PHYS466
Test No.1 Review, Spring 2011
SUBJECT MATTER:
Class notes through Feb. 28.
on Chaps. 1 thru 3-4C, equation (3-26). The test does
not include the Saha equation.
All homework problems through
#58.
Photometry and the magnitude
system.
The modern magnitude scale:
How defined and general relationship:
Difference in magnitude = 2.5 log (brightness ratio).
Combined magnitudes.
Intensity and Flux (monochromatic
and polychromatic)
Trignometric parallax method
of distance determination.
Abdsolute magnitude and Luminosity.
Distance units: AU, ly,
and parsec.
The H-R Diagram
Laws of radiation: Stefan-Boltzmann
Law, Wien's Law, and Planck's Law. Planckian or
Black Body radiation curves.
Kirchhoff' Laws of spectroscopy
(Three kinds of spectra).
Determining Stellar Temperatures.
Color magnitudes.
Color indices and relation
to temperature.
Bohr Atom and energy levels
Bohr' Equation: En=
2(pi)2mZ2e4/n2h2.=-13.6/n2
for hydrogen.
Balmer Formula (for wavelengths
of lines in a series)
The different spectral line
series for hydrogen. Grotrian Diagram.
Modes of excitation and
ionization.
Kinetic Theory: 0.5mv2
=3kT/2, concept of kinetic temperature.
Maxwell-Boltzmann velocity
distribution function for temperature T.
The 3 different speed statistics.
Thermal Excitation Equilibrium
and the Boltzmann Equation.
Partition Function
Thermal Ionization; Saha
Equation
Combined Boltzmann and Saha
equations.
Spectral classes and luminosity
classes and loci in HR-Diagram
Stellar spectra and the
production of absorption lines.
KNOW:
Definition and properties of:
apparent brightness, intrinsic brightness,
intensity, flux, surface brightness,
luminosity, absolute magnitude,
color magnitude, color index,
& distance modulus.
What intrinsic brigtness
depends on.
Thermodynamic meaning of
absolute temperature.
Difference between scattering,
reflection, and thermal emission.
Stefan-Boltzmann Law; Wien
Displacement. Incandescence.
Meaning and use of Planck's
Black-Body Law for monochromatic intensity.
How luminosities may be calculated;
how parallaxes are found;
how absolute
magnitudes are found.
Know the derivation of monochromatic
surface flux from monochromatic intensity.
How stellar spectra depart
from Black-Body spectra and what causes this.
How B-V values are related
to surface temperature.
Equations
to memorize:
(1-1),
(1-9), (1-10), (1-12), (1-14), (1-17), (1-19), (1-21), (1-23), (1-23),
(1-24)
(2-12),
(2-13), (2-51), (2-52)
(3-11),
(3-16)
(4-1),
(4-3), (4-8), (4-9).
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