Read delta t values from external file. * record structure: year(whitespace)delta_t in 0.01 sec. */

function calculates maximum distance, minimum distance and true distance between * the Sun and the Earth-Moon barycentre. Maximum and minimum distan

precession matrix Owen 1990 */

* Long term high precision precession, * according to Vondrak/Capitaine/Wallace, "New precession expressions, valid * for long time intervals", i

precession of the equator */

precession matrix */

SWISSEPH * reads constants on ephemeris file * ifno file # * serr error string */

* this entry obtains the constants from the ephemeris file * call state to initialize the ephemeris and read in the constants */

Simple fast algorithm for risings and settings of * - planets Sun, Moon, Mercury - Pluto + Lunar Nodes and Fixed stars * Does not work well for g

SWISSEPH * adds reference orbit to chebyshew series (if SEI_FLG_ELLIPSE), * rotates series to mean equinox of J2000 * * ipli planet number */

* houses to sidereal * ------------------ * there are two methods: * a) the traditional one * houses are computed tropically, then nutatio

* Be t the birth date and t0 the epoch at which ayanamsa = 0. * 1. Compute the angle between the solar system rotation plane and * the true eq

common simplified procedure */

* The time range of DE431 requires a new calculation of sidereal time that * gives sensible results for the remote past and future. * The algorit

* decimal degrees in zodiac to nakshatra position, deg, min, sec * * for definition of input see function swe_split_deg(). * output: * ideg deg

Prepare lookup table of sin and cos ( i*Lj ) * for required multiple angles */

the ayanamsa (precession in longitude) * according to Newcomb's definition: 360 - * longitude of the vernal point of t referred to the * ecliptic

returns data from internal file structures sweph.fidat used in last call to swe_calc() or swe_fixstar() ifno = 0 planet file sepl_xxx, used for Su

* Function returns OK or ERR. * cusps are returned in double cusp[13], * or cusp[37] with house system 'G'. * cusp[1..

* Input: tjd_et Julian day number, terrestrial time (ephemeris time). * gregfalg Calendar flag * Output: UTC year, month, day, hour, mi

When is the next lunar eclipse? * * retflag SE_ECL_TOTAL or SE_ECL_PENUMBRAL or SE_ECL_PARTIAL * * tret[0] time of maximum eclipse * tret[1]

same as swe_rise_trans(), but allows to define the height of the horizon * at the point of the rising or setting (horhgt) */

* Input: Clock time UTC, year, month, day, hour, minute, second (decimal). * gregflag Calendar flag * serr error string *

Evaluates a given chebyshev series coef[0..ncf-1] * with ncf terms at x in [-1,1]. Communications of the ACM, algorithm 446, * April 1973 (vol.

* evaluates derivative of chebyshev series, see echeb */

function calculates a fixstar from a record from sefstars.txt * input: * char *srecord fixed star data record from sefstars.txt * double tjd

SWISSEPH * generates name of ephemeris file * file name looks as follows: * swephpl.m30, where * * "sweph" "swiss ephemeris"

Calculate geometric coordinates of true interpolated Moon apsides */

function for sorting fixed stars with qsort() */

help function for finding a fixed star with bsearch() */

$Header: d2l.c,v 1.9 91/11/16 16:24:20 alois Exp $ double to long with rounding, no overflow check *************************************/

closes all open files, frees space of planetary data, * deletes memory of all computed positions */

* conversion between ecliptical and equatorial polar coordinates * with speed. * for users of SWISSEPH, not used by our routines. * for ecl. to

round second, but at 29.5959 always down *************************************/

double to int32 with rounding, no overflow check *************************************/