1
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- Chapter 5: Just a few topics
- Telescope resolution
- Function of size, wavelength
- Observations at different wavelengths
- Electromagnetic Spectrum
- Telescopes in space (why)
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2
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- Chapter 6: Starlight and Atoms
- Model Atom, parts, energy levels
- Emission and Absorption Lines
- Blackbody Radiation
- Wien’s Law, Steffan-Boltzmann Law
- Spectra of Stars
- Balmer thermometer, spectral types (OBAFGKM)
- Doppler Effect
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3
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- Chapter 7: The Sun
- Atmospheric Structure
- Temperature, density, etc., with radius
- Sunspots/Magnetic Phenomena
- What are they? Why do they
exist?
- Nuclear Fusion – proton-proton chain
- What is it? How does it
produce energy?
- Solar Neutrino “Problem”
- What is it? Is it still a
problem?
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4
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- Chapter 7: The Sun – example question
- Q. The fusion process in the sun, the "proton-proton" chain,
requires high temperatures because:
- c of the
ground-state energy of the Hydrogen atom.
- c of the
presence of Helium atoms.
- c the colliding
protons need high energy to overcome the Coulomb barrier.
- c of the need
for low density.
- c the neutrinos
carry more energy away than the reaction produces.
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5
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- Problem from textbook:
- mV MV d (pc) P (arcsec)
- ___ 7 10 _______
- 11 ___ 1000 _______
- ___ -2 ____ 0.025
- 4 ___ ____ 0.040
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6
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- Problem #4:
- m MV d (pc) P (arcsec)
- 7 7 10 0.1
- 11 1 1000 0.001
- 1 -2 40 0.025
- 4 2 25 0.040
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7
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- Chapter 8: The Properties of Stars
- Distances to Stars
- Parallax and Parsecs
- Spectroscopic Parallax
- Intrinsic Brightness: Luminosity
- Luminosity, Radius, and Temperature
- Hertzsprung-Russell (H-R) Diagram
- Luminosity Classes (e.g., Main Sequence, giant)
- Masses of Stars
- Binary Stars and Kepler’s Law
- Mass-Luminosity Relationship
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8
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- Chapter 8: Properties of Stars—example question
- Q. A star’s luminosity depends only on the star’s:
- c distance and
diameter.
- c temperature
and distance.
- c distance.
- c temperature
and diameter.
- c apparent
magnitude
- Another version of the question can be made for apparent magnitude .
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