SYLLABUS for course ASTB23, Title: Stars, Galaxies & the Universe Fall 2023. Please download updated syllabus ~every week. ___________________________________________________________________________________ Lectures: Thursdays 12-14 HW408. Tutorials: Thu 17-18 SW311. Calendar od lectures (L1...L24) and tutorials (T1...T10). A1..A4 are due dates to submit assignments 1..4 on Quercus/Assignments **by noon** ___________________________________________________________________________________ 7 Sep L1 + L2, -- (no tutorial) 14 Sep L3 + L4, T1 21 Sep L5 + L6, T2 28 Sep L7 + L8, T3 A1 5 Oct L9 + L10, T4 12 - no meetings, reading week 19 Oct L11 + L12, T5 A2 26 Oct L13 + L14, T6 <-- in-class midterm during T6 2 Nov L15 + L16, T7 9 Nov L17 + L18, -- 16 Nov L19 + L20, T8 A3 (drop&remove course from transcr.< 20 Nov) 23 Nov L21 + L22, T9 30 Nov L23 + L24, T10 A4 19 Dec (Tue) 14:00-17:00 in HW214 <--- final exam [8 hand-written pages on 4 or 8 sheets (not printed or photocopied) of your own notes are allowed at midterm; total of 8 pages allowed during final exam. Calculators are required. Books, phones, electronic devices not allowed.] ___________________________________________________________________________________ Office hours: an hour or so right after lectures. Contact: marker TA: Abdur (abdu.khan AT mail.utoronto.ca) or the lecturer pawel.artymowicz AT utoronto.ca [subject line ASTB23 required. Use your utor mail not gmail or facebook] Note: URL of updated syllabus http://planets.utsc.utoronto.ca/~pawel/ASTB23 Topic number below does not in general coincide with lecture number. Symbols ##### in first column below area a pointer to "where we've stopped" during the latest lecture. Symbols ^^^^^ show to which place it's recommended to read ahead. See course web page for textbooks. After midterm the posted PDF lecture notes will be more useful than textbooks. The relevant chapters/sections of the textbook #3 are indicated as, for instance, Chapter 5.1, => [5.1], while [L10] would indicate Lecture10 in PDF/PPT form. ................................................................................ 0. Organization and goals of the course 1. Introduction to stellar (and planetary) astrophysics [L1] * Comments on the history of the idea of other stars and planets 2. The Present Revolution in Astronomy: An Overview [1-Unnumbered] From p. xvii of textbook 1. PLEASE READ - it's a very good overview, we skip most of it during the lecture as it is a bit long, but you should read the whole 150+ page textbook, and one or two questions from this overview may be asked in midterm/final quiz, for ex. about Hubble law. [Until the midterm, we will follow closely textbook 1 "What are the stars"] 1. What are the Stars? * Historical Introduction * The Photosphere * The Interior of the Sun * The Virial Theorem 2. Stars as Globes of Gas * A Theory of the Stars * Hydrostatic Equilibrium * Why Does the Sun Shine? * Source of Energy 3. Eddington’s Theory of the Stars * Radiation Pressure * Radiative Equilibrium * Basic Equations of Stellar Structure * Solution of the Equations of Stellar Structure * Eddington’s Mass–Luminosity Relation * The Eddington Luminosity Limit 5. Energy Generation in the Stars * The Hypothesis of Nuclear Fusion in the Stars * The Basic Difficulty * Tunnelling Through a Potential Barrier * The Neutron and the Neutrino * The Synthesis of Helium in the Stars * Why Does the Sun Not Blow Itself Up? 6. Sounds of the Sun * The Standard Model of the Sun * The Phenomenon of Convection * Sounds of the Sun * Nodes, Nodal Lines and Nodal Surfaces * Vibrating Spheres * Helioseismology * The Antarctic * The Standard Model Put to Test * Rotation of the Sun from Helioseismology 7. The Smoking Gun is Finally Found * The Hunt for the Smoking Gun * The Kamiokande II Experiment & The Atmospheric Neutrinos * The Sudbury Neutrino Observatory * Neutrinos Do Oscillate in Flavour from Book 2 by Srinivasan "Life and Death of Stars" 8. (ch. 2) Stars in Their Youth * H-R diagram 15 (i.e. page 15) * Energy Generation in the Main Sequence 17 * Convection in Stars 20 * The Lifetime of Stars 21 * The Ultimate Fate of the Stars 23 9. (ch. 3) White Dwarf Stars 25 * The Strange Companion of Sirius 26 * Gravitational Redshift 27 * A Stellar Paradox: Have Stars Enough E to Cool? 10. (ch. 5) Fermi–Dirac Distribution 55 * Pauli’s Exclusion Principle 55 * The Fermi–Dirac Distribution 56 * Pressure laws of the Degenerate Electron Gas 58 * Fermi Momentum 60 11. (ch. 6) Quantum Stars 67 * Fowler and Chandra 67 * Chandrasekhar’s Theory of the White Dwarfs 71 * All Stars will Ultimately Find Peace 77 12. (ch. 7) The Chandrasekhar Limit 79 * Relativistic Stars 79 * Chandrasekhar limit 84 * Can All Stars Find Peace? 