1.HINTS
ON TAKING "OPEN BOOK AND NOTES" TESTS:
b.
Carefully read the Chapter Summary, try to do the Conceptual Questions,
and know the meaning of allthe
Key Terms at the back of each chapter.
c.
Don't forget the index or the glossary.
d.
Read
the test questions carefully!
e.
Go through the test once and answer all of the questions that you can.Then
go back and do the other questions.
f.
Mark on the test booklet: cross off obviously wrong answers, work the problems,
and show your work. Circle the answer on the test booklet - that is the
last resort if you have made a mistake on the answer sheet.
g.
Carefully darken in the answer on the answer sheet, do not rip, mutilate,
or fold it.
h.
Check your answer sheet. Make sure you have answered all 50 questions.
i.
MAKE SURE THAT YOUR NAME IS ON THE ANSWER SHEET AND YOU HAVE PUT IN YOUR
UNIVERSITY
ID NUMBER-LEFT JUSTIFIED.FILL
IN THE CIRCLES SO THE MACHINE CAN READ IT!!!! I
will subtract points if this is not done
BRING
A PICTURE ID. I WILL ASK YOU TO PLACE IT ON THE TABLE IN FRONT OF YOU AND
I WILL GO AROUND THE CLASS DURING THE EXAM CHECKING EACH ID.
Chapter
6: LIGHT The Cosmic Messenger
1.
What is meant by electromagnetic radiation? What are some of the properties
of light?
2.
What is meant by the wavelength and frequency of light?
3.
What is an Angstrom?I will use
Angstroms not nanometers. What is the velocity of light?
4.
What is a photon? What is meant by the wave-particle duality of light?
5.
What is the relationship between wavelength, frequency, and energy of light?How
does the energy of a photon of light depend on its wavelength? What kind
of light is most energetic, least energetic?
6.
What are the various parts of the spectrum? Note the definitions of infra-red,
ultraviolet, X-ray, Gamma-ray, ..Know the different kinds of light (page
101 Figure 6.2).
7.
What is meant by atmospheric windows? Where in the spectrum is the atmosphere
transparent, opaque?
8.
What are refracting telescopes? Reflection telescopes? How do they differ?
9.
What is the objective? Eyepiece?
10.
What is the fundamental difficulty with refracting telescopes? (Chromatic
Aberration)
11.
How does a telescope form an image? Note that the image is upside down.
How is your eye like a telescope?What
is meant by the focus of a lens or mirror? What is the focal length of
a lens or mirror?
12.
What is an achromatic lens? Does it really fix chromatic aberration?
13.
What is the objective mirror? What is a newtonian telescope? Cassegrain
telescope? Prime Focus? (Look at Figure 6-6)
14.
Where are the Keck telescopes located? Why on a mountain top?
15.
What is the light-gathering power of a telescope?On
what does it depend?
16.
What is the resolving power of a telescope?Why
is it relatively unimportant for ground based telescopes?
17.
What atmospheric effect reduces the resolving power of a telescope? (Seeing)
18.
What are some of the advantages of a reflector over a refractor for large
astronomical telescopes.
19.
Why is magnification unimportant when buying a new telescope for ground
based viewing?
19.
Active optics means that the shape of the mirror can be changed (slightly)
over a few minutes to correct for the atmosphere.
20.
What are some of the new large telescopes called? LBT, VLT, ... I showed
pictures and discussed them in class.
21.
A CCD (charge couple device) is a light sensitive surface divided into
a lot of pixels. They are very common.A
CCD detector is also used in camcorders.A
spectrograph can separate the wavelengths of light out so we can see all
the colors.One instrument for
doing this is a prism. Another is a grating. The back of an audio or digital
CD is a grating. (Not a good one)
22.
Why are radio telescopes so big?A
radio interferometer makes a lot of separate radio antennas act as a single
antenna improving the resolution. One
such observatory is the VLA. Where is it located? Did you see it in the
movie AContact@?
We do not listen to the signal from a radio telescope.
23.
Where is the Arecibo radio telescope located?
24.We
launch satellite observatories to observe in wavelengths blocked by the
atmosphere or to observe without worrying about the effects of Aseeing.@
25.
Some of the infra-red satellites were ISO, IRAS, and soon SIRTF. In the
UV we had IUE, EUVE, and HST. In the X-ray we have CHANDRA.
26.
Read the Summary.
Chapter
7. Starlight and Atoms.
1.
The temperature of a gas is a measure of the average speed of the particles
in the gas.
