GSPH force computation using Riemann solver results. More...

#include "shambackends/math.hpp"
#include "shambackends/sycl.hpp"
#include "shammodels/gsph/math/riemann/iterative.hpp"
#include "shammodels/sph/math/forces.hpp"

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Namespaces
namespace	shammodels
	namespace for models

Functions
template<class Tvec , class Tscal >
Tscal	shammodels::gsph::gsph_energy_rate (Tscal m_b, Tscal p_star, Tscal v_star, Tscal rho_a_sq, Tscal rho_b_sq, Tscal omega_a, Tscal omega_b, Tvec v_a, Tvec r_ab_unit, Tvec nabla_W_a, Tvec nabla_W_b)
	Compute GSPH energy equation contribution.

template<class Tvec , class Tscal >
void	shammodels::gsph::add_gsph_force_contribution (Tscal m_b, Tscal p_star, Tscal v_star, Tscal rho_a, Tscal rho_b, Tscal omega_a, Tscal omega_b, Tscal Fab_a, Tscal Fab_b, Tvec r_ab_unit, Tvec v_a, Tvec &dv_dt, Tscal &du_dt)
	Add GSPH force contribution from a single neighbor pair.

Detailed Description

GSPH force computation using Riemann solver results.

Author: Guo Yansong (guo.y.nosp@m.anso.nosp@m.ng.ng.nosp@m.y@gm.nosp@m.ail.c.nosp@m.om); Timothée David–Cléris (tim.s.nosp@m.hamr.nosp@m.ock@p.nosp@m.roto.nosp@m.n.me); Yona Lapeyre (yona..nosp@m.lape.nosp@m.yre@e.nosp@m.ns-l.nosp@m.yon.f.nosp@m.r)

Implements the Godunov SPH (GSPH) force formulation following Cha & Whitworth (2003). The key difference from standard SPH is that the interface pressure p* comes from solving the Riemann problem, rather than using artificial viscosity.

References:

Cha, S.-H. & Whitworth, A.P. (2003) "Implementations and tests of Godunov-type particle hydrodynamics"
Inutsuka, S. (2002) "Reformulation of Smoothed Particle Hydrodynamics with Riemann Solver"

Definition in file forces.hpp.

Function Documentation

◆ add_gsph_force_contribution()

template<class Tvec , class Tscal >

void shammodels::gsph::add_gsph_force_contribution	(	Tscal	m_b,
		Tscal	p_star,
		Tscal	v_star,
		Tscal	rho_a,
		Tscal	rho_b,
		Tscal	omega_a,
		Tscal	omega_b,
		Tscal	Fab_a,
		Tscal	Fab_b,
		Tvec	r_ab_unit,
		Tvec	v_a,
		Tvec &	dv_dt,
		Tscal &	du_dt
	)

inline

Add GSPH force contribution from a single neighbor pair.

Convenience function that computes both acceleration and energy rate contributions from a single particle pair, given the Riemann solver result.

Template Parameters

Tvec	Vector type
Tscal	Scalar type

Parameters

	m_b	Mass of neighbor particle
	p_star	Interface pressure from Riemann solver
	v_star	Interface velocity from Riemann solver
	rho_a	Density of particle a
	rho_b	Density of particle b
	omega_a	Grad-h correction factor for particle a
	omega_b	Grad-h correction factor for particle b
	Fab_a	Kernel gradient magnitude \|nabla W_ab(h_a)\|
	Fab_b	Kernel gradient magnitude \|nabla W_ab(h_b)\|
	r_ab_unit	Unit vector from a to b (points toward b)
	v_a	Velocity of particle a
[out]	dv_dt	Accumulated acceleration
[out]	du_dt	Accumulated energy rate

Definition at line 119 of file forces.hpp.

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◆ gsph_energy_rate()

template<class Tvec , class Tscal >

Tscal shammodels::gsph::gsph_energy_rate	(	Tscal	m_b,
		Tscal	p_star,
		Tscal	v_star,
		Tscal	rho_a_sq,
		Tscal	rho_b_sq,
		Tscal	omega_a,
		Tscal	omega_b,
		Tvec	v_a,
		Tvec	r_ab_unit,
		Tvec	nabla_W_a,
		Tvec	nabla_W_b
	)

inline

Compute GSPH energy equation contribution.

Following Cha & Whitworth (2003), the energy equation uses the same symmetric force as the momentum equation: f_ab = m_b * p* * (nabla_W_a / (rho_a^2 * Omega_a) + nabla_W_b / (rho_b^2 * Omega_b)) du_a/dt = -f_ab dot (v* - v_a)

This ensures proper energy conservation in shocks by using the same force that appears in the momentum equation.