ele2.c

#include <stdio.h>
#include <stdlib.h>
#include <math.h>
#include "philsp.h"

//------------------------------------------------------------------------

// We will use units of
//         Astronomical Units for length
//         Solar Masses for mass
//         1/(2 Pi) Earth Year for time
#define GGRAV 4*M_PI*M_PI

// NBODMX is the maximum number of bodies (masses) for which
// to provide space
#define NBODMX 403

// NDIM is the number of spatial dimensions to use
#define NDIM 2

// MAP is a function to map x[i][l] and v[i][l] to the
// single, one-dimensional, one-offset (y[1..N]) array
// used by odeint, below
//    k=0 corresponds to position, k=1 to velocity
//    l=0 is X, l=1 is Y, and l=2 is Z direction (l=2 only if NDIM is 3)
//    i is the body number
// Given a set (i,l,k), MAP(i,l,k) produces a unique index into the array
#define MAP(i,l,k) (1+l*(NDIM-1)+k*NDIM+i*NDIM*2)

// these are mnemonics to use with MAP
// so, for example, the Y velocity of body i is foo[MAP(i,Y,V)]
#define X 0
#define Y 1
#define Z 2
#define R 0
#define V 1

//------------------------------------------------------------------------

// number of masses
int nbodies;
// number of massive bodies
int nmass;
// position and velocity
double x[NBODMX][NDIM], v[NBODMX][NDIM];
// mass
double m[NBODMX];
// semimajor axis, eccentricity of orbits
double semi[NBODMX], eccen[NBODMX];
// energy variables
double energy, penergy, kenergy;
// total angular momentum vector
double l_tot[3];
// semi-major axis and eccentricity
double semi[NBODMX], eccen[NBODMX];

//------------------------------------------------------------------------

// function prototypes to use odeint routine below
void derivs(double t, double *x, double *dx);
void bsstep(double y[], double dydx[], int nv, double *xx, double htry,
            double eps, double yscal[], double *hdid, double *hnext,
            void (*derivs)(double, double [], double []));

//------------------------------------------------------------------------

// In the following code, loop variables i and j are used for body number
//                                       l is used for direction


// compute derivatives
//    odeint gives us the independent variable (here called t),
//      and the values of the dependent variables (here called f)
//    it expects us to compute the derivatives of these variables
//      and return them in the array df
//    f and df are one-offset, one-dimensional vectors
//    we use the MAP definition above to translate between this and
//      a more meaningful notation

void derivs(double t, double *f, double *df) {
  int i, j, l;
  double dr[NDIM];
  double rij, rij2, rij3;

  // zero the derivatives
  for(i=0; i<nbodies; i++) {
    for(l=0; l<NDIM; l++) {
      df[MAP(i,l,R)] = 0;   // position derivative w/r to time
      df[MAP(i,l,V)] = 0;   // velocity derivative w/r to time
    }
  }

  // zero potential energy
  penergy = 0;

  // Loop over all bodies to compute the derivatives
  for(i=0; i<nbodies; i++) {

    // compute velocity derivative (aka acceleration!)
    // sum the acceleration due to all other bodies j

// NOTE CHANGE HERE
    // If we only take the nmass bodies of large mass into account,
    // the problem will run much faster
    for(j=0; j<nmass; j++) {

      // self-acceleration not allowed!
      if(i!=j) {
        // get displacement vector
        for(l=0; l<NDIM; l++) dr[l] = f[MAP(i,l,0)] - f[MAP(j,l,0)];
        // get distance
        rij2 = 0;
        for(l=0; l<NDIM; l++) rij2 += dr[l]*dr[l];
        rij = sqrt(rij2);
        rij3 = rij*rij*rij;
        // the acceleration of body i due to body j
        for(l=0; l<NDIM; l++) df[MAP(i,l,V)] -= GGRAV * m[j] *dr[l] / rij3;
        // while we have the data handy, compute the potential energy
        penergy += GGRAV*m[i]*m[j]/rij;
      }
    }

    // compute position derivative (aka velocity!)
    for(l=0; l<NDIM; l++) df[MAP(i,l,R)] = f[MAP(i,l,V)];
  }

  // the algorithm above double-counts (i.e. adds
  //   the constribution to the energy twice for each pair of bodies
  penergy = penergy/2.0;

}


// integrate the orbits
//    from time t1 to time t2 starting with timestep hguess,
//    keeping the solution relative accuracy to within tol
void orbit_int(double t1, double t2, double hguess, double tol) {
  static double y[NBODMX*NDIM*2];
  int i, l;
  int nok, nbad;
  double hmin;

