Robert Daniel DeSonia, MHPCC
Definition in file psEarthOrientation.h.
#include "psCoord.h"
#include "psTime.h"
#include "psSphereOps.h"
Include dependency graph for psEarthOrientation.h:
This graph shows which files directly or indirectly include this file:
Go to the source code of this file.
Data Structures | |
| struct | psEarthPole |
| Structure for respresenting the Earth's pole at any moment or determine velocity at the pole. More... | |
Enumerations | |
| enum | psPrecessMethod { PS_PRECESS_ROUGH, PS_PRECESS_COMPLETE_A, PS_PRECESS_COMPLETE_B, PS_PRECESS_IAU2000A } |
| Method for spherical precession used to specify the level of detail used in calculation. More... | |
Functions | |
| bool | p_psEOCInit (void) |
| Initialize EOC. | |
| bool | p_psEOCFinalize (void) |
| Finalize EOC after using functions that make calls to eocInit for time table data. | |
| psEarthPole * | psEarthPoleAlloc (void) |
| Allocates a new psEarthPole structure. | |
| psSphere * | psAberration (psSphere *apparent, const psSphere *actual, const psSphere *direction, double speed) |
| Calculates the apparent position of a star, given its actual position and the velocity vector of the observer. | |
| psSphere * | psGravityDeflection (psSphere *apparent, psSphere *actual, psSphere *sun) |
| Calculates the apparent position of a star, given its actual position and the position of the sun. | |
| psEarthPole * | psEOC_PrecessionModel (const psTime *time) |
| Calculates the components of the rotation between the CEO and GCRS frames, X, Y, and s, using the IAU2000A precession & nutation model. | |
| psEarthPole * | psEOC_PrecessionCorr (const psTime *time, psTimeBulletin bulletin) |
| Provides interpolated corrections to the X and Y components of the polar coordinates from the tables provided by the IERS, just as it does for UT1 and polar motion. | |
| psSphereRot * | psSphereRot_CEOtoGCRS (const psEarthPole *pole) |
| Constructs the spherical rotation for transforming from CEO to GCRS coordinates. | |
| psSphereRot * | psSphereRot_TEOtoCEO (const psTime *time, psEarthPole *tidalCorr) |
| Calculates the rotation of the Earth about the CIP. | |
| psEarthPole * | psEOC_GetPolarMotion (const psTime *time, psTimeBulletin bulletin) |
| Provides interpolated values of the polar motion components extracted from the IERS tables. | |
| psEarthPole * | psEOC_PolarTideCorr (const psTime *time) |
| Provides tidal corrections to the polar motion components using the Ray model of Simon et al. | |
| psEarthPole * | psEOC_NutationCorr (psTime *time) |
| Provides the additional corrections due to nutation terms with periods less than or equal to two days, as well as the correction to the s-prime component of polar motion. | |
| psSphereRot * | psSphereRot_ITRStoTEO (const psEarthPole *motion) |
| Converts the polar motion corrections to a spherical rotation. | |
| psSphereRot * | psSpherePrecess (const psTime *fromTime, const psTime *toTime, psPrecessMethod mode) |
| Generates the complete spherical rotation to account for precession between two times. | |
|
|
Method for spherical precession used to specify the level of detail used in calculation.
Definition at line 40 of file psEarthOrientation.h. |
|
|
Finalize EOC after using functions that make calls to eocInit for time table data.
|
|
|
Initialize EOC. Parses IERS table data and creates the polynomials used by certain EOC functions.
|
|
||||||||||||||||||||
|
Calculates the apparent position of a star, given its actual position and the velocity vector of the observer. The actual and apparent positions are represented as psSphere entries, as is the direction of motion. The speed in that direction is given in units of the speed of light. If the value of apparent is NULL, a new psSphere is allocated, otherwise the point to apparent is used for the result.
|
|
|
Allocates a new psEarthPole structure.
|
|
||||||||||||
|
Provides interpolated values of the polar motion components extracted from the IERS tables.
|
|
|
Provides the additional corrections due to nutation terms with periods less than or equal to two days, as well as the correction to the s-prime component of polar motion.
|
|
|
Provides tidal corrections to the polar motion components using the Ray model of Simon et al.
|
|
||||||||||||
|
Provides interpolated corrections to the X and Y components of the polar coordinates from the tables provided by the IERS, just as it does for UT1 and polar motion.
|
|
|
Calculates the components of the rotation between the CEO and GCRS frames, X, Y, and s, using the IAU2000A precession & nutation model. The input time may be represented in any format other than UT1. This routine must give results identical to the IERS XYS2000A subroutine.
|
|
||||||||||||||||
|
Calculates the apparent position of a star, given its actual position and the position of the sun. The actual and apparent positions are represented as psSphere entries, as is position of the sun. If the value of apparent is NULL, a new psSphere is allocated, otherwise the point to apparent is used for the result.
|
|
||||||||||||||||
|
Generates the complete spherical rotation to account for precession between two times. The equinoxes shall be Julian equinoxes. If NULL is provided for either time, it is assumed to have the reference equinox value of J2000. The mode argument is used to specify the level of detail used in the calculation.
|
|
|
Constructs the spherical rotation for transforming from CEO to GCRS coordinates. The resulting psSphereRot may be used to determine the rotation from CIP/CEO to GCRS. This function must give results identical to the IERS BPN2000.
|
|
|
Converts the polar motion corrections to a spherical rotation. This function should give identical results to the IERS POM2000 subroutine.
|
|
||||||||||||
|
Calculates the rotation of the Earth about the CIP. If tidalCorr is non-NULL, use the S-component to provide tidal corrections to the UT1 time. If tidalCorr is NULL, no corrections are made & this step is skipped.
|
1.4.4