Add:Core:Support for automatic day night switching|Thanks chollya

git-svn-id: http://svn.code.sf.net/p/navit/code/trunk/navit@2746 ffa7fe5e-494d-0410-b361-a75ebd5db220

1 files changed, 309 insertions, 0 deletions

diff --git a/navit/sunriset.c b/navit/sunriset.c
new file mode 100644
index 000000000..ee6a37b31
--- /dev/null
+++ b/navit/sunriset.c
@@ -0,0 +1,309 @@
+/*
+
+SUNRISET.C - computes Sun rise/set times, start/end of twilight, and
+             the length of the day at any date and latitude
+
+Written as DAYLEN.C, 1989-08-16
+
+Modified to SUNRISET.C, 1992-12-01
+
+(c) Paul Schlyter, 1989, 1992
+
+Released to the public domain by Paul Schlyter, December 1992
+
+*/
+
+
+#include <stdio.h>
+#include <math.h>
+#include <time.h>
+
+#include "sunriset.h"
+
+/* The "workhorse" function for sun rise/set times */
+
+int __sunriset__( time_t ts, double lon, double lat,
+                  double altit, int upper_limb, double *trise, double *tset )
+/***************************************************************************/
+/* Note: year,month,date = calendar date, 1801-2099 only.             */
+/*       Eastern longitude positive, Western longitude negative       */
+/*       Northern latitude positive, Southern latitude negative       */
+/*       The longitude value IS critical in this function!            */
+/*       altit = the altitude which the Sun should cross              */
+/*               Set to -35/60 degrees for rise/set, -6 degrees       */
+/*               for civil, -12 degrees for nautical and -18          */
+/*               degrees for astronomical twilight.                   */
+/*         upper_limb: non-zero -> upper limb, zero -> center         */
+/*               Set to non-zero (e.g. 1) when computing rise/set     */
+/*               times, and to zero when computing start/end of       */
+/*               twilight.                                            */
+/*        *rise = where to store the rise time                        */
+/*        *set  = where to store the set  time                        */
+/*                Both times are relative to the specified altitude,  */
+/*                and thus this function can be used to comupte       */
+/*                various twilight times, as well as rise/set times   */
+/* Return value:  0 = sun rises/sets this day, times stored at        */
+/*                    *trise and *tset.                               */
+/*               +1 = sun above the specified "horizon" 24 hours.     */
+/*                    *trise set to time when the sun is at south,    */
+/*                    minus 12 hours while *tset is set to the south  */
+/*                    time plus 12 hours. "Day" length = 24 hours     */
+/*               -1 = sun is below the specified "horizon" 24 hours   */
+/*                    "Day" length = 0 hours, *trise and *tset are    */
+/*                    both set to the time when the sun is at south.  */
+/*                                                                    */
+/**********************************************************************/
+{
+      int year, month, day;
+      struct tm ymd;
+      double  d,  /* Days since 2000 Jan 0.0 (negative before) */
+      sr,         /* Solar distance, astronomical units */
+      sRA,        /* Sun's Right Ascension */
+      sdec,       /* Sun's declination */
+      sradius,    /* Sun's apparent radius */
+      t,          /* Diurnal arc */
+      tsouth,     /* Time when Sun is at south */
+      sidtime;    /* Local sidereal time */
+
+      int rc = 0; /* Return cde from function - usually 0 */
+
+      //Split ts to y/m/d
+      gmtime_r(&ts,&ymd);
+      year=ymd.tm_year+1900;
+      month=ymd.tm_mon+1;
+      day=ymd.tm_mday+1;
+
+      /* Compute d of 12h local mean solar time */
+      d = days_since_2000_Jan_0(year,month,day) + 0.5 - lon/360.0;
+
+      /* Compute local sideral time of this moment */
+      sidtime = revolution( GMST0(d) + 180.0 + lon );
+
+      /* Compute Sun's RA + Decl at this moment */
+      sun_RA_dec( d, &sRA, &sdec, &sr );
+
+      /* Compute time when Sun is at south - in hours UT */
+      tsouth = 12.0 - rev180(sidtime - sRA)/15.0;
+
+      /* Compute the Sun's apparent radius, degrees */
+      sradius = 0.2666 / sr;
+
+      /* Do correction to upper limb, if necessary */
+      if ( upper_limb )
+            altit -= sradius;
+
+      /* Compute the diurnal arc that the Sun traverses to reach */
+      /* the specified altitide altit: */
+      {
+            double cost;