90 [ Start looking at the lecture notes from now on since they are the main source from now on! ] You may also read a book by Sparke & Gallagher "Galaxies in the Universe" to supplement the lectures and lecture notes, but ut's not required. 13. Formation of disks and stars * Giant molecular clouds * Jeans instability of protostellar cloud cores * Opacity-limited fragmentation * Simulations: the ubiquity of protostellar disks, brown dwarfs * Accretion disks [9] * AGN and quasars: accretion onto `black' holes * Accretion disk geometry * Disks as evolving, shearing flows * Collapse simulations using SPH (smoothed particle hydrodynamics) read Lecture notes 13-14 14. Introduction, The Milky Way [1] [1.a] History of the discovery of the Galaxy [1.b] The Great Debate about galaxies [1.2] Our Milky Way 15. [1.3] Other galaxies, Galaxy photometry Hubble sequence, other classifications [1.4] Galaxies Typical properties and statistics of of galaxies Gauss theorem and examples of its use. Laplace equation Gravity force and potential Spherical systems & Newton's theorems Potentials of some simple systems Potential- density pairs of flattened systems 16. [2] Mapping our Milky Way [2.1] The solar neighborhood 2.2 The stars in the Galaxy The vertical structure of the disk / Distances to star clusters / Bottliger diagram, asymmetric drift 17. [2.3] Galactic rotation Infrared & radio view of the Milky Way Glactic bulge and Center (Nucleus) Measuring the Galactic rotation curve 18. Relaxation and evolution, part I [3] The orbits of stars [3.2] Why the Galaxy isn't bumpy: two-body relaxation, encounters Relaxation time: theory and the inferred histogram for globular clusters 19. Relaxation and evolution, part II ###### we stopped here in L21 on 23 Nov The virial theorem / Evaporation / mass segregation Effects of two-body relaxation: core collapse of globular clusters [3.x] Angular momentum and energy conservation in stellar motion Epicyclic theory of orbits in galactic potentials epicyclic frequecy, vertical frequency, azimuthal frequency and the corresponding periods 20. [4] Our backyard: the Local Group [4.2] Spirals of the Local Group The Andromeda galaxy / M33: a late-type spiral [5] Spiral and S0 galaxies [5.3] Gas motions and the masses of disk galaxies 21. Rotation Curves and Spiral Arms in Galaxies Decomposition of rotation curves. Two types of rotation curves. Dark matter in disk galaxies The Tully-Fisher versus the Faber-Jackson relationship [5.4] Spiral arms and galactic bars Observed spiral patterns: trailing vs. leading spirals Disk Dynamics and Spiral Structure Dispersion relation for gaseous disks Long waves / Short waves / Toomre stability of disks SWING amplifier Lin-Shu theory of spiral modes and WASER cycle Correlation of rotation curve with the type of spiral pattern: physical explanation of spiral galaxy classification ^^^^^^^ 22. Bars as a by-product of spiral mode evolution Encounters and mergers between galaxies Gravitational lensing [We didn't study in 2023: 23. [6] Elliptical galaxies [6.2] Motions of the stars The Faber-Jackson vs. Tully-Fisher relations [6.5] Galaxy clusters: the domain of elliptical galaxies Elliptical galaxies: nature, nurture, or merger? [8]Supermassive Black Holes and Active Galactic Nuclei Early history of galaxies Instead, we have learned in L23 the history and diverse evidence of Dark Matter in the universe (evidence from rotoation curves and stability of gala, galactic pairs and clusters, grav. lensing) ] 24. The Universe [7] Large-scale distribution of galaxies [7.1] Observations of large-scale structure: galaxy clustering [7.2] Expansion of a homogeneous Universe [7.3] Growth of structure: peculiar motions clusters, walls, and voids [8.3] Cosmic Microwave Background Radiation (CMBR) Historical microwave Holmdale antenna discovery Modern satellite observatories First observational proof of a flat spacetime in our universe: Boomerag and WMAP experiments The universe in 21st century: Einstein's cosmological constant Lambda returns (Dark Energy)