void
pstime(double d)
{
setime(d);
semi = 0;
motion = 0;
rad = 1.e9;
lambda = 0;
beta = 0;
// uses lambda, beta, rad, motion
// sets alpha, delta, rp
helio();
// uses alpha, delta, rp
// sets ra, decl, lha, decl2, az, el
geo();
print(" %R %D %D %4.0f", lha, nlat, awlong, elev/3.28084);
}
void
venus(void)
{
double pturbl, pturbb, pturbr;
double lograd;
double dele, enom, vnom, nd, sl;
double v0, t0, m0, j0, s0;
double lsun, elong, ci, dlong;
/*
* here are the mean orbital elements
*/
ecc = .00682069 - .00004774*capt + 0.091e-6*capt2;
incl = 3.393631 + .0010058*capt - 0.97e-6*capt2;
node = 75.779647 + .89985*capt + .00041*capt2;
argp = 130.163833 + 1.408036*capt - .0009763*capt2;
mrad = .7233316;
anom = 212.603219 + 1.6021301540*eday + .00128605*capt2;
motion = 1.6021687039;
/*
* mean anomalies of perturbing planets
*/
v0 = 212.60 + 1.602130154*eday;
t0 = 358.63 + .985608747*eday;
m0 = 319.74 + 0.524032490*eday;
j0 = 225.43 + .083090842*eday;
s0 = 175.8 + .033459258*eday;
v0 *= radian;
t0 *= radian;
m0 *= radian;
j0 *= radian;
s0 *= radian;
incl *= radian;
node *= radian;
argp *= radian;
anom = fmod(anom, 360.)*radian;
/*
* computation of long period terms affecting the mean anomaly
*/
anom +=
(2.761-0.022*capt)*radsec*sin(
13.*t0 - 8.*v0 + 43.83*radian + 4.52*radian*capt)
+ 0.268*radsec*cos(4.*m0 - 7.*t0 + 3.*v0)
+ 0.019*radsec*sin(4.*m0 - 7.*t0 + 3.*v0)
- 0.208*radsec*sin(s0 + 1.4*radian*capt);
/*
* computation of elliptic orbit
*/
enom = anom + ecc*sin(anom);
do {
dele = (anom - enom + ecc * sin(enom)) /
(1 - ecc*cos(enom));
enom += dele;
} while(fabs(dele) > converge);
vnom = 2*atan2(sqrt((1+ecc)/(1-ecc))*sin(enom/2),
cos(enom/2));
rad = mrad*(1 - ecc*cos(enom));
lambda = vnom + argp;
/*
* perturbations in longitude
*/
icosadd(venfp, vencp);
pturbl = cosadd(4, v0, t0, m0, j0);
pturbl *= radsec;
/*
* perturbations in latidude
*/
pturbb = cosadd(3, v0, t0, j0);
pturbb *= radsec;
/*
* perturbations in log radius vector
*/
pturbr = cosadd(4, v0, t0, m0, j0);
/*
* reduction to the ecliptic
*/
lambda += pturbl;
nd = lambda - node;
lambda = node + atan2(sin(nd)*cos(incl),cos(nd));
sl = sin(incl)*sin(nd);
beta = atan2(sl, pyth(sl)) + pturbb;
lograd = pturbr*2.30258509;
rad *= 1 + lograd;
motion *= radian*mrad*mrad/(rad*rad);
/*
* computation of magnitude
*/
lsun = 99.696678 + 0.9856473354*eday;
lsun *= radian;
elong = lambda - lsun;
ci = (rad - cos(elong))/sqrt(1 + rad*rad - 2*rad*cos(elong));
dlong = atan2(pyth(ci), ci)/radian;
mag = -4 + .01322*dlong + .0000004247*dlong*dlong*dlong;
semi = 8.41;
helio();
geo();
}
void
star(void)
{
double xm, ym, zm, dxm, dym, dzm;
double xx, yx, zx, yy, zy, zz, tau;
double capt0, capt1, capt12, capt13, sl, sb, cl;
/*
* remove E-terms of aberration
* except when finding catalog mean places
*/
alpha += (.341/(3600.*15.))*sin((alpha+11.26)*15.*radian)
/cos(delta*radian);
delta += (.341/3600.)*cos((alpha+11.26)*15.*radian)
*sin(delta*radian) - (.029/3600.)*cos(delta*radian);
/*
* correct for proper motion
*/
tau = (eday - epoch)/365.24220;
