spell checked some files; moved and added images; fixed some links; added warnings

1 files changed, 42 insertions, 14 deletions

diff --git a/physics/gravitational waves b/physics/gravitational waves
index db2e667..81080c3 100644
--- a/physics/gravitational waves
+++ b/physics/gravitational waves
@@ -2,14 +2,14 @@
 Gravitational Waves
 =======================
 
-:Author: bnewbold@mit.edu
+.. warning:: This is a rough work in progress!! Likely to be factual errors, poor grammer, etc.
 
 .. note:: Most of this content is based on a 2002 Caltech course taught by
     Kip Thorn [PH237]_
 
 Raw Info
 -----------------
-Rank 4 Riemann tensors, will cover different gages.
+Rank 4 Riemann tensors, will cover different gauge.
 Waves are double integrals of curvature tensor...
  
 
@@ -20,38 +20,66 @@ Invariance angles: (Spin of quantum particle) = :latex:`$2 pi$` / (invariance an
 
 Graviton has :latex:`$\pi$` invariance angle, so it is spin 2; photons have unique :latex:`$\arrow{E}$` vector, so invariance angle is :latex:`$2\pi$`, spin 1
 
-Also describes spin by the group of lorentz transformations which effect propogation.
+Also describes spin by the group of Lorentz transformations which effect propagation.
 
-Two polarizations: cross and plus, corresponding to spin of particles aligning wiht or against propagation?  (Ref: eugene vickner? reviews of modern physics)
+Two polarizations: cross and plus, corresponding to spin of particles aligning with or against propagation?  (Ref: Eugene Vickner? reviews of modern physics)
 
-Waves' multipole order $\geq$ spin of quantum = 2 for graviton ((??))
+Waves' multipole order :latex:`$\geq$` spin of quantum = 2 for graviton ((??))
 
-Waves don't propogate like E, because mass monopoles don't oscillate like charges.
+Waves don't propagate like E, because mass monopoles don't oscillate like charges.
 
-:latex:`$ h \req \frac{G}{c^2} \frac{M_0}{r} + \frac{G}{c^3} \frac{M'_1}{r} + \frac{G}{c^4} \frac{M''_2}{r} + \frac{G}{c^4} \frac{S'_1}{r} + \frac{G}{c^5} \frac{S''_1}{r}$` 
+:latex:`$ h \approx \frac{G}{c^2} \frac{M_0}{r} + \frac{G}{c^3} \frac{M'_1}{r} + \frac{G}{c^4} \frac{M''_2}{r} + \frac{G}{c^4} \frac{S'_1}{r} + \frac{G}{c^5} \frac{S''_1}{r}$` 
 First term: mass can't oscillate
 Second term: momentum can't oscillate
-Third term: mass qudrupole moment dominates
+Third term: mass quadrupole moment dominates
 Fourth term: angular momentum can't oscillate
 Fifth term: current quadrupole
 
 Energy
 ----------------
 
-Quick calculation: for a source with mass M, size L, period P, the quadupole moment $M_2 \req M L^2$, h \req 1/c^2 (newtonian potential energy) ????
+Quick calculation: for a source with mass M, size L, period P, the quadrupole moment $M_2 \approx M L^2$, h \approx 1/c^2 (Newtonian potential energy) ????
 
 h on the order of $10^{-22}$
 
-Propogation
+Propagation
 -----------------
 
-When wavelength much less than curvature of universe (background), then gravitational waves propagate like light waves: undergo red shifts, gravitational lensing, inflationary redshift, etc. 
+When wavelength much less than curvature of universe (background), then gravitational waves propagate like light waves: undergo red shifts, gravitational lensing, inflationary red shift, etc. 
+
+Sources
+-------------
+
+Inspirals of bodies into super-massive black holes
+    Eg, white dwarfs, neutron stars, small black holes.
+    Super-massive black holes are expected near the centers of galaxies.
+    Low frequencies (LISA); waveforms could hold data about spacetime curvature
+    local to the black hole.
+    Waveforms could be very difficult to predict.
+
+Binary black hole mergers
+    Broadband signals depending on masses.
+
+Neutron Star/Black hole mergers
+    Stellar mass objects existing in the main bodies of galaxies.
+    Higher frequencies (LIGO and AdvLIGO).
+
+Neutron Star/Neutron Star mergers
+    Have actual examples in our galaxy of these events; but final inspiral rate
+    is so low that we have must listen in other galaxies. Merger waves will
+    probably be lost in higher frequency noise, so can't probe local 
+    gravitational curvature. 
+    May observe "tails" of waves: scattering off of high curvature around the 
+    binary.
+
+Pulsars (spinning neutron stars)
+    Known to exist in our galaxy.
 
 Spectrum
 ----------------
 
 High Frequency: Above 1 Hz, LIGO (10 Hz to 1kHz), resonant bars
-    Small black holes (2 to 1k suns), neutron stars, supernovae
+    Small black holes (2 to 1k suns), neutron stars, supernovas
 
 Low frequency: 1Hz and lower, LISA (10^-4 Hz to 0.1 Hz), Doppler tracking of spacecraft
     Massive black holes (300 to 30 million suns), binary stars
@@ -63,12 +91,12 @@ Extreme Low Frequency: 10^-16 Hz, Cosmic Microwave Background anisotropy
 Detectors
 -----------------
 
-$\Delta L = h L \lreq 4 \times 10^{-16} \text{cm}$
+:m:`$\Delta L = h L ~ \leq 4 \times 10^{-16} \text{cm}$`
 
 LIGO (10 Hz to 1kHz)
     Also GEO, VIRGO, TAMA (?), AIGO
 
-LISA (10^-4 Hz to 0.1 Hz)
+LISA (10e-4 Hz to 0.1 Hz)
 
 Resonant Bars
 ~~~~~~~~~~~~~~~