ASTRONOMY 110 - UNIT 3
Chapters 8 - 14
Learning Goals and Outcomes
Be able to describe the scientific tools and processes used to understand our
place in the cosmos
Be able to describe fundamental properties and characteristics of stars and
stellar evolution
Be able to describe our understanding of the formation and evolution of the largescale universe and the interactions of objects within it
Explain the processes of nuclear fission and fusion
Describe the major features of the Sun, including the sunspot cycle
Describe the various methods for determining distances to stars and galaxies and the
cosmic distance ladder
Explain how the H-R diagram is used as an astronomical tool for determining various
properties and characteristics of stars
Explain the role nuclear fusion plays in stellar evolution
Describe the life cycles of stars and explain the difference between white dwarfs, neutron
stars, and black holes
Describe the major features and properties of the Milky Way Galaxy
Describe the large-scale structure of the universe
Explain the major features of the Big Bang Theory and the observations that provide
support to this theory on the origin of the Universe
Describe the current theories on the evolution of the Universe and explain the role dark
matter and dark energy play in the evolution and fate of the Universe
Major topics and key concepts covered to meet learning goals and outcomes
NUCLEAR ENERGY
atomic structure
protons (chemical identity and atomic number)
relative abundance of the elements in the universe
nuclear energy
fission
fusion
E = mc2 (equivalence of mass and energy; conversion of mass into energy)
energy released by fission and fusion
significance of iron in the nuclear energy process
ASTRONOMY 110 - UNIT 3
Chapters 8 - 14
THE SUN AND SOLAR ACTIVITY
solar activity and surface features of the Sun
granulation (convective cells)
prominences (relationship to sunspots)
solar flares
sunspots
characteristics of sunspots
the sunspot cycle (sunspot numbers and the magnetic cycle)
coronal mass ejections
structure of the Sun
nuclear burning core
radiation zone
convection zone
gravitational equilibrium
PROPERTIES OF STARS AND MEASURING COSMIC DISTANCES
distance measurements to stars
the parallax method (for nearby stars) - understand how this is used
parsecs (1 parsec = 3.26 light-years)
distance limitations (when this method no longer works)
apparent brightness (factors affecting the apparent brightness of stars)
luminosity
distance
other methods of distance determination
using the inverse-square law for light to get distance
variable stars (light curves)
distance limitations (when this method no longer works)
Stellar Classification
the H-R Diagram (stellar properties, characteristics, and evolution)
Main Sequence stars
Red Giants
Supergiants
White Dwarfs
the H-R Diagram as a tool (determining distance, age, size, mass, lifespan,
evolutionary stages)
using spectra and the H-R diagram for distance measurements to stars
spectroscopic parallax/Main-Sequence fitting
distance limitations (when this method no longer works)
determining the ages of stars
star clusters
Main-Sequence turnoff point (used to determine the age of stars in a cluster)
ASTRONOMY 110 - UNIT 3
Chapters 8 - 14
determining the masses of stars
Main-Sequence stars (H-R Diagram) - where the least/most massive stars are found
binary star systems (determining mass from orbital characteristics)
using Kepler's 3rd Law (orbital distance and orbital period)
the Cosmic Distance Ladder - summary of methods for distance determination
trigonometric parallax
the inverse-square law for light
spectroscopic parallax/Main-Sequence fitting
variable stars
standard candles - galaxies and supernovae
the Hubble Law
STELLAR EVOLUTION
stellar evolution driven by gravity
mass is the most important characteristic in a star's life cycle
formation of stars from nebulae
interstellar shock waves
gravitational collapse
protostars
Main-Sequence lifetime
hydrogen burning (fusion) -- gravitational equilibrium
changes in a star when hydrogen fuel in the core is depleted
collapse of inert helium core
expansion of the star's surface
Red Giant stage
helium burning (fusion)
core temperature for helium burning
depletion of helium and formation of carbon core
evolutionary pathways
low-mass stars (helium fusion to inert carbon core)
collapse of carbon core produces planetary nebula
formation of white dwarfs ("degeneracy" of the core)
intermediate and high-mass stars (nuclear fusion, produces carbon and oxygen cores)
nuclear fusion of heavy elements
formation of inert iron core
gravitational collapse and the formation of supernovae
neutron stars and pulsars
neutron "degeneracy"
black holes
singularities
the event horizon
ASTRONOMY 110 - UNIT 3
Chapters 8 - 14
GALAXIES AND STRUCTURE OF THE UNIVERSE
Milky Way galaxy
structure
nucleus, disk, and halo
spiral arms, globular clusters
how globular clusters are used to determine our position in, and the size of our
galaxy
size of the Milky Way galaxy
location of the Sun within the Milky Way galaxy
orbital period of the Sun around the galaxy
Population I and Population II stars
characteristics of each type
determining the number of stars in our galaxy
orbits of stars in the Milky Way Galaxy
rotation curves
dark matter
distribution of galaxies in the universe
the local group
clusters and superclusters
types of galaxies
spiral galaxies
elliptical galaxies
irregular galaxies
galactic collisions
COSMOLOGY AND EVOLUTION OF THE UNIVERSE
Hubble's observations
the expanding universe
cosmological red shift
The Hubble Law
distance measurements
age of the universe (the Hubble constant)
the big bang theory (the birth of the universe)
evolution of the universe
the cosmic microwave background radiation
ordinary matter, dark matter, dark energy, and the future of the universe
relative abundances of each type in the universe