department of astronomy - courses  
home dept of astronomy mcdonald observatory research hobby-eberly telescope directory university of texas  
home
department of astronomy
mcdonald observatory
research
hobby-eberly telescope
directory
university of texas
 
 
AST 309L

Lectures

Links

Review

Course Schedule

Syllabus

Courses
Review for Test 1


AST. 309L - REVIEW OF CH. 1 - 3D
  1. Basics
    Typical dimensions in universe, common structures
    Definition of life - traditional (5 attributes) and more abstract
    Chemical composition of life, and relative to earth/universe
    The Drake Equation, metric system, absolute temp. scale
  2. Origin of atoms
    1. Before stars
      1. Elementary particles and the Big Bang
      2. Four fundamental forces - gravity, electromag., strong, weak
      3. Nuclei after 3 minutes (H 75%, He 25%), atoms after several x 100,000 yrs
      4. Galaxies and stars formed from gravitational instabilities
      5. Velocity of a particle in a gas, depends on T and m.
    2. Nuclear reactions in stars
      1. Potential energy diagrams
      2. Repulsion of like charges creates "barrier" to climb for nuclear strong force
      3. Conversion of mass into energy
      4. H into He via p-p cycle (later in more massive stars, CNO cycle)
      5. "Triple alpha" process makes C via route using unstable Be
      6. Adding another He nucleus makes O
      7. Heavy elements made at high T, in massive star centers; and SN (beyond iron)
  3. Origin of molecules and planets
    1. Chemical interactions (reactions)
      1. Potential energy diagrams; chemical bond = shared electrons, EM force
      2. Activation energy barrier, due to electron repulsion
      3. No energy barrier present for ion-molecule interactions
    2. Molecules and dust in space (dust is about 1% by mass, but important)
      1. Many molecules found in space, high % have carbon; C in long chains even
      2. Molecules found by radio emission from rotational energy changes
      3. Molecules and dust found together; PAH's are like large mol, or small dust
      4. Dust comes from old stars; both silicate and carbonaceous dust
      5. "Ice" mantles on grains where cold; possible chem. reactions
      6. Dust protects molecules from UV, provides site for making H2
      7. Molecular clouds, range of sizes and masses, produce stars
    3. Star formation - R(*)
      1. Rate calculated from # stars in galaxy and life of galaxy (corrections for stars that are already dead, and if rate not constant)
      2. Theory: inside collapses first, disk forms for more matter to accumulate
      3. Massive stars form and evolve much faster than low mass stars
      4. Disks inferred from bi-directional winds, from large amount of dust seen in infrared together with not-obscured stars, HST images
      5. Disks a natural consequence of angular momentum of parent cloud
      6. "Stars" that don't burn H are "brown dwarfs", more mass than planet
    4. Planet detection - f(p)
      1. Detection of planets very difficult, wobbling in space or velocity most likely detection methods; direct observation very difficult because of resolving power, infrared better than visible but still too hard
      2. Virtually all detected planets (~ 30) seen by periodic velocity change of star
      3. Properties of our solar system are consistent with disk formation model, so maybe many planets exist since we see so many disks
      4. Detected planets heavily influenced by detection method - massive and close to star







 





16 September 2006
Astronomy Program · The University of Texas at Austin · Austin, Texas 78712
prospective student inquiries: studentinfo@astro.as.utexas.edu
site comments: www@www.as.utexas.edu