alpha += tau*da/3600.;
delta += tau*dd/3600.;
alpha *= 15.*radian;
delta *= radian;
/*
* convert to rectangular coordinates merely for convenience
*/
xm = cos(delta)*cos(alpha);
ym = cos(delta)*sin(alpha);
zm = sin(delta);
/*
* convert mean places at epoch of startable to current
* epoch (i.e. compute relevant precession)
*/
capt0 = (epoch - 18262.427)/36524.220e0;
capt1 = (eday - epoch)/36524.220;
capt12 = capt1*capt1;
capt13 = capt12*capt1;
xx = - (.00029696+26.e-8*capt0)*capt12
- 13.e-8*capt13;
yx = -(.02234941+1355.e-8*capt0)*capt1
- 676.e-8*capt12 + 221.e-8*capt13;
zx = -(.00971690-414.e-8*capt0)*capt1
+ 207.e-8*capt12 + 96.e-8*capt13;
yy = - (.00024975+30.e-8*capt0)*capt12
- 15.e-8*capt13;
zy = -(.00010858+2.e-8*capt0)*capt12;
zz = - (.00004721-4.e-8*capt0)*capt12;
dxm = xx*xm + yx*ym + zx*zm;
dym = - yx*xm + yy*ym + zy*zm;
dzm = - zx*xm + zy*ym + zz*zm;
xm = xm + dxm;
ym = ym + dym;
zm = zm + dzm;
/*
* convert to mean ecliptic system of date
*/
alpha = atan2(ym, xm);
delta = atan2(zm, sqrt(xm*xm+ym*ym));
cl = cos(delta)*cos(alpha);
sl = cos(delta)*sin(alpha)*cos(obliq) + sin(delta)*sin(obliq);
sb = -cos(delta)*sin(alpha)*sin(obliq) + sin(delta)*cos(obliq);
lambda = atan2(sl, cl);
beta = atan2(sb, sqrt(cl*cl+sl*sl));
rad = 1.e9;
if(px != 0)
rad = 20600/px;
motion = 0;
semi = 0;
helio();
geo();
}
void
plut(void)
{
double pturbl, pturbb, pturbr;
double lograd;
double dele, enom, vnom, nd, sl;
double capj, capn, eye, comg, omg;
double sb, su, cu, u, b, up;
double sd, ca, sa;
double cy;
cy = (eday - elem[0]) / 36525.; /* per julian century */
mrad = elem[1] + elem[1+6]*cy;
ecc = elem[2] + elem[2+6]*cy;
cy = cy / 3600; /* arcsec/deg per julian century */
incl = elem[3] + elem[3+6]*cy;
node = elem[4] + elem[4+6]*cy;
argp = elem[5] + elem[5+6]*cy;
anom = elem[6] + elem[6+6]*cy - argp;
motion = elem[6+6] / 36525. / 3600;
incl *= radian;
node *= radian;
argp *= radian;
anom = fmod(anom,360.)*radian;
enom = anom + ecc*sin(anom);
do {
dele = (anom - enom + ecc * sin(enom)) /
(1. - ecc*cos(enom));
enom += dele;
} while(fabs(dele) > converge);
vnom = 2.*atan2(sqrt((1.+ecc)/(1.-ecc))*sin(enom/2.),
cos(enom/2.));
rad = mrad*(1. - ecc*cos(enom));
lambda = vnom + argp;
pturbl = 0.;
lambda += pturbl*radsec;
pturbb = 0.;
pturbr = 0.;
/*
* reduce to the ecliptic
*/
nd = lambda - node;
lambda = node + atan2(sin(nd)*cos(incl),cos(nd));
sl = sin(incl)*sin(nd) + pturbb*radsec;
beta = atan2(sl, pyth(sl));
lograd = pturbr*2.30258509;
rad *= 1. + lograd;
lambda -= 1185.*radsec;
beta -= 51.*radsec;
motion *= radian*mrad*mrad/(rad*rad);
semi = 83.33;
/*
* here begins the computation of magnitude
* first find the geocentric equatorial coordinates of Saturn
*/
sd = rad*(cos(beta)*sin(lambda)*sin(obliq) +
sin(beta)*cos(obliq));
sa = rad*(cos(beta)*sin(lambda)*cos(obliq) -
sin(beta)*sin(obliq));
ca = rad*cos(beta)*cos(lambda);
sd += zms;
sa += yms;
ca += xms;
alpha = atan2(sa,ca);
delta = atan2(sd,sqrt(sa*sa+ca*ca));
/*
* here are the necessary elements of Saturn's rings
* cf. Exp. Supp. p. 363ff.
