5 files changed, 80 insertions, 106 deletions
diff --git a/physics/general relativity.page b/physics/general relativity.page
deleted file mode 100644
index f4a45af..0000000
--- a/physics/general relativity.page
+++ /dev/null
@@ -1,24 +0,0 @@
----
-format: rst
-categories: physics
-toc: no
-...
-
-===========================
-General Relativity
-===========================
-
-.. warning:: This is a rough work in progress!! Likely to be factual errors, 
-    poor grammar, etc.
-
-.. note:: Most of this content is based on a 2002 Caltech course taught by
-    Kip Thorn [PH237]_
-
-*See also `math/tensors </math/tensors>`__*
-
-(no content)
-
-References
-----------------
-
-.. [PH237] `Gravitational Waves`:title: (aka ph237), a course taught by Kip Thorne at Caltech in 2002. See http://elmer.tapir.caltech.edu/ph237/ for notes and lecture videos.
diff --git a/physics/gravitational waves.page b/physics/gravitational-waves.page
index 66f6c04..c853e2b 100644
--- a/physics/gravitational waves.page
+++ b/physics/gravitational-waves.page
@@ -22,33 +22,33 @@ Waves are double integrals of curvature tensor...
 
 Gravitons as Quantum Particles
 ---------------------------------
-Invariance angles: (Spin of quantum particle) = :latex:`$2 pi$` / (invariance angle)
+Invariance angles: (Spin of quantum particle) = $2 pi$ / (invariance angle)
 
-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
+Graviton has $\pi$ invariance angle, so it is spin 2; photons have unique $\arrow{E}$ vector, so invariance angle is $2\pi$, spin 1
 
 Also describes spin by the group of Lorentz transformations which effect propagation.
 
 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 :latex:`$\geq$` spin of quantum = 2 for graviton ((??))
+Waves' multipole order $\geq$ spin of quantum = 2 for graviton ((??))
 
 Waves don't propagate like E, because mass monopoles don't oscillate like charges.
 
-: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}$` 
-First term: mass can't oscillate
-Second term: momentum can't oscillate
-Third term: mass quadrupole moment dominates
-Fourth term: angular momentum can't oscillate
+$ 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 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 quadrupole
-moment :m:`$M_2 \approx M L^2$`, :m:`$h \approx 1/c^2` (Newtonian potential
-energy) ????
+moment $M_2 \approx M L^2$, $h \approx 1/c^2 (Newtonian potential energy) ????
 
-h on the order of :m:`$10^{-22}$`
+h on the order of $10^{-22}$
 
 Propagation
 -----------------
@@ -99,7 +99,7 @@ Extreme Low Frequency: 10^-16 Hz, Cosmic Microwave Background anisotropy
 Detectors
 -----------------
 
-:m:`$\Delta L = h L ~ \leq 4 \times 10^{-16} \text{cm}$`
+$\Delta L = h L ~ \leq 4 \times 10^{-16} \text{cm}$
 
 LIGO (10 Hz to 1kHz)
     Also GEO, VIRGO, TAMA (?), AIGO
@@ -114,4 +114,4 @@ Currently in Louisiana State University (Allegro), University of West Australia
 References
 ----------------
 
