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/*
* Constructor of class Mag_NS (magnetized neutron star exportation)
* which depends explicitely on Lorene objects.
*
* (see file mag_ns.h for documentation).
*/
/*
* Copyright (c) 2002 Eric Gourgoulhon
* Copyright (c) 2009 Jerome Novak
*
* This file is part of LORENE.
*
* LORENE is free software; you can redistribute it and/or modify
* it under the terms of the GNU General Public License version 2
* as published by the Free Software Foundation.
*
* LORENE is distributed in the hope that it will be useful,
* but WITHOUT ANY WARRANTY; without even the implied warranty of
* MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the
* GNU General Public License for more details.
*
* You should have received a copy of the GNU General Public License
* along with LORENE; if not, write to the Free Software
* Foundation, Inc., 59 Temple Place, Suite 330, Boston, MA 02111-1307 USA
*
*/
char mag_ns_aux_C[] = "$Header: /cvsroot/Lorene/Export/C++/Source/mag_ns_aux.C,v 1.4 2016/02/17 09:46:35 j_novak Exp $" ;
/*
* $Id: mag_ns_aux.C,v 1.4 2016/02/17 09:46:35 j_novak Exp $
* $Log: mag_ns_aux.C,v $
* Revision 1.4 2016/02/17 09:46:35 j_novak
* u_euler output in units of c.
*
* Revision 1.3 2014/10/13 08:54:06 j_novak
* Lorene classes and functions now belong to the namespace Lorene.
*
* Revision 1.2 2014/05/13 10:06:45 j_novak
* Update to take unto account the change in Lorene magnetic units.
*
* Revision 1.1 2009/11/19 16:15:21 j_novak
* Export class for magnetized neutron stars.
*
*
* $Header: /cvsroot/Lorene/Export/C++/Source/mag_ns_aux.C,v 1.4 2016/02/17 09:46:35 j_novak Exp $
*
*/
#include "../Include/mag_ns.h"
// C headers
#include <cstring>
#include <cmath>
// Lorene headers
#include "tenseur.h"
#include "et_rot_mag.h"
#include "eos.h"
#include "unites.h"
#include "metric.h"
#include "utilitaires.h"
//----------------------------------------//
// Constructor from LORENE data //
//----------------------------------------//
namespace Lorene {
Mag_NS::Mag_NS(int nbpoints, const double* xi, const double* yi,
const double* zi, const char* filename)
: np(nbpoints) {
using namespace Unites ;
using namespace Unites_mag ;
// Reading of data
// ---------------
FILE* fich = fopen(filename, "r") ;
Mg3d spectral_grid(fich) ;
int nphi = spectral_grid.get_np(0) ;
if (nphi < 4) {
cout << "Contructor of Mag_NS: " << endl ;
cout << "Fatal problem with initial data, "<< endl ;
cout << "the number of points in the phi direction is lower than 4."
<< endl ;
cout << "Impossible to rotate tensors to Cartesian triad. Please give as"
<< endl ;
cout << "an input a result file from magstar with nphi >=4." << endl ;
abort() ;
}
Map_et mapping(spectral_grid, fich) ;
Eos* p_eos = Eos::eos_from_file(fich) ;
Et_rot_mag star(mapping, *p_eos, fich) ;
star.equation_of_state() ;
star.update_metric() ;
star.extrinsic_curvature() ;
star.hydro_euler() ;
const Map& mp = star.get_mp();
const Base_vect_spher& bspher = mp.get_bvect_spher() ;
Sym_tensor gij(mp, COV, bspher) ;
gij.set_etat_zero() ;
gij.set(1,1) = star.get_a_car()() ;
gij.set(2,2) = star.get_a_car()() ;
gij.set(3,3) = star.get_b_car()() ;
Metric gam(gij) ; //the 3-metric in quasi-isotropic coordinates
// Initialisation of member data
// -----------------------------
const Eos_poly* p_eos_poly = dynamic_cast<const Eos_poly*>( p_eos ) ;
double m_0 = 1. ;
if ( p_eos_poly != 0x0 ) {
strcpy(eos_name, "Polytropic EOS") ;
gamma_poly = p_eos_poly->get_gam() ;
kappa_poly = p_eos_poly->get_kap() ;
m_0 = p_eos_poly->get_m_0() ;
}
else {
strncpy(eos_name, (star.get_eos()).get_name(), 100) ;
gamma_poly = 0 ;
kappa_poly = 0 ;
cout << "Mag_NS::Mag_NS : not a ploytropic EOS" << endl ;
cout << "WARNING!!" << endl ;
cout << "exporting the baryon density instead of the mass density!" << endl ;
arrete() ;
}
Scalar sp_density = m_0 * star.get_nbar()()*rho_unit ;
Scalar sp_energy = star.get_ener()() * rho_unit;
omega = star.get_omega_c() * f_unit ;
rho_c = m_0*sp_density.val_grid_point(0,0,0,0) ;
eps_c = sp_energy.val_grid_point(0,0,0,0) / rho_c - 1. ;
mass_b = star.mass_b() / msol ;
mass_g = star.mass_g() / msol ;
r_eq = star.ray_eq() / km ;
r_p = star.ray_pole() / km ;
angu_mom = star.angu_mom() / ( ggrav * msol*msol) ;
T_over_W = star.tsw() ;
magn_mom = star.MagMom() ;
b_z_pole =
star.Magn()(0).va.val_point(star.l_surf()(0,0), star.xi_surf()(0,0),0.,0.)
