Introduction to Astrophysics
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1 Introduction to Astrophysics PHYS 4330 Fall 2017: offered in English ourse webpage: 1 ourse Information This course is aimed at building a solid foundation for science majors inclined to pursue research in astronomy related fields. Lectures in the first semester cover broad, considerable knowledge of modern astrophysics, including astronomical measurements, physical processes in celestial objects, dynamics in stellar systems, (the Solar system objects if time allows), etc. Students must have prerequisite skills in physics at undergraduate level unless otherwise approved by the instructor. 3 Instructor & GSI Instructor: Huei-Ru Vivien hen Office: nd General Building Office hour: Tuesday 10:30-11:30 Phone: (03) hchen@phys.nthu.edu.tw 2 Textbook & Reference Textbook An Introduction to Modern Astrophysics (2ed) Bradley W. arroll & Dale A. Ostile 2006 (Pearson Addison-Wesley) Website: 4 Graduate Student Instructor: Li-Wen Liao Office: nd General Building Office hour: Wednesday 16:00-17:00 liwen@gapp.nthu.edu.tw Reference The Physical Universe by Frank H. Shu 1982 (University Science Books)
2 More on Your Textbooks 5 ourse overage I 7 An Introduction to Modern Astrophysics (1st edition) 1996, Addison-Wesley cgs units Match research better, but Some chapters need further editing An Introduction to Modern Astrophysics (2nd edition) Tools of Astrophysics Overview elestial sphere and celestial mechanism Telescopes Basic measurements and nature of light Interaction of light and matter 2007, Addison-Wesley MKS units Match general public better, but bad for future reading of professional astronomy journals or articles Improved content arrangement with better figures Stars and Interstellar Medium Binary systems The classification of stellar spectra Stellar atmospheres Main-sequence stars & their interior structures Lectures and Grading Policy 6 ourse overage II 8 Time and Venue Tuesdays 14:20-17:20, nd General Building Lecture arrangement Offered in, but not limited to, English Stellar evolution Interstellar medium & star formation Main sequence and post-main-sequence stars Pulsating stars The fate of massive stars 14 lectures in total lass cancelled on October 3 and 17 National holidays: October 10 Final examination on January 9 th, 2018 Grading Policy 60% problem sets (due 5PM of the following Thursday) 30% final exam 10% attendance
3 9 Lots and Lots of Math But before we start, let s have a chat. (Oh, yeah, we mean it.) Astronomy? Astrology? Welcome to Introduction to Astrophysics. Before we start, are there any questions? 10 redit: Evad Damast 12 Yeah, like, what makes astronomy different from astrology? (And your thoughts?) But not just math, Astronomy is Art!
4 Astronomy is Passive Science 13 oordinate Systems 15 We observe, observe, and observe. Then we come to understand what it is all about in Nature. How to register stars on the sky? Sometimes, exciting predictions are also out there. How do we know where to find what? How do we register ourselves in the Universe? 14 elestial Mechanics 16 More on the lass ontents Kepler s laws (1609) Gelilo (1610, 1632) Father of modern observational astronomy Newton s laws of motion (1687) Tools of Astrophysics Stars and Interstellar Medium Stellar Evolution The Virial theorem: dynamics in a relaxed system
5 Spectrum of Light Above the louds Seeing through the Atmosphere 18 Telescopes 20 Wavebands that are unaccessible on the ground Far-infrared (FIR) Mid-infrared (MIR) Ultraviolet (UV) X-ray Gamma-ray VLBA UKIRT Hawaii 2.2m Gemini North JMT SO FHT SMA Keck NASA IRTF
6 21 Space Observatories Binary Systems 23 Important for deriving stellar parameters Interaction of Light & Matter How to form spectrum? What can we learn in the Solar spectrum? How about stellar spectra?
7 Main-Sequence Stars 25 Stellar Evolution 27 lassification of stellar spectra Stellar atmosphere & radiative transfer Interiors of stars The Sun lassification of Stars 26 Interstellar Medium 28 Hertzsprung-Russell Diagram (HR Diagram) redit: David De Martin Strong UV radiation I 1805 creating H II regions filled with ionized gas I 1848 H I = H H II = H + = p
8 29 Star Formation Planetary Nebulae Stellar explosions Planetary nebula Supernova remanent 30 Standard Paradigm Infall envelope Bipolar jet/outflow Accretion disk Infall envelope 32 Supernova Remanent Stellar explosions Planetary nebula Supernova remanent 31
9 33 Star lusters and Ages Globular clusters Population II, old stars, gravitationally bound, virialized M13 (globular cluster) Pleiades (open cluster) Eta arinae M 120 M The only star known to exhibit lasers in the UV 34 Pulsating Stars - epheids redit: Jeffrey Newman (U Berkeley) & NASA Population I, young stars, gravitationally unbound Extremely Massive Stars Open clusters 35
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