verplichte literatuur 


Entreevoorwaarden  The course unit assumes prior knowledge acquired from preceding BSc courses, in particular first and second year astronomy courses, programming, calculus and atomic physics.  
Opmerkingen  Final exam and computer model both require a mark >=4.5 to be compensated by midterm and homework marks. Mandatory presence at tutorials when homework assignments will be handed out and handed in. Not handing in one homework assignment results in the lowest mark obtained for the other 3 assignments. Not handing in 2 or more homework assignments will result in a mark 1 for each missed assignment. 

Opgenomen in 
