Materials for PHYS2160 Part 1 - 2015

 
 

  1. •Combined Notes for all of Part I (162Mb) - PHYS2160 Notes Combined.pdf

  2. •Lecture 1 - PHYS2160 Notes 1.pdf

  3. •Shu - The Physical Universe, Chapter 12 on Google Books.

  4. •Lecture 2 - PHYS2160 Notes 2.pdf

  5. •Galactic Centre Movies - 1992-1995, 1995-2013

  6. •Very Cool 3D animation of the Galactic Centre stars

  7. •Lecture 3 -PHYS2160 Notes 3.pdf

  8. •Lecture 4 - PHYS2160 Notes 4.pdf

  9. •PHYS2160 Tutorial problems - Part I.pdf

  10. •Shu Chapter 11 on Google Books

  11. •Bate et al Star Formation Simulation

  12. •Transit Planet Animation

  13. •Link to Radial Velocity Simulator

  14. •Lecture 5 - PHYS2160 Notes 5.pdf

  15. •Milky Way CO maps (Dame et al.) from
            http://www.cfa.harvard.edu/mmw/MilkyWayinMolClouds.html -
            Emission Intensity Map, Velocity Position Diagram

  16. •Lecture 6 - PHYS2160 Notes 6.pdf

  17. •Hubble Ultra Deep Field – images available at many locations on web. Image used in class came from an ESA site - http://www.spacetelescope.org/images/heic0611b/. Or download Hubble_UDF_heic0611b.jpg

  18. •The Sloan Digital Sky Survey site has an excellent discussion of the characteristics and classification of galaxies, with many lovely images from their large survey of the Northern sky (http://skyserver.sdss.org/dr1/en/proj/advanced/galaxies/tuningfork.asp)

  19. •Movies on spiral arms used in class are from http://en.wikipedia.org/wiki/Density_wave_theory)

  20. •http://commons.wikimedia.org/wiki/File:Galaxy_rotation_rigid.ogv
    Galaxy_rotation_rigid.ogv.360p..mov

  21. •http://commons.wikimedia.org/wiki/File:Galaxy_rotation_wind.ogv
    Galaxy_rotation_wind.ogv.360p..mov

  22. •http://commons.wikimedia.org/wiki/File:Galaxy_rotation_wave.ogv
    Galaxy_rotation_wave.ogv.360p..mov

 

Materials

  1. •Links on this page will be activated as the course progresses. I will endeavour to ave them active one week in advance of the lectures. In particular the combined lecture notes PDF will not be activated until near the end of the 6 weeks of this first half of the course.


  1. •Lecture 7 - PHYS2160 Notes 7.pdf

  2. •Lecture 8 - PHYS2160 Notes 8.pdf

  3. •Lecture 9 - PHYS2160 Notes 9.pdf

  4. •Lecture 10 - PHYS2160 Notes 10.pdf

  5. •Freedman (2013) "The cosmic distance scale and H0: Past, present, and future"
    http://dx.doi.org/10.1017/S1743921312021047  or Freedman et al. 2013 H0.pdf

  6. •Freedman & Madore (2010) "The Hubble Constant"

  7. •Freedman et al. 2001 - 0012376v1.pdf

  8. •Lecture 11 - PHYS2160 Notes 11.pdf

  9. •Brian Schmidt Nobel Lecture

  10. •Adam Reiss' Nobel Lecture


  1. •In-Class Exam - Wed September 2

  2. •PHYS2160 Mid-Term 2015 Solns.pdf

  3. •PHYS2160 Tutorial problems - Part I.pdf

  4. •PHYS2160 Assignment - Part I.pdf

  5. •PHYS2160_2015_Ass_1_Solns.pdf = CGT: Updated 2 Sep to fix error in Q3),d),ii)

  6. •PHYS2160 More Tutorial problems - Part I.pdf



  1. •General Rules for Assignments

  2. •Please show your working. If you make an error, I can give partial credit if you show your thought process. If you just have an incorrect answer, I can't.

  3. •Use words to define symbols being used and to explain your thought processes.

  4. •Assignments may be submitted in handwritten format - as long as I can read them!  If I can't read it I can't assess it.

  5. •If you need a figure to explain your work, then you must draw it yourself (either by hand or electronically). You may not cut-and-paste figures or text from the lecture notes or other sources. To do so with attribution is pointless, and to do so without attribution is plagiarism.

  6. •In accordance with UNSW policy, the assignments handed in should be your own work.



Above left - solid body rotation looks like a spiral galaxy, but we know it is unphysical.


Above right - if the arms move with the rotation kinematics known for stars, then they will rapidly "wind-up" and become so scrambled they will vanish.


Lower right - for the pattern to persist, it must move at a different velocity to the stars, i.e. it propagates as a wave.


Source: Wikipedia commons