* mag_unit / 1.e9 ;
int theta_eq = mapping.get_mg()->get_nt(star.get_nzet() - 1) - 1 ;
b_z_eq = star.Magn()(1).va.val_point(star.l_surf()(0,theta_eq),
star.xi_surf()(0,theta_eq),M_PI_2,0.)
* mag_unit / 1.e9 ;
cout.precision(13) ;
cout << endl << "Magnetized star read in file : " << endl ;
cout << "------------------------------ " << endl ;
cout << star << endl ;
cout << endl << "Summary : " << endl ;
cout << "-------" << endl ;
cout << " Omega : " << omega << " rad/s" << endl ;
cout << " Baryon mass : " << mass_b
<< " M_sol" << endl ;
cout << " Gravitational mass : " << mass_g
<< " M_sol" << endl ;
cout << " Equatorial radius : " << r_eq
<< " km" << endl ;
cout << " Polar radius : " << r_p
<< " km" << endl ;
cout << " Total angular momentum : " << angu_mom
<< " G M_sol^2 / c" << endl ;
cout << " T/W : " << T_over_W << endl ;
cout << " Magnetic momentum : " << magn_mom
<< " A/m^2" << endl ;
cout << " Radial magnetic field polar value : " << b_z_pole
<< " GT" << endl ;
cout << " Tangent magnetic field equatorial value : " << b_z_eq
<< " GT" << endl ;
// Creation of the various arrays on the Cartesian grid
// ----------------------------------------------------
alloc_memory() ;
// Initialisation of the Cartesian grid
// ------------------------------------
for (int i=0; i<np; i++) {
xx[i] = xi[i] ;
}
for (int i=0; i<np; i++) {
yy[i] = yi[i] ;
}
for (int i=0; i<np; i++) {
zz[i] = zi[i] ;
}
// Computation of the values at the points of the Cartesian grid
// -------------------------------------------------------------
assert(star.is_relativistic()) ;
Scalar sp_lapse = star.get_nnn()() ;
Vector sp_shift(mapping, CON, mapping.get_bvect_cart()) ;
sp_shift.set(1) = star.get_shift()(0) ; //contravariant representation!!
sp_shift.set(2) = star.get_shift()(1) ;
sp_shift.set(3) = star.get_shift()(2) ;
Sym_tensor sp_gamma(mapping, COV, mapping.get_bvect_spher()) ;
sp_gamma.set_etat_qcq() ;
for (int i=1; i<=3; i++) {
for (int j=1; j<=i; j++)
sp_gamma.set(i,j) = 0 ;
if (i != 3) sp_gamma.set(i,i) = star.get_a_car()() ;
else sp_gamma.set(3,3) = star.get_bbb()()*star.get_bbb()() ;
}
sp_gamma.change_triad(mapping.get_bvect_cart()) ;
Sym_tensor sp_kij(mapping, COV, mapping.get_bvect_cart()) ;
sp_kij.set_etat_qcq() ;
for (int i=0; i<3; i++)
for (int j=i; j<3; j++) {
sp_kij.set(i+1, j+1) =
star.get_bbb()()*star.get_bbb()()*star.get_tkij()(i,j) / r_unit ;
sp_kij.set(i+1, j+1).dec_dzpuis(2) ;
}
Vector sp_u_euler(mapping, CON, mapping.get_bvect_cart()) ;
sp_u_euler.set(1) = star.get_u_euler()(0) ;
sp_u_euler.set(2) = star.get_u_euler()(1) ;
sp_u_euler.set(3) = star.get_u_euler()(2) ;
Vector sp_current(mp, CON, mapping.get_bvect_spher()) ;
sp_current.set(1) = 0 ;
sp_current.set(2) = 0 ;
sp_current.set(3) = Scalar(star.get_jphi()*j_unit) ;
sp_current.set(3).mult_rsint() ;
sp_current.change_triad(mapping.get_bvect_cart()) ;
Scalar sp_jt = star.get_jt() * j_unit ;
Scalar fac = 1.e9*sqrt(star.get_a_car()())/mag_unit ;//to transform B^(i) into B^i
fac.std_spectral_base() ;
Vector sp_Bmag(mp, CON, bspher) ;
sp_Bmag.set(1) = Scalar(star.Magn()(0)) / fac ;
sp_Bmag.set(1).dec_dzpuis(2) ;
sp_Bmag.set(2) = Scalar(star.Magn()(1)) / fac ;
sp_Bmag.set(2).dec_dzpuis(2) ;
sp_Bmag.set(3) = 0 ;
sp_Bmag.change_triad(mapping.get_bvect_cart()) ;
for (int i=0; i<np; i++) {
double x0 = xx[i] * km ; // x, y, z in Lorene's unit
double y0 = yy[i] * km ;
double z0 = zz[i] * km ;
// Values of (l, xi, theta, phi) corresponding to (x,y,z):
// -------------------------------------------------------
double r, theta, phi ; // polar coordinates centered on the star
mapping.convert_absolute(x0, y0, z0, r, theta, phi) ;
// Lapse function
// --------------
nnn[i] = sp_lapse.val_point(r, theta, phi) ;
// Shift vector
// ------------
beta_x[i] = sp_shift(1).val_point(r, theta, phi) ;
beta_y[i] = sp_shift(2).val_point(r, theta, phi) ;
beta_z[i] = sp_shift(3).val_point(r, theta, phi) ;
// 3-metric
// ---------
g_xx[i] = sp_gamma(1,1).val_point(r, theta, phi) ;
g_yy[i] = sp_gamma(2,2).val_point(r, theta, phi) ;
g_zz[i] = sp_gamma(3,3).val_point(r, theta, phi) ;
g_xy[i] = sp_gamma(1,2).val_point(r, theta, phi) ;
g_xz[i] = sp_gamma(1,3).val_point(r, theta, phi) ;
g_yz[i] = sp_gamma(2,3).val_point(r, theta, phi) ;
// Extrinsic curvature
// -------------------
k_xx[i] = sp_kij(1,1).val_point(r, theta, phi) ;
k_xy[i] = sp_kij(1,1).val_point(r, theta, phi) ;
k_xz[i] = sp_kij(1,1).val_point(r, theta, phi) ;
k_yy[i] = sp_kij(1,1).val_point(r, theta, phi) ;
k_yz[i] = sp_kij(1,1).val_point(r, theta, phi) ;
k_zz[i] = sp_kij(1,1).val_point(r, theta, phi) ;
// Baryon density [kg/m^3]
// --------------
nbar[i] = sp_density.val_point(r, theta, phi) ;
// Energy density
// --------------
double ener = sp_energy.val_point(r, theta, phi) ;
if ( nbar[i] == double(0) ) {
ener_spec[i] = 0 ;
}
else {
ener_spec[i] = ener / nbar[i] - double(1) ;
}
// 3-velocity with respect to the Eulerian observer
// ------------------------------------------------
u_euler_x[i] = sp_u_euler(1).val_point(r, theta, phi) ;
u_euler_y[i] = sp_u_euler(2).val_point(r, theta, phi) ;
u_euler_z[i] = sp_u_euler(3).val_point(r, theta, phi) ;
// Magnetic field
//---------------
bb_x[i] = sp_Bmag(1).val_point(r, theta, phi) ;
bb_y[i] = sp_Bmag(2).val_point(r, theta, phi) ;
bb_z[i] = sp_Bmag(3).val_point(r, theta, phi) ;
// 4-current
//----------
jj_t[i] = sp_jt.val_point(r, theta, phi) ;
jj_x[i] = sp_current(1).val_point(r, theta, phi) ;
jj_y[i] = sp_current(2).val_point(r, theta, phi) ;
jj_z[i] = sp_current(3).val_point(r, theta, phi) ;
} // End of loop on the points
delete p_eos ;
}
}
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