+            cost = ( sind(altit) - sind(lat) * sind(sdec) ) /
+                  ( cosd(lat) * cosd(sdec) );
+            if ( cost >= 1.0 )
+                  rc = -1, t = 0.0;       /* Sun always below altit */
+            else if ( cost <= -1.0 )
+                  rc = +1, t = 12.0;      /* Sun always above altit */
+            else
+                  t = acosd(cost)/15.0;   /* The diurnal arc, hours */
+      }
+
+      /* Store rise and set times - in hours UT */
+      *trise = tsouth - t;
+      *tset  = tsouth + t;
+
+      return rc;
+}  /* __sunriset__ */
+
+
+
+/* The "workhorse" function */
+
+
+double __daylen__( int year, int month, int day, double lon, double lat,
+                   double altit, int upper_limb )
+/**********************************************************************/
+/* Note: year,month,date = calendar date, 1801-2099 only.             */
+/*       Eastern longitude positive, Western longitude negative       */
+/*       Northern latitude positive, Southern latitude negative       */
+/*       The longitude value is not critical. Set it to the correct   */
+/*       longitude if you're picky, otherwise set to to, say, 0.0     */
+/*       The latitude however IS critical - be sure to get it correct */
+/*       altit = the altitude which the Sun should cross              */
+/*               Set to -35/60 degrees for rise/set, -6 degrees       */
+/*               for civil, -12 degrees for nautical and -18          */
+/*               degrees for astronomical twilight.                   */
+/*         upper_limb: non-zero -> upper limb, zero -> center         */
+/*               Set to non-zero (e.g. 1) when computing day length   */
+/*               and to zero when computing day+twilight length.      */
+/**********************************************************************/
+{
+      double  d,  /* Days since 2000 Jan 0.0 (negative before) */
+      obl_ecl,    /* Obliquity (inclination) of Earth's axis */
+      sr,         /* Solar distance, astronomical units */
+      slon,       /* True solar longitude */
+      sin_sdecl,  /* Sine of Sun's declination */
+      cos_sdecl,  /* Cosine of Sun's declination */
+      sradius,    /* Sun's apparent radius */
+      t;          /* Diurnal arc */
+
+      /* Compute d of 12h local mean solar time */
+      d = days_since_2000_Jan_0(year,month,day) + 0.5 - lon/360.0;
+
+      /* Compute obliquity of ecliptic (inclination of Earth's axis) */
+      obl_ecl = 23.4393 - 3.563E-7 * d;
+
+      /* Compute Sun's position */
+      sunpos( d, &slon, &sr );
+
+      /* Compute sine and cosine of Sun's declination */
+      sin_sdecl = sind(obl_ecl) * sind(slon);
+      cos_sdecl = sqrt( 1.0 - sin_sdecl * sin_sdecl );
+
+      /* Compute the Sun's apparent radius, degrees */
+      sradius = 0.2666 / sr;
+
+      /* Do correction to upper limb, if necessary */
+      if ( upper_limb )
+            altit -= sradius;
+
+      /* Compute the diurnal arc that the Sun traverses to reach */
+      /* the specified altitide altit: */
+      {
+            double cost;
+            cost = ( sind(altit) - sind(lat) * sin_sdecl ) /
+                  ( cosd(lat) * cos_sdecl );
+            if ( cost >= 1.0 )
+                  t = 0.0;                      /* Sun always below altit */
+            else if ( cost <= -1.0 )
+                  t = 24.0;                     /* Sun always above altit */
+            else  t = (2.0/15.0) * acosd(cost); /* The diurnal arc, hours */
+      }
+      return t;
+}  /* __daylen__ */
+
+
+/* This function computes the Sun's position at any instant */
+
+void sunpos( double d, double *lon, double *r )
+/******************************************************/
+/* Computes the Sun's ecliptic longitude and distance */
+/* at an instant given in d, number of days since     */
+/* 2000 Jan 0.0.  The Sun's ecliptic latitude is not  */
+/* computed, since it's always very near 0.           */
+/******************************************************/
+{
+      double M,         /* Mean anomaly of the Sun */
+             w,         /* Mean longitude of perihelion */
+                        /* Note: Sun's mean longitude = M + w */
+             e,         /* Eccentricity of Earth's orbit */
+             E,         /* Eccentric anomaly */
+             x, y,      /* x, y coordinates in orbit */
+             v;         /* True anomaly */
+
+      /* Compute mean elements */
+      M = revolution( 356.0470 + 0.9856002585 * d );
+      w = 282.9404 + 4.70935E-5 * d;
