Study Guide for Exam 3
Chapter 5B -Light, and Atoms
Be able to define:
wavelength
visible light
ultraviolet radiation
infrared ratiation
electromagnetic radiation
speed of light
photon
diffraction
spectrum
temperature
absolute temperature scale
kelvins
thermal radiation
reflected radiation
Wien’s law
emission
energy levels
emission lines
ground state
excited state
absorption line
Be able to:
- list the names of the types of Electromagnetic radiation in order of wavelength
- the basic components of the atom and describe our modern conception of its structure.
- discuss the nature of electromagnetic radiation, and tell how that
radiation transfers energy and information through interstellar space
- explain how we can determine an object's temperature by observing
the radiation it emits
- explain why do scientists use Kelvins
- explain the differences between thermal radiation and reflected radiation
- state Wien’s Law in connection with the colors of stars
- describe the characteristics of continuous, emission, and absorption spectra, and the conditions under which each is produced
- explain how electron transitions within atoms produce unique
emission and absorption spectra
- explain how an electron gets from the ground state to an excited state
Chapter 6 - Family of Stars
Be able to define:
stars
light-year
parsec
apparent magnitude
absolute magnitude
luminosity
clases of stars
H-R diagram
main-sequence stars
giant stars
supergiant start
white dwarf stars
mass-luminosity relation
Stefan-Boltzmann law
Doppler effect
blueshift
redshift
Spectroscopic Parallax
Main Sequence Fitting
binary star system
multiple star system
optical double stars
visual inary
spectroscopic binary
eclipsing binary
light curves
Be able to:
- explain how stellar distances are determined.
- discuss stellar motion and how this motion is measured from Earth.
- explain how physical laws are used to estimate stellar sizes.
- distinguish between luminosity and absolute brightness, and explain how stellar
luminosity is determined.
- explain the usefulness of classifying stars according to their colors, surface
temperatures, and spectral characteristics.
- describe how an H-R diagram is constructed and used to identify stellar properties.
- explain how stellar masses are measured and how mass is related to other stellar properties.
- explain how spectroscopic parallax is determined
- explain how Main Sequence Fitting
is determined
- explain how the formation of a star is affected by its mass.
Chapter 7 - Stellar Evolution - Birth & Middle Age
Be able to define:
protostar stage
theory of star formation
gravitational contraction
protostar
brown dwarfs
T Tauri stars
red giant
helium flash
Zero age main sequence stars
HI regions
HII regions
Be able to:
- summarize the composition and physical properties of the interstellar medium.
- describe the characteristics of emission nebulae, and explain their significance in the life cycle of stars.
- discuss the nature of dark interstellar clouds.
- specify the radio techniques used to probe the nature of interstellar matter.
- importance of the 21 cm line
- explain why stars evolve off the main sequence.
Chapter 8 - Stellar Evolution II: Death of Stars
Be able to define:
variable star
Cepheid variable
supergiants
planetary nebulae
degenerate matter
Chandrasekhar Limit
supernova
core collapse
supernova remnant
neutron star
pulsars
special theory of relativity
general theory of relativity
event horizon
Schwarzschild radius
accretion disk
nova
type I supernova
type II supernova
Be able to:
- summarize the evolutionary stages followed by a Sun-like star once it leaves
the main sequence and describe the resulting remnant.
- explain how white dwarfs in binary-star systems can become explosively active.
- contrast the evolutionary histories of high-mass and low-mass stars.
- describe the two types of supernovae and explain how each is produced.
- explain the origin of elements heavier than helium and discuss the significance
of these elements for the study of stellar evolution.
- discuss the observations that help verify the theory of stellar evolution.
- describe the properties of neutron stars and explain how these strange objects
are formed.
- explain the nature and origin of pulsars, and account for their characteristic
radiation.
- list and explain some of the observable properties of neutron-stars.
- describe how black holes are formed and discuss their effects on matter and
radiation in their vicinity.
- relate the phenomena that occur near black holes to the warping of space around
them.
- discuss some of the ways in which the presence of a black hole might be detected.
Chapter 9 - Milky Way Galaxy
Be able to define:
Milky Way
Milky Way Galaxy
Galactic Disk
Galactic Bulge
Galactic Center
Open or Galactic Cluster
Globular Cluster
Population I Stars
Population II Stars
Be able to:
- List the major parts of our galaxy, what is found in each part, and and know where they are located.
- Describe the shape and size of the Milky Way Galaxy
- Define the Sun's position in the Milky Way.
- Explain the differences between a Galactic Cluster and a Globular Cluster
- Explain the differences between a Population I and a Population II stars by location and age..
Chapter 10 - Galaxies
Be able to define:
Elliptical Galaxies
Disk Shaped Galaxies
Irregular Galaxies
Parallax
Spectroscopic Parallax
Main Sequence Fitting
Cepheid Variable as distance indicator
type I supernova as a distance indicator
local group
Be able to:
- Explain the differences between the 3 major types of galaxies
- Review the Geometric and Standard Candle methods of determing astronomical diatances
- Explain how the Period-Luminosity Relation is used to determining distances within our galaxy.
- Why is a Type I supernova used instead of a Type II for distance determination?
Chapter 11 - Cosmology
Be able to define: (some of these may be in other chapters)
expanding universe
Hubble's Law
redshift of galaxies
cosmological redshifts
Local Group
Magellanic clouds
dwarf galaxies
Andromeda galaxy
cosmology
isotropic
cosmological principle
open universe
critical density
flat universe
closed universe
big bang model
Penzias and Wilson
cosmic background radiation
matter-dominated
supercluster
Local Supercluster
gravitational lensing
grand unified theories
quasars
Maarten Schmidt
properties of quasars
dark matter
dark energy
Be able to:
- state the cosmological principle and explain its significance.
- explain how the age of the universe is determined and discuss the uncertainties involve.
- summarize the leading evolutionary models of the universe and discuss the factors that determine whether or not the universe will expand forever.
- describe the cosmic microwave background radiation and explain its importance to our understanding of cosmology.