Chap. 1
pp. 1-7

Ch. 2
pp. 30, 32

Chap. 1
pp. 7-end

[2] • Galaxy Song -- Monty Python      video version
      How fast are you moving when you are sitting still? Astro Soc of Pacific Newsletter.
  MW "image", simple diagram, labeled str, named spiral arms, Local group diagram, Virgo cl (#6), overview of structures.
Structure of galaxy clusters Geller & Huchra; 2dF slice.
nasa cosmology, model of cluster str (3d rotn).

What a light-year is. Finish position tutorial for WED.

• MA website: interactive figure 19.1 view of MW
     large scale str in univ 22.14
• Calculating Scale Models.

• Star-galaxy scale model worksheet

Path of object that rises in the east.
  circumpolar long image, medium length, shorter image [10,40]
  star trail images large not orion dipper trail
  large orion (apod 2/7/03) (10)

Quiz 1: fists/fingers measurements and calculations, tutorial 1
•Finish Star-galaxy scale model worksheet

[3] • Celestial Sphere: Strobel's Astro Notes, [another "text"].
• Tutorial 2 worksheet

• Telling time: solar, standard, daylight saving, UT.
• Seasons, seasonal stars, signs of the zodiac and astrology.
• Tutorial 2 worksheet (con't)
• Tutorials 3/4 worksheet

[4] Sidereal and Synodic month animation.
Seasons and eclipses.

Angles in degrees, minutes, seconds
Light, color, spectra intro.
Light, color -- why things are the colors they are, how filters work.
• The electromagnetic spectrum (or here): how the wave and particle properties interact.
   Energy of a photon = hc/λ = 1240 eV·nm / λ
         where 1 nanometer = 1 x 10^-9 m

EM Spectrum,
  pp. 45-47

How colors work -- filters transmit and opaque materials "reflect" (specular vs. diffuse)

Relation between size, temperature, and luminosity for a blackbody:
    power per square meter = "sigma" * (temperature)^4 = σT⁴
    Luminosity = "sigma"*(temperature)^4 *(surface area of star)
  **      L = σT⁴ * 4πR²

Temperature and color relation
•blackbody applet -- drag temp, see graph change
• another blackbody applet -- enter temp, see plot

Relation between color (wavelength) and temperature:
   Blackbody Radiation

Luminosity, temperature, & Size
  pp. 53-56

Measure the Luminosity of the Sun using the "Inverse square law"
  (brightness ratio) = (distance ratio)^2

Luminosity, temperature, & Size
  pp. 53-56

[5] Returned and went over:
• Tutorial 2 worksheet
• S&T Almanac worksheet
• Luminosity of the Sun worksheet

H-R Diagram image.

Relation between color (wavelength) and temperature: blackbody radiation con't
    lambda_max = λ_max = wavelength at which blackbody curve is maximum
    λ_max * T = 2.9 x 10⁶ nm·K

Blackbody Radiation
  pp. 57-60

Spectra: Examples from Dr. Richmond
Neon spectrum (others linked).
Daylight and bulbs -- from Ioannis Galidakis 1
• How spectra work:
electron in Bohr model as wave and particle applet
Hands-On Atom -- no longer available there, but archived here!

MA website: interactive figure 5.15

[6] Test 1   Details here.

Showed spectra in class (H and Ne)
Used spectrometers to measure Fraunhofer lines in the spectrum of the Sun

Types of spectra
  pp. 61-62

[7] Magnitudes
  L1 / L2 = 100^[(M2 - M1) / 5 ]

Magnitudes (apparent, m, and Absolute, M)
Magnitudes and Distance worksheet

Analyzing Spectra
  pp. 69-72

[Apparent & Absolute Magnitudes
  pp. 67-68]

Review what we find out about stars from their light:
• types of spectra --> continuum, emission line (bright lines), absorption line (dark lines), combinations
• color --> temperature
• lines --> composition
• line width --> see below

Doppler Effect    Δλ/λ = v/c
    • redshift [=z] when moving away;
    • blueshift when moving toward
Doppler identifies spectroscopic binary stars.
Line Profile/Broadening
  • rotation of stars
  • thermal broadening
  • density in stellar atmosphere

The Parsec, p. 35
    and
Parallax and Distance

Parallax and distances
      d (in parsecs) = 1 / [p (in arc sec)]
      1 pc = 3.26 lt-yr

Quiz     light, EM spectrum, luminosity & size, temperature and blackbody curves, types of spectra

[8] Types of binary stars:
• optical doubles are not binary -- they just line up in the sky
• visual doubles -- we see the second star and/or its effect
• spectroscopic binary -- we see the spectral line(s) shift due to the Doppler effect   [applet]
•eclipsing binary -- a special case of the above.   [applet]

Moon Phase models ...

Test 2, Thurs, 23 Oct 08     Details here.

[9] Binary stars: ** masses ** from Kepler's 3rd law:
        (M1 + M2)P² = A³
binary star simulations fr HW:   general        eclipsing

How we know what we knew to create the H-R Diagram
 especially distances via parallax
MA website: interactive figure 15.3 (parallax & blinking)

The Sun -- How it produces energy and Einstein's famous equation
Fission of U235 applet
MA website: interactive figure 14.7 fusion animation
  p-p cycle net effect: 4H --> He⁴ + stuff + energy
Einstein figured out where the energy of the sun comes from:
  E = mc²   mass of 4H > mass of He-4
MA website: interactive figure 14.3 interior of sun

Life of Sun on MS when
      4H --> He⁴ + stuff + energy
hot gas supports sun against gravitaional collapse (balloon and liquid nitrogen)
H-R Diagram ...
 • luminosity classes
 • mass-luminosity relation (glow stick in ice water and boiling water)
Story of the life of the Sun I.
 Collapse of nebula (= cloud of gas and dust)
Types of Nebulae:
• cold, dark
• emission = hot and bright (red/pink due to hydrogen emission)
• reflection = reflect light of nearby star (blue)

H-R Diagram ...
MA website: interactive figure 15.4 stellar luminosity function; 15.10 HR
 • spectroscopic parallax

[Doppler Shift, p. 73]

Spectroscopic Parallax, p. 43

[10] Stellar evolution movies from the Digital Demo Room
  MA website: interactive figure 14.8 neg feedback -> equil.
      preMS evol 16.15
     death of sun Fig. 17.4
End states of stars -- summary chart

Quiz 3 -- Moon Phase Cause worksheet/tutorial, identifying types of nebulae, and sun hemispheres.

MA website: interactive figure 17.12 Death of high mass star
   Crab nebula at various wavelengths 17.17
   Time dilation near BH 18.13, 18.13 evol of BH
   Binary star movie parts 3 & 4.
Star Clusters and ages: interactive fig 19.2 -- where clusters are located in MW