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Peano
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Peano
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#include <config.h>#include "adaptive_softening_struct.h"#include "inline.h"#include "kernel_hydro.h"
Go to the source code of this file.
Functions | |
| __attribute__ ((always_inline)) INLINE static void adaptive_softening_add_correction_term(struct part *pi | |
| Computes the contribution to the softening length change term. | |
Variables | |
| const float | ui = r * h_inv |
| const float const float | hi_inv |
| __attribute__ | ( | (always_inline) | ) |
Computes the contribution to the softening length change term.
Computes the kernel function derivative.
Computes the kernel function in double precision.
Computes the kernel function.
Calculate the gradient interaction between particle i and particle j.
Density interaction between two particles (non-symmetric).
Update the value of the viscosity alpha for the scheme.
Correct the signal velocity of the particle partaking in supernova (kinetic) feedback based on the velocity kick the particle receives.
Sets the drifted physical internal energy of a particle.
Sets the physical internal energy of a particle.
Sets the physical entropy of a particle.
Sets the time derivative of the co-moving internal energy of a particle.
Returns the time derivative of internal energy of a particle.
Returns the time derivative of co-moving internal energy of a particle.
Sets the mass of a particle.
Returns the mass of a particle.
Returns the comoving density of a particle.
Returns the physical sound speed of a particle.
Returns the comoving sound speed of a particle.
Returns the physical entropy of a particle drifted to the current time.
Returns the comoving entropy of a particle drifted to the current time.
Returns the physical entropy of a particle at the last time the particle was kicked.
Returns the comoving entropy of a particle at the last time the particle was kicked.
Returns the physical pressure of a particle.
Returns the comoving pressure of a particle.
Returns the physical internal energy of a particle drifted to the current time.
Returns the comoving internal energy of a particle drifted to the current time.
Returns the physical internal energy of a particle at the last time the particle was kicked.
Get the radius of a dimension sphere with the given volume.
Inverts the given dimension by dimension matrix (in place)
Returns the argument to the power given by the dimension minus one.
Returns the argument to the power given by the dimension plus one.
Returns the argument to the power given by the inverse of the dimension.
No adaptive softening --> Nothing to do.
| pi | The part for which we compute terms. |
| ui | The ratio of the inter-particle distance to the smoothing length. |
| hi_inv | The inverse the particle's smoothing length. |
| mj | The mass of the other particle. |
Computes \(x^{1/d}\).
Computes \(x^{d+1}\).
Computes \(x^{d-1}\).
| A | A 3x3 matrix of which we want to invert the top left dxd part |
| volume | Volume of the dimension sphere |
| p | The particle of interest. |
| xp | The extended data of the particle of interest. |
| cosmo | The cosmological model. |
| p | The particle of interest |
| p | The particle of interest. |
| cosmo | The cosmological model. |
Computes the pressure based on the particle's properties.
| p | The particle of interest |
Computes the pressure based on the particle's properties and convert it to physical coordinates.
| p | The particle of interest |
| cosmo | The cosmological model. |
| p | The particle of interest. |
| xp | The extended data of the particle of interest. |
| p | The particle of interest. |
| p | The particle of interest |
| cosmo | The cosmological model. |
| p | The particle of interest |
| m | The mass to set. |
We assume a constant density.
| p | The particle of interest |
We assume a constant density.
| p | The particle of interest |
| cosmo | Cosmology data structure |
We assume a constant density for the conversion to entropy.
| p | The particle of interest. |
| du_dt | The new time derivative of the internal energy. |
We assume a constant density.
| p | The particle of interest. |
| cosmo | Cosmology data structure |
| du_dt | The new time derivative of the internal energy. |
| p | The particle of interest. |
| xp | The extended particle data. |
| cosmo | Cosmology data structure |
| entropy | The physical entropy |
| p | The particle of interest. |
| xp | The extended particle data. |
| cosmo | Cosmology data structure |
| u | The physical internal energy |
| p | The particle of interest. |
| cosmo | Cosmology data structure |
| u | The physical internal energy |
| p | The particle of interest. |
| cosmo | Cosmology data structure |
| dv_phys | The velocity kick received by the particle expressed in physical units (note that dv_phys must be positive or equal to zero) |
| p | the particle of interest |
| alpha | the new value for the viscosity coefficient. |
| r2 | Comoving square distance between the two particles. |
| dx | Comoving vector separating both particles (pi - pj). |
| hi | Comoving smoothing-length of particle i. |
| hj | Comoving smoothing-length of particle j. |
| pi | First particle. |
| pj | Second particle (not updated). |
| a | Current scale factor. |
| H | Current Hubble parameter. |
Nothing to do here in this scheme.
| r2 | Comoving squared distance between particle i and particle j. |
| dx | Comoving distance vector between the particles (dx = pi->x - pj->x). |
| hi | Comoving smoothing-length of particle i. |
| hj | Comoving smoothing-length of particle j. |
| pi | Particle i. |
| pj | Particle j. |
| a | Current scale factor. |
| H | Current Hubble parameter. |
The kernel function needs to be mutliplied by \(h^{-d}\), where \(d\) is the dimensionality of the problem.
Returns 0 if \(u > \gamma = H/h\)
| u | The ratio of the distance to the smoothing length \(u = x/h\). |
| W | (return) The value of the kernel function \(W(x,h)\). |
Required for computing the projected kernel because rounding error causes problems for the GSL integration function if we evaluate in single precision.
The kernel function needs to be mutliplied by \(h^{-d}\), where \(d\) is the dimensionality of the problem.
Returns 0 if \(u > \gamma = H/h\)
| u | The ratio of the distance to the smoothing length \(u = x/h\). |
| W | (return) The value of the kernel function \(W(x,h)\). |
The kernel function needs to be mutliplied by \(h^{-d}\) and the gradient by \(h^{-(d+1)}\), where \(d\) is the dimensionality of the problem.
Returns 0 if \(u > \gamma = H/h\).
| u | The ratio of the distance to the smoothing length \(u = x/h\). |
| dW_dx | (return) The norm of the gradient of \(|\nabla W(x,h)|\). |
Definition at line 98 of file dimension.h.
| const float const float hi_inv |
Definition at line 101 of file adaptive_softening_iact.h.
Referenced by swift2::kernels::legacy::density_kernel().
Definition at line 100 of file adaptive_softening_iact.h.
1.10.0