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BnsInitialData::FirstOrderSystem Struct Reference

The Irrotational Bns equations From Baumgarte and Shapiro Chapter 15 formulated as a set of coupled first-order PDEs. More...

#include <FirstOrderSystem.hpp>

Public Types

using primal_fields = implementation defined
 
using primal_fluxes = implementation defined
 
using background_fields = implementation defined
 
using inv_metric_tag = gr::Tags::InverseSpatialMetric< DataVector, 3 >
 
using fluxes_computer = Fluxes
 
using sources_computer = Sources
 
using boundary_conditions_base = elliptic::BoundaryConditions::BoundaryCondition< 3 >
 
using modify_boundary_data = void
 

Static Public Attributes

static constexpr size_t volume_dim = 3
 

Detailed Description

The Irrotational Bns equations From Baumgarte and Shapiro Chapter 15 formulated as a set of coupled first-order PDEs.

Details

This system formulates the Irrotational Bns Hydrostatic Equilibrium equations for the velocity potential Φ. For a background matter distribution (given by the specific enthalpy h) and a background metric γij. The velocity potential is defined by DiΦ=hui with ui (the spatial part of) the four velocity and where Γjki=12γil(jγkl+kγjllγjk) are the Christoffel symbols of the second kind of the background (spatial) metric γij. The background metric γij and the Christoffel symbols derived from it are assumed to be independent of the variables Φ and ui, i.e. constant throughout an iterative elliptic solve. Additionally a background lapse ( α) and shift ( β) must be provided. Finally, a "rotational killing vector" ki (with magnitude proportional to the angular velocity of the orbital motion) is provided. The rotational shift is defined as Bi=βi+ki which is heuristically the background motion of the spacetime.

The system can be formulated in terms of these fluxes and sources (see elliptic::protocols::FirstOrderSystem):

iFi+S=f

Fi=DiϕBjDjϕα2BiS=FiDi(lnαρh)ΓijiFjf=Di(CBiα2)Cα2BiDi(lnαρh)


The documentation for this struct was generated from the following file: