After reading Ch 9 in Croswell:
 How did Fred Hoyle know that the nucleus of Carbon had a
special energy state, known as a "resonance"?

What are the rprocess and the sprocess? How do they differ?
 Which seminal paper first demonstrated their importance?
Which two reactions permit the sprocess to occur?
How was Cameron's paper presenting the first
of these reactions received?
After reading Sec. 10.3 in C&O:
 A.) To see that E=mc^{2} is relevant even to chemical
reactions, perform the calculation suggested on p. 299 as follows:
Which has lower mass: a Hydrogen atom (consisting of an electron
orbiting a proton at the Bohr radius) OR a proton plus an electron (assumed
to be a large distance apart)? Use values for physical constants in your book.
Does your result make sense in light of Coulomb's Law?
B.)
Compute the mass difference, in kg, and convert it into an energy
difference, recording as many
significant figures as needed. Express this energy in both
Joules and eV.

Suppose 1000 kg of Hydrogen inside the Sun undergoes nuclear fusion.
What is the mass of Helium that is produced?
In the example just above, how much energy is released?

A.) How much mass, in kg, does the Sun lose in one second due to nuclear fusion?
How about in one day?
B.) How much mass will the Sun have lost after it is 10 billion years old?
Express this as a fraction of the Sun's total (current) mass.

Compare the energy released in one second by the Sun to that released by
a nuclear weapon of your choice. Use this comparison to create a simple sentance
which you can say to nonscientists to give them some idea of the energy
output of the Sun. (For more information on nuclear weapons,
and to test your own simulated ones visit:
http://nuclearsecrecy.com/nukemap/
)
 Using a periodic table, fill in the blanks in these nuclear reactions involving
beta (positive) decays. (Both reactions are relevant to stellar energy
generation):
^{13}N → ^{??}___ + e^{+} + ν_{e }
^{19}F → ^{??}___ + e^{+} + ν_{e }
Hint: Start with the most basic weak interaction, that of decay of a
neutron.

Suppose you wish to make a model of a star. You begin by assuming
it to be spherically symmetric. Hence all properties of the star can be
written as a function of radius alone, f(r). Which properties
could you include in your model? List as many as you can think of.
What other starting assumptions (that is, initial attributes of the star)
would you need to create the model?