+      e = 0.016709 - 1.151E-9 * d;
+
+      /* Compute true longitude and radius vector */
+      E = M + e * RADEG * sind(M) * ( 1.0 + e * cosd(M) );
+      x = cosd(E) - e;
+      y = sqrt( 1.0 - e*e ) * sind(E);
+      *r = sqrt( x*x + y*y );              /* Solar distance */
+      v = atan2d( y, x );                  /* True anomaly */
+      *lon = v + w;                        /* True solar longitude */
+      if ( *lon >= 360.0 )
+            *lon -= 360.0;                   /* Make it 0..360 degrees */
+}
+
+void sun_RA_dec( double d, double *RA, double *dec, double *r )
+{
+  double lon, obl_ecl;
+  double xs, ys, zs;
+  double xe, ye, ze;
+  
+  /* Compute Sun's ecliptical coordinates */
+  sunpos( d, &lon, r );
+  
+  /* Compute ecliptic rectangular coordinates */
+  xs = *r * cosd(lon);
+  ys = *r * sind(lon);
+  zs = 0; /* because the Sun is always in the ecliptic plane! */
+
+  /* Compute obliquity of ecliptic (inclination of Earth's axis) */
+  obl_ecl = 23.4393 - 3.563E-7 * d;
+  
+  /* Convert to equatorial rectangular coordinates - x is unchanged */
+  xe = xs;
+  ye = ys * cosd(obl_ecl);
+  ze = ys * sind(obl_ecl);
+  
+  /* Convert to spherical coordinates */
+  *RA = atan2d( ye, xe );
+  *dec = atan2d( ze, sqrt(xe*xe + ye*ye) );
+      
+}  /* sun_RA_dec */
+
+
+/******************************************************************/
+/* This function reduces any angle to within the first revolution */
+/* by subtracting or adding even multiples of 360.0 until the     */
+/* result is >= 0.0 and < 360.0                                   */
+/******************************************************************/
+
+#define INV360    ( 1.0 / 360.0 )
+
+double revolution( double x )
+/*****************************************/
+/* Reduce angle to within 0..360 degrees */
+/*****************************************/
+{
+      return( x - 360.0 * floor( x * INV360 ) );
+}  /* revolution */
+
+double rev180( double x )
+/*********************************************/
+/* Reduce angle to within -180..+180 degrees */
+/*********************************************/
+{
+      return( x - 360.0 * floor( x * INV360 + 0.5 ) );
+}  /* revolution */
+
+
+/*******************************************************************/
+/* This function computes GMST0, the Greenwhich Mean Sidereal Time */
+/* at 0h UT (i.e. the sidereal time at the Greenwhich meridian at  */
+/* 0h UT).  GMST is then the sidereal time at Greenwich at any     */
+/* time of the day.  I've generelized GMST0 as well, and define it */
+/* as:  GMST0 = GMST - UT  --  this allows GMST0 to be computed at */
+/* other times than 0h UT as well.  While this sounds somewhat     */
+/* contradictory, it is very practical:  instead of computing      */
+/* GMST like:                                                      */
+/*                                                                 */
+/*  GMST = (GMST0) + UT * (366.2422/365.2422)                      */
+/*                                                                 */
+/* where (GMST0) is the GMST last time UT was 0 hours, one simply  */
+/* computes:                                                       */
+/*                                                                 */
+/*  GMST = GMST0 + UT                                              */
+/*                                                                 */
+/* where GMST0 is the GMST "at 0h UT" but at the current moment!   */
+/* Defined in this way, GMST0 will increase with about 4 min a     */
+/* day.  It also happens that GMST0 (in degrees, 1 hr = 15 degr)   */
+/* is equal to the Sun's mean longitude plus/minus 180 degrees!    */
+/* (if we neglect aberration, which amounts to 20 seconds of arc   */
+/* or 1.33 seconds of time)                                        */
+/*                                                                 */
+/*******************************************************************/
+
+double GMST0( double d )
+{
+      double sidtim0;
+      /* Sidtime at 0h UT = L (Sun's mean longitude) + 180.0 degr  */
+      /* L = M + w, as defined in sunpos().  Since I'm too lazy to */
+      /* add these numbers, I'll let the C compiler do it for me.  */
+      /* Any decent C compiler will add the constants at compile   */
+      /* time, imposing no runtime or code overhead.               */
+      sidtim0 = revolution( ( 180.0 + 356.0470 + 282.9404 ) +
+                          ( 0.9856002585 + 4.70935E-5 ) * d );
+      return sidtim0;
+}  /* GMST0 */