Equations of State

Currently (if the documentation was well updated), we have two different gas equations of state (EoS) implemented: ideal and isothermal; as well as a variety of EoS for “planetary” materials. The EoS describe the relations between our main thermodynamical variables: the internal energy (\(u\)), the density (\(\rho\)), the entropy (\(A\)) and the pressure (\(P\)).

Gas EoS

In the following section, the variables not yet defined are: \(\gamma\) for the adiabatic index and \( c_s \) for the speed of sound.

Ideal Gas
Variable A u P
A   \( \left( \gamma - 1 \right) u \rho^{1-\gamma} \) \(P \rho^{-\gamma} \)
u \( A \frac{ \rho^{ \gamma - 1 } }{\gamma - 1 } \)   \(\frac{1}{\gamma - 1} \frac{P}{\rho}\)
P \( A \rho^\gamma \) \( \left( \gamma - 1\right) u \rho \)  
\(c_s\) \(\sqrt{ \gamma \rho^{\gamma - 1} A}\) \(\sqrt{ u \gamma \left( \gamma - 1 \right) } \) \(\sqrt{ \frac{\gamma P}{\rho} }\)
Isothermal Gas
Variable A u P
A   \(\left( \gamma - 1 \right) u \rho^{1-\gamma}\)  
u   const  
P   \(\left( \gamma - 1\right) u \rho \)  
\( c_s\)   \(\sqrt{ u \gamma \left( \gamma - 1 \right) } \)  

Planetary EoS

Configuring SWIFT with the --with-equation-of-state=planetary and --with-hydro=planetary options enables the use of multiple 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:

  • Tillotson (Melosh, 2007): 1
    • Iron: 100
    • Granite: 101
    • Water: 102
  • Hubbard & MacFarlane (1980): 2
    • Hydrogen-helium atmosphere: 200
    • Ice H20-CH4-NH3 mix: 201
    • Rock SiO2-MgO-FeS-FeO mix: 202
  • SESAME (and similar): 3
    • Iron (2140): 300
    • Basalt (7530): 301
    • Water (7154): 302
    • Senft & Stewart (2008) water (in a SESAME-style table): 303

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 Planetary (Density-Energy, Multi-Material) SPH hydrodynamics scheme, but makes these materials currently incompatible with other entropy-based schemes.

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). The table files for the HM80 and SESAME-style EoS can be downloaded using the examples/EoSTables/get_eos_tables.sh script.

How to Implement a New Equation of State

See General information for adding new schemes for a full list of required changes.

You will need to provide an equation_of_state.h file containing: the definition of eos_parameters, IO functions and transformations between the different variables: \(u(\rho, A)\), \(u(\rho, P)\), \(P(\rho,A)\), \(P(\rho, u)\), \(A(\rho, P)\), \(A(\rho, u)\), \(c_s(\rho, A)\), \(c_s(\rho, u)\) and \(c_s(\rho, P)\). See other equation of state files to have implementation details.