Physics 303—The
Universe in Ten Weeks—Spring 2006
Midterm Review Sheet
The midterm will cover material from Ch 1, Ch2 (Section 1 only), Ch S2, Ch S4, Ch 14 (Sections 1 and 2), and Chapter 15.
Bring a calculator.
You may bring one sheet (8 ½ x 11, both sides) of any notes you like.
No need to bring scantron form or paper; all answers will be written on exam sheets.
Exam will consist of ~50% multiple choice and ~50% free response (simple calculations, short answers, brief essays, etc.)
During the midterm you may not 1) use any type of communication device or 2) wear a brimmed hat.
Brief summary of important
topics:
Chapter 1
Structure and distance scales of the observable universe: How galaxies are distributed on the largest scales, the approximate number of galaxies, superclusters, clusters, the size and structure of galaxies, the number of stars in a galaxy, the size and structure of the solar system, distances to other objects in the soar system in light minutes or hours.
The expanding the universe: The big bang, the age of the universe, looking back in time by looking at distant objects.
Composition of the universe: Primordial hydrogen and helium, how heavier elements are formed.
Motions of objects: EarthÕs rotation and revolution, SunÕs motion around the galaxy, random relative motion of local galaxies, organized recession of distant galaxies.
Chapter 2, Section 1
How things look from Earth: Relative proximity of visible stars, the Milky Way, determining the angular size of objects
Chapter S2
The postulates of relativity: Laws of
nature are the same for all observers + speed of light is same fro all
observers.
The results of the postulates: No
motion faster than light, the relativity of simultaneity, time dilation, length
contraction, velocity addition.
Experimental confirmation: Direct
measurements of the speed of light, elementary particle accelerators, nuclear
power.
The sense of relativity: How the effects of the relativity of
simultaneity, time dilation, and length contraction combine to make sense.
Chapter S4
The standard model: Leptons and
quarks, families
Fundamental forces: Characteristics of
gravity, electromagnetic, nuclear weak force, and strong force
Quantum effects: Exclusion principle for fermions and
degeneracy pressure, uncertainty principle and virtual particles and tunneling,
slow ÒevaporationÓ of black holes?
Chapter 14, Sections 1 and 2
The mystery of the SunÕs energy:
Chemical, gravitational, mass energy.
Gravitational equilibrium: Fusion in
the core and the SunÕs thermostat.
The proton-proton chain and the
synthesis of Helium.
Neutrinos as a probe of the SunÕs
core: Neutrino detectors and the solar neutrino problem.
Chapter 15
Properties of stars: Temperature,
Luminosity, Size, Mass, Lifetime.
How we determine temperature: Spectral
types
How we determine luminosity: Distance
from parallax measurements and apparent brightness.
How we determine size: From dependence
of luminosity on temperature and surface area. Radius is proportional to the square root of luminosity over
the square of the temperature. Lines of constant radius on the H-R diagram.
How we determine mass: Gravitational
interactions with other objects, binary systems
The H-R diagram: Plotting luminosity
versus inverse temperature.
The main sequence: Characteristic core
fusion of hydrogen, fundamental dependence of all properties on mass and age.
Lifetime as a main sequence star:
Reason for inverse relationship of mass and lifetime.
Red giants and white dwarfs.
Star clusters: Open and globular,
numbers of stars, sizes, and locations, Òmain sequence turnoffsÓ and ages.