Update planetary docs

doc/RTD/source/Planetary/equations_of_state.rst

@@ -7,39 +7,51 @@ Planetary Equations of State
 ============================
    
 Configuring SWIFT with the ``--with-equation-of-state=planetary`` and 
-``--with-hydro=planetary`` options enables the use of multiple EoS.
+``--with-hydro=planetary`` options enables the use of multiple 
+equations of state (EoS).
 Every SPH particle then requires and carries the additional ``MaterialID`` flag 
 from the initial conditions file. This flag indicates the particle's material 
 and which EoS it should use. 
 
-So far, we have implemented several Tillotson, SESAME, and Hubbard \& MacFarlane 
-(1980) materials, with more on their way.
-The material's ID is set by a base type ID (multiplied by 100), plus a minor 
-type:
+It is important to check that the EoS you use are appropriate 
+for the conditions in the simulation that you run.
 
-+ Tillotson (Melosh, 2007): Base type ``1``
+So far, we have implemented several Tillotson, ANEOS, SESAME, 
+and Hubbard \& MacFarlane (1980) materials, with more on the way.
+The material's ID is set by a base type ID (multiplied by 100), 
+plus a minor type:
+
++ Tillotson (Melosh, 2007): ``1``
     + Iron: ``100``
     + Granite: ``101``
     + Water: ``102``
-+ Hubbard \& MacFarlane (1980): Base type ``2``
++ Hubbard \& MacFarlane (1980): ``2``
     + Hydrogen-helium atmosphere: ``200``
     + Ice H20-CH4-NH3 mix: ``201``
     + Rock SiO2-MgO-FeS-FeO mix: ``202``
-+ SESAME (and similar): Base type ``3``
++ SESAME (and similar): ``3``
     + Iron (2140): ``300``
     + Basalt (7530): ``301``
     + Water (7154): ``302``
-    + Senft \& Stewart (2008) water (in a SESAME-style table): ``303``
+    + Senft \& Stewart (2008) water in a SESAME-style table: ``303``
++ ANEOS (in SESAME-style tables): ``4``
+    + Forsterite (Stewart et al. 2019): ``400``
+    + Iron (Stewart, zenodo.org/record/3866507): ``401``
+    + Fe85Si15 (Stewart, zenodo.org/record/3866550): ``402``
 
 Unlike the EoS for an ideal or isothermal gas, these more complicated materials 
 do not always include transformations between the internal energy, 
-temperature, and entropy. At the moment, we have only implemented 
-\\(P(\\rho, u)\\) and \\(c_s(\\rho, u)\\). 
-This is sufficient for the simple :ref:`planetary_sph` hydrodynamics scheme, 
+temperature, and entropy. At the moment, we have implemented 
+\\(P(\\rho, u)\\) and \\(c_s(\\rho, u)\\), 
+which is sufficient for the :ref:`planetary_sph` hydrodynamics scheme, 
 but makes these materials currently incompatible with entropy-based schemes.
 
+The data files for the tabulated EoS can be downloaded using 
+the ``examples/EoSTables/get_eos_tables.sh`` script.
+
 The Tillotson sound speed was derived using 
-\\(c_s^2 = \\left. \\dfrac{\\partial P}{\\partial \\rho} \\right|_S \\)
-as described in `Kegerreis et al. (2019) <https://doi.org/10.1093/mnras/stz1606>`_.
-The table files for the HM80 and SESAME-style EoS can be downloaded using 
-the ``swiftsim/examples/EoSTables/get_eos_tables.sh`` script.
+\\(c_s^2 = \\left. ( \\partial P / \\partial \\rho ) \\right|_S \\)
+as described in Kegerreis et al. (2019). 
+Note that there is a typo in the sign of
+\\(du = T dS - P dV = T dS + (P / \\rho^2) d\\rho \\),
+which was not used in the derivation.

doc/RTD/source/Planetary/index.rst

@@ -7,24 +7,24 @@ Planetary Simulations
 =====================
 
 SWIFT is also designed for running planetary simulations
-with a focus on giant impacts, as presented in 
+with a current focus on giant impacts, as presented in 
 `Kegerreis et al. (2019) <https://doi.org/10.1093/mnras/stz1606>`_, MNRAS 487:4.
 
-New features for planetary simulations are in active development
+More features for planetary simulations are in active development
 so please let us know if you are interested in using SWIFT 
 or have any implementation requests. For example a new equation of state
 or extensions to the tools for creating initial conditions.
     
 You can find an example simulation in ``swiftsim/examples/Planetary/``
 under ``EarthImpact/``.
-The tabulated equations of state files can be downloaded using 
+The tabulated equation of state files can be downloaded using 
 ``EoSTables/get_eos_tables.sh``.
 
 Planetary simulations are currently intended to be run with 
 SWIFT configured to use the planetary hydrodynamics scheme and equations of state:
 ``--with-hydro=planetary`` and ``--with-equation-of-state=planetary``.
 These allow for multiple materials to be used,
-chosen from the several available equations of state (more coming soon!).
+chosen from the several available equations of state.
 
 .. toctree::
    :maxdepth: 2

doc/RTD/source/Planetary/initial_conditions.rst

+.. Planetary Initial Conditions
+   Jacob Kegerreis, 13th March 2020
+
+.. _planetary_initial_conditions:
+   
+Initial Conditions
+==================
+
+(Full documentation coming soon!)
+
+See `Kegerreis et al. (2019) <https://doi.org/10.1093/mnras/stz1606>`_
+and `SEAGen <https://github.com/jkeger/seagen>`_.
\ No newline at end of file