  // odeint requires the minimum timestep allowed (can be zero)
  hmin = 1.0e-06*hguess;

  // load the initial conditions into the 1-based array for odeint
  for(i=0; i<nbodies; i++) {
    for(l=0; l<NDIM; l++) {
      y[MAP(i,l,R)] = x[i][l];
      y[MAP(i,l,V)] = v[i][l];
    }
  }

  // integrate the nbodies*NDIM*2 equations from t1 to t2
  odeint(y, nbodies*NDIM*2, t1, t2, tol, hguess, hmin, &nok, &nbad, derivs, bsstep);

  // now put the result back into our x and v arrays
  for(i=0; i<nbodies; i++) {
    for(l=0; l<NDIM; l++) {
      x[i][l] = y[MAP(i,l,R)];
      v[i][l] = y[MAP(i,l,V)];
    }
  }

}


// removes the center of mass velcity from the system
//    and put the center of mass at the origin
void remove_com() {
  int i, l;
  double vcom[NDIM], rcom[NDIM];
  double mtotal;

  // get total mass
  mtotal = 0.0;
  for(i=0; i<nbodies; i++) mtotal += m[i];

  // zero in preparation for summing
  for(l=0; l<NDIM; l++) {
    vcom[l] = 0.0;
    rcom[l] = 0.0;
  }

  // find center of mass position and velocity
  for(i=0; i<nbodies; i++) {
    for(l=0; l<NDIM; l++) {
      rcom[l] += m[i]*x[i][l]/mtotal;
      vcom[l] += m[i]*v[i][l]/mtotal;
    }
  }

  // subtract from the bodies
  for(i=0; i<nbodies; i++) {
    for(l=0; l<NDIM; l++) {
      x[i][l] -= rcom[l];
      v[i][l] -= vcom[l];
    }
  }

}

// rotate the 2D vector v clockwise through angle
//    theta (in radians)
void rotate_2vector(double *v, double t) {
  int l, ll;
  double rmat[2][2], vtmp[2];

  // make the rotation matrix
  //
  //  cos(t)    sin(t)
  // -sin(ta)   cos(t)

  rmat[0][0] = rmat[1][1] = cos(t);
  rmat[0][1] = sin(t);
  rmat[1][0] = -rmat[0][1];

  // multiply the vector by the matrix
  for(l=0; l<2; l++) {
    vtmp[l] = 0;
    for(ll=0; ll<2; ll++) {
      vtmp[l] += v[ll]*rmat[ll][l];
    }
  }
  for(l=0; l<NDIM; l++) {
    v[l] = vtmp[l];
  }

}


// set the initial conditions
//    and the number of bodies
void initial_conditions() {
  int i;
  double r, dr, rmin, rmax;

  nbodies = 200;
  // we only need to take into account the gravitational
  // potential due to the first two masses
  nmass = 3;

  // Sun
  m[0] = 1.0;
  x[0][0] = 0.0;
  x[0][1] = 0.0;
  v[0][0] = 0.0;
  v[0][1] = 0.0;

  // Jupiter
  //    Jupiter is really 1.0e-03 solar masses but this makes
  //    the effects more readily apparent
  //    We use a circular orbit here.
  m[1] = 1.0e-02;
  x[1][0] = 5.2;
  x[1][1] = 0.0;
  v[1][0] = 0.0;
  v[1][1] = sqrt(GGRAV*m[0]/x[1][0]);

  //Mars
  m[2] = 1.0e-04;
  x[2][0] = 1.5;
  x[2][1] = 0.0;
  v[2][0] = 0.0;
  v[2][1] = sqrt(GGRAV*m[0]/x[2][0]);
  // now put in the remaining bodies as almost massless test particles
  //    between rmin and rmax
  rmin = 1.5;
  rmax = 5.2;
  dr = (rmax - rmin)/(double)(nbodies-2);
  for(i=3; i<nbodies; i++) {

    // radius to put asteroid
    r = rmin + (i-2)*dr;

    // set up the particle on the y-axis with negative x velocity
    m[i] = 1.0e-20;
    x[i][0] = 0;
    x[i][1] = r;
    v[i][0] = -sqrt(GGRAV*m[0]/r);
    v[i][1] = 0.0;
  }


  // put system in its center of mass coordinates
  remove_com();

}


// compute conserved quantities
void conservation() {
  int i, l;
  double v2;

  // we have potential energy from derivs, above
  // get kinetic energy here
  kenergy = 0.0;
  for(i=0; i<nbodies; i++) {
    v2 = 0.0;
    for(l=0; l<NDIM; l++) v2 += v[i][l]*v[i][l];
    kenergy += m[i]*v2/2.0;
  }

  // total energy
  energy = kenergy + penergy;

  // get angular momentum
  // for NDIM of 1, there is no angular momentum
  for(l=0; l<3; l++) l_tot[l] = 0.0;
#if (NDIM>1)
  // for NDIM of 2, the angular momentum vector points out of the plane
  //    so we need only one component
  for(i=0; i<nbodies; i++) {
    l_tot[2] += m[i] * (x[i][0]*v[i][1] - x[i][1]*v[i][0]);
#if (NDIM==3)
    // for NDIM of 3, we need all three components of the angular momentum
    l_tot[1] += m[i] * (x[i][2]*v[i][0] - x[i][0]*v[i][2]);
    l_tot[0] += m[i] * (x[i][1]*v[i][2] - x[i][2]*v[i][1]);

#endif
  }
#endif

  // for the two-dimensional version
  //printf("conservation: %12.5e  %12.5e\n", energy, l_tot[2]);


}


// compute orbital elements for the asteroids
//    Note that the definition of the eccentricity is not
//    really correct
void orbital_elements() {
  int i, j, l;
  double r, v2, e, L, p;

  for(i=nmass; i<nbodies; i++) {

    // compute the potential energy due to the Sun
    //    get the separation from the Sun
    r = 0;
    for(l=0; l<NDIM; l++) r += pow(x[i][l] - x[0][l],2);
    r = sqrt(r);
    //    compute the potential energy
    p = - GGRAV * m[0] * m[i] / r;

    // get the kinetic energy
    v2 = 0;
    for(l=0; l<NDIM; l++) v2 += pow(v[i][l],2);

    // the total energy
    e = m[i]*v2/2.0 + p;

    // the angular momentum
    L = m[i] * (x[i][0]*v[i][1] - x[i][1]*v[i][0]);

    // if the particle is bound (i.e. has negative energy)
    //    compute the osculating element
    if(e<0) {
      // semi-major axis
      semi[i] = -GGRAV*m[0]*m[i]/(2.0*e);
      // eccentricity squared (which can nonetheless be negative!)
      eccen[i] = 1 - L*L/(GGRAV*m[0]*m[i]*m[i]*semi[i]);
      //printf("semi= %12.5e eccen= %12.5e\n", semi[i], eccen[i]);
    }
    else {
      semi[i] = 0.0;
      eccen[i] = 0.0;
    }
  }


}

//------------------------------------------------------------------------


int main() {
  int i, k, n, nplot;
  double t, step, hguess, tol;
  double size, psize;

  // set up the plotting window
  open_plot("800x800");

  // the size of the points to plot
  psize = 0.75;

  // plot every nplot calls to odeint
  nplot = 1;
  n = 0;

  // the limits of the box
  size = 6.9;
  box_plot(-size,size,-size,size,1.5,1,"","","","");
  flush_plot();

  // set up the problem
  t = 0;
  initial_conditions();

  // each call to odeint advances by this time
  step = 1.0e-1;
  // start with this timestep inside odeint
  hguess = step/1.0e+3;
  // keep solution relative accuracy to this
  tol = 1.0e-05;

  // loop over time
  for(k=0; k<100000; k++) {

    // integrate from t to t+step
    orbit_int(t, t+step, hguess, tol);
    t += step;

    n++;
    if(n==nplot) {
      n = 0;

      // draw the massive bodies
      for(i=0; i<nmass; i++) {
        putpoint_plot(x[i][0],x[i][1],10,1,2,psize,0);
      }
      // draw the test particles
      for(i=nmass; i<nbodies; i++) {
        putpoint_plot(x[i][0],x[i][1],10,1,2,0.25,0);
      }
      // paint the screen
      flush_plot();
      // erase the points in preparation for next time
      for(i=0; i<nmass; i++) {
        putpoint_plot(x[i][0],x[i][1],10,1,0,psize,0);
      }
      for(i=nmass; i<nbodies; i++) {
        putpoint_plot(x[i][0],x[i][1],10,1,0,0.25,0);
      }
      // compute and print out the conserved quantities
      conservation();
    }

  }

  // all done
  return 0;
}