-.. [PH237] `Gravitational Waves`:title: (aka ph237), a course taught by Kip Thorne at Caltech in 2002. See http://elmer.tapir.caltech.edu/ph237/ for notes and lecture videos.
+[PH237]: **Gravitational Waves** (aka ph237), a course taught by Kip Thorne at Caltech in 2002. See http://elmer.tapir.caltech.edu/ph237/ for notes and lecture videos.
diff --git a/physics/special relativity.page b/physics/special relativity.page
deleted file mode 100644
index 2f5b9af..0000000
--- a/physics/special relativity.page
+++ /dev/null
@@ -1,62 +0,0 @@
----
-format: rst
-categories: physics
-toc: no
-...
-
-===========================
-Special Relativity
-===========================
-
-.. warning:: This is a rough work in progress!! Likely to be factual errors, 
-    poor grammar, etc.
-
-.. note:: Most of this content is based on a 2002 Caltech course taught by
-    Kip Thorn [PH237]_
-
-*See also `physics/general relativity</physics/generalrelativity/>`__*
-
-As opposed to general relativity, special relativity takes place in a *flat*
-Minkowski space time: a 4-space with three spatial dimensions and one time
-dimension.
-
-+----------------+--------------------+
-| Index notation | Variable | Type    |
-+----------------+--------------------+
-| `$x^0$`:m:     | `$t$`:m: | Time    |
-| `$x^1$`:m:     | `$x$`:m: | Spatial |
-| `$x^2$`:m:     | `$y$`:m: | Spatial |
-| `$x^3$`:m:     | `$z$`:m: | Spatial |
-+----------------+--------------------+
-
-Separations
--------------
-
-The separation `$(\Delta s)^2$`:m: between two events in space time, in a given
-Lorentzian/inertial frame, is defined
-as:
-
-:m:`$$ (\Delta s)^2 \equiv -(\Delta t)^2 + (\Delta x)^2 + (\Delta y)^2 + (\Delta z)^2 $$`
-
-or
-
-:m:`$$ (\Delta s)^2 \equiv -(\Delta x^0)^2 + \sum_{i,j} \delta_{ij} \Delta x^i \Delta x^j$$`
-
-where :m:`$\delta_{ij}$` is the Kronecker delta (unity or 1 when 
-:m:`$i=j$`; zero otherwise), and the indices i and j are over the spatial
-dimensions 1,2,3 (corresponding to x,y,z). It can be shown that this separation
-is Lorentz-invariant; the scalar value of separation between two events does
-not depend on the inertial frame chosen.
-
-Note the negative sign in front of the time dimension. The are three types of
-separations: **space-like** when :m:`$(\Delta s)^2 > 0$`, **null-** or 
-**light-like** when :m:`$(\Delta s)^2 = 0$`, and **time-like** when 
-:m:`$(\Delta s)^2 < 0$`. When dealing with time-like separations, ignore the
-implication of an imaginary number. The difference in time :m:`$\Delta \Tau$` 
-is always real: :m:`($\Delta \Tau)^2= -(\Delta s)^2$`.
-
-
-References
-----------------
-
-.. [PH237] `Gravitational Waves`:title: (aka ph237), a course taught by Kip Thorne at Caltech in 2002. See http://elmer.tapir.caltech.edu/ph237/ for notes and lecture videos.
diff --git a/physics/special-relativity.page b/physics/special-relativity.page
new file mode 100644
index 0000000..bb5f564
--- /dev/null
+++ b/physics/special-relativity.page
@@ -0,0 +1,60 @@
+---
+format: rst
+categories: physics
+toc: no
+...
+
+===========================
+Special Relativity
+===========================
+
+.. warning:: This is a rough work in progress!! Likely to be factual errors, 
+    poor grammar, etc.
+
+.. note:: Most of this content is based on a 2002 Caltech course taught by
+    Kip Thorn [PH237]_
+
+As opposed to general relativity, special relativity takes place in a *flat*
+Minkowski space time: a 4-space with three spatial dimensions and one time
+dimension.
+
+-------------- --------   ---------
+Index notation Variable   Type    
+-------------- --------   ---------
+  $x^0$          $t$       Time    
+  $x^1$          $x$       Spatial 
+  $x^2$          $y$       Spatial 
+  $x^3$          $z$       Spatial 
+-------------- --------   ---------
+
+Separations
+-------------
+
+The separation $(\Delta s)^2$ between two events in space time, in a given
+Lorentzian/inertial frame, is defined
+as:
+
+$$ (\Delta s)^2 \equiv -(\Delta t)^2 + (\Delta x)^2 + (\Delta y)^2 + (\Delta z)^2 $$
+
+or
+
+$$ (\Delta s)^2 \equiv -(\Delta x^0)^2 + \sum_{i,j} \delta_{ij} \Delta x^i \Delta x^j$$
+
+where $\delta_{ij}$ is the Kronecker delta (unity or 1 when 
+$i=j$; zero otherwise), and the indices i and j are over the spatial
+dimensions 1,2,3 (corresponding to x,y,z). It can be shown that this separation
+is Lorentz-invariant; the scalar value of separation between two events does
+not depend on the inertial frame chosen.
+
+Note the negative sign in front of the time dimension. The are three types of
+separations: **space-like** when $(\Delta s)^2 > 0$, **null-** or 
+**light-like** when $(\Delta s)^2 = 0$, and **time-like** when 
+$(\Delta s)^2 < 0$. When dealing with time-like separations, ignore the
+implication of an imaginary number. The difference in time $\Delta \Tau$ 
+is always real: ($\Delta \Tau)^2= -(\Delta s)^2$.
+
+
+References
+----------------
+
+[PH237]: **Gravitational Waves** (aka ph237), a course taught by Kip Thorne at Caltech in 2002. See http://elmer.tapir.caltech.edu/ph237/ for notes and lecture videos.
diff --git a/physics/units.page b/physics/units.page
index 385136c..bfc78bc 100644
--- a/physics/units.page
+++ b/physics/units.page
@@ -3,11 +3,11 @@ format: rst
 categories: physics
 toc: no
 ...
+
 ======================
 Units
 ======================
 