*/
capj = 6.9056 - 0.4322*capt;
capn = 126.3615 + 3.9894*capt + 0.2403*capt2;
eye = 28.0743 - 0.0128*capt;
comg = 168.1179 + 1.3936*capt;
omg = 42.9236 - 2.7390*capt - 0.2344*capt2;
capj *= radian;
capn *= radian;
eye *= radian;
comg *= radian;
omg *= radian;
/*
* now find saturnicentric ring-plane coords of the earth
*/
sb = sin(capj)*cos(delta)*sin(alpha-capn) -
cos(capj)*sin(delta);
su = cos(capj)*cos(delta)*sin(alpha-capn) +
sin(capj)*sin(delta);
cu = cos(delta)*cos(alpha-capn);
u = atan2(su,cu);
b = atan2(sb,sqrt(su*su+cu*cu));
/*
* and then the saturnicentric ring-plane coords of the sun
*/
su = sin(eye)*sin(beta) +
cos(eye)*cos(beta)*sin(lambda-comg);
cu = cos(beta)*cos(lambda-comg);
up = atan2(su,cu);
/*
* at last, the magnitude
*/
sb = sin(b);
mag = -8.68 +2.52*fabs(up+omg-u)-
2.60*fabs(sb) + 1.25*(sb*sb);
helio();
geo();
}
void
jup(void)
{
double pturbl, pturbb, pturbr;
double lograd;
double dele, enom, vnom, nd, sl;
ecc = .0483376 + 163.e-6*capt;
incl = 1.308660 - .0055*capt;
node = 99.43785 + 1.011*capt;
argp = 12.71165 + 1.611*capt;
mrad = 5.202803;
anom = 225.22165 + .0830912*eday - .0484*capt;
motion = 299.1284/3600.;
incl *= radian;
node *= radian;
argp *= radian;
anom = fmod(anom,360.)*radian;
enom = anom + ecc*sin(anom);
do {
dele = (anom - enom + ecc * sin(enom)) /
(1. - ecc*cos(enom));
enom += dele;
} while(fabs(dele) > converge);
vnom = 2.*atan2(sqrt((1.+ecc)/(1.-ecc))*sin(enom/2.),
cos(enom/2.));
rad = mrad*(1. - ecc*cos(enom));
lambda = vnom + argp;
pturbl = 0.;
lambda += pturbl*radsec;
pturbb = 0.;
pturbr = 0.;
/*
* reduce to the ecliptic
*/
nd = lambda - node;
lambda = node + atan2(sin(nd)*cos(incl),cos(nd));
sl = sin(incl)*sin(nd) + pturbb*radsec;
beta = atan2(sl, pyth(sl));
lograd = pturbr*2.30258509;
rad *= 1. + lograd;
lambda += 555.*radsec;
beta -= 51.*radsec;
motion *= radian*mrad*mrad/(rad*rad);
semi = 98.47;
mag = -8.93;
helio();
geo();
}