2.
Look back at the temperature scales in your notes. I did this early in
the semester.
6.
What is the Stefan-Boltzmann Law? Wien=s
Law? How can we use Wien=s
Law to determine at what wavelength a thermal emitter radiates most strongly.?
The value of the constant given in class is 5000 * 6000 because I use Angstroms
not nanometers.
7.
SKIP Color Index.
8.
Remember the structure of an atom (nucleus with protons and neutrons plus
electron cloud orbiting the nucleus)
9.
What is meant by neutral, ionized, electron shells. Remember that all normal
matter consists of atoms. Each atom consists of a nucleus with electron(s)
in orbit around the nucleus.The
nucleus consists of proton(s) and neutron(s).Know
what is meant by atomic number and atomic weight. What is an isotope? How
are the chemical elements labeled?
10.
The Coulomb force binds the electrons to the nucleus.
11.
The various orbits around the nucleus are called energy levels because
it takes energy to move away from the nucleus or the atom must give up
energy for the electron to jump back toward the nucleus. Remember that
only certain energies (distances from the nucleus) are permitted.
12.
What is an excited atom? Ground state?
13.
Know Kirchhof=s
Laws as shown in Table 7-1 on page 132 and Figure 7-11 on page 133:(1)
A hot solid or dense gas produces a continuous spectrum. (2) A low density
excited or hot gas produces a bright, emission line spectrum. (3) Put a
low density gas in front of a continuous spectrum and you get a continuous
spectrum with dark, absorption lines superimposed.
14.
Know emission and absorption lines and where and how they are formed.
15.
Review the hydrogen spectrum and the details of figure 7-12.What
is a transition?
16.
SKIP 7-4 from pages 135 to 140. You are responsible for the Doppler Effect
on pages 140 to 142.
17.
What is the Doppler Effect or Doppler Shift.How
can we use it to tell whether an object is moving toward or away from us?
What is meant by a blue shift? A red shift?
18.
Review the use of the Doppler effect as I discussed in class.
19.
Skip AThe
Shapes of Spectral Lines@
Chapter
8.The Sun
Know
the data on Page 147
1.
What are the photosphere, chromosphere, corona?
2.
What is granulation?What is it
telling us about heat flow from the interior? How long does a granule last?
3.
What is convection? Conduction? Radiation?
4.
What is supergranulation? Spicules are found at the edges of supergranules.
5.
What do we learn from Limb Darkening? (That the temperature decreases outward
in the photosphere)
6.
How far does the Corona extend into space? How hot is the corona?What
are the various ideas for causing the heat? What is the solar wind?What
is the speed of the solar wind at the Earth=s
distance from the Sun?
7.Helioseismology
is the study of the interior of the Sun using the Sun=s
oscillations in radius.We can study
the interior of the sun just as ringing a bell tells us how the bell is
made.
8.
What are sunspots? Why do they appear dark?Which
part is the Umbra? The Penumbra?Note
that they are located in Active Regions.
9.
The Zeeman effect is a way to measure the strength of a magnetic field
in an ionized gas.We know that sunspots
are somewhat like bar magnets.How
does the polarity (N or S pole) of sunspots change over the solar cycles?
10.How
long is the solar sunspot cycle?The
solar active cycle?
11.How
long is the solar magnetic cycle?
12.
When was the Maunder minimum?
13.
What is the Butterfly diagram and what does it tell us (Figure 8-13)?
14.
What is a Prominence, what is a Flare?Look
at the pictures on page 161.
15.What
is ejected from Coronal Holes?
16.
Is there any evidence for a Solar-Terrestrial Climate link? At all?
17.
What were some of the early ideas about the source of the Sun=s
energy. How did we know they were wrong?
18.
Where does the energy from the sun come from? Why do we know that it must
be nuclear energy?
19.
Binding energy is the energy that keeps the protons and neutrons in the
nucleus from flying apart.
20.
Nuclear Fusion requires high temperatures and high densities to overcome
the Coulomb barrier. (Like charges repel)
21.What
is the proton-proton chain? Who first proposed it in 1938 (and is still
around publishing).
22.
What is a neutrino? How is energy released in the proton-proton chain?Deuterium
is an isotope of hydrogen.
23.
How does the energy flow from the center to the surface? What are convection,
conduction, radiation?
24.
What is the difference between nuclear fusion and nuclear fission. Which
is most important in current nuclear power plants?
25.
What does the solar neutrino experiment tell us? What are the most recent
results: Discussed in class.