-.. contents::
 
 SI Units
 --------------------
@@ -26,7 +26,7 @@ Natural Units
 Natural units are a system of units which replace (or re-scale) the usual mass,
 length, and time bases with quantities which have "natural" (physical)
 constants associated with them. The two constants usually chosen are the speed
-of light (c) and Plank's constant (:m:`$\hbar$`); the gravitational constant
+of light (c) and Plank's constant ($\hbar$); the gravitational constant
 (G) is a possibility for the third constant/unit, but energy (in
 electron-volts: eV) is often used instead because it gives more useful
 relations and because there is no accepted theory of quantum gravity to unite
@@ -36,18 +36,18 @@ Working with natural units simplifies physical relations and equations because
 many conversion factors drop out.
 
 Given the relations between cgs units (gm, cm, sec) and natural units (c,
-:m:`$\hbar$` , eV), we can find the natural units of an arbitrary quantity
-:m:`$[Q]=[gm]^{a}[cm]^{b}[sec]^{c}=[c]^{\alpha}[\hbar]^{\beta}[eV]^{\gamma}$`:
+$\hbar$ , eV), we can find the natural units of an arbitrary quantity
+$[Q]=[gm]^{a}[cm]^{b}[sec]^{c}=[c]^{\alpha}[\hbar]^{\beta}[eV]^{\gamma}$:
 
-:m:`$$(\alpha,\beta,\gamma)=\left(\begin{array}{ccc} -2 & 1 & 0\\ 0 & 1 & 1\\ 1 & -1 & -1\end{array}\right)\left(\begin{array}{c} a\\ b\\ c\end{array}\right)=(-2a+b,b+c,a-b-c)$$`
+$$(\alpha,\beta,\gamma)=\left(\begin{array}{ccc} -2 & 1 & 0\\ 0 & 1 & 1\\ 1 & -1 & -1\end{array}\right)\left(\begin{array}{c} a\\ b\\ c\end{array}\right)=(-2a+b,b+c,a-b-c)$$
 
 or in reverse:
 
-:m:`$$(a,b,c)=\left(\begin{array}{ccc} 0 & 1 & 1\\ 1 & 2 & 2\\ -1 & -1 & -2\end{array}\right)\left(\begin{array}{c} \alpha\\ \beta\\ \gamma\end{array}\right)=(\beta+\gamma,\alpha+2\beta+\gamma,-\alpha-\beta-2\gamma)$$`
+$$(a,b,c)=\left(\begin{array}{ccc} 0 & 1 & 1\\ 1 & 2 & 2\\ -1 & -1 & -2\end{array}\right)\left(\begin{array}{c} \alpha\\ \beta\\ \gamma\end{array}\right)=(\beta+\gamma,\alpha+2\beta+\gamma,-\alpha-\beta-2\gamma)$$
 
 Plank Units
 ----------------
-Plank units (defined by Plank soon after defining his constant :m:`$\hbar$`) are a version of _`Natural Units` using the gravitational constant G as the the 
+Plank units (defined by Plank soon after defining his constant $\hbar$) are a version of _`Natural Units` using the gravitational constant G as the the 
 third unit (instead of the common measure of energy). When converted back into
 mass-length-time units we get three quantities which define the "Plank Scale",
 which may provide estimation of the domain where quantum gravity effects become