new physics we learned in astro
behavior of light	Kirchhoff�s laws	what kind of spectrum (continuous, bright-line, dark-line) comes from what state of matter
	blackbody laws	Wien�s ( lmax flux  =  constant/T Stefan�s (surface flux = s T^4) blackbody curve shapes
	interference	n l = d sin q
	Doppler effect (shifting and broadening)	Dl/l = v(radial)/c
	photon energy	E = hc/l
angular physics	angular size, velocity, and acceleration	q, w, a
	angular momentum & conservation	L = Iw   for an extended particle L = mvr  for a point particle
	torque	t   =  force x lever arm x sin q
	angular version of Newton's 2nd law	DL  =  t Dt
quantum physics	Bohr model of the atom; quantization of energy levels
	Heisenberg uncertainty principle: why fusion can occur in the sun; how degenerate matter acquires high speeds to produce high pressure	Dp  Dx  =  h DE  Dt  =  h
	Pauli exclusion principle	the behavior of degenerate matter
nuclear physics	mass energy	mc^2
particle physics	conservation laws	old: charge, energy, momentum new: baryon number, lepton    numbers, angular momentum
	KE/light released in fusion reactions	conservation of energy
fluids	Pascal�s principle	P = r g h
	Archimedes� principle	buoyant force = weight of fluid displaced
	ideal gas law	P = n k T
temperature and energy transfer	avg KE/particle	3/2 k T
	energy transfer methods & conditions under which they occur	convection photon diffusion (random walk)
gravitation	grav energy of two point masses	- G M m/d
	grav energy of a spherical cloud	- G M^2/R
	Kepler's 3 laws
	Newton's version of  Kepler's 3rd  law	(m1 + m2) P^2= (4p^2/G)(a1 + a2)^3