illum_c |

## Procedurevoid illum_c ( ConstSpiceChar * target, SpiceDouble et, ConstSpiceChar * abcorr, ConstSpiceChar * obsrvr, ConstSpiceDouble spoint [3], SpiceDouble * phase, SpiceDouble * solar, SpiceDouble * emissn ) ## AbstractDeprecated: This routine has been superseded by the CSPICE routine ilumin_c. This routine is supported for purposes of backward compatibility only. Find the illumination angles at a specified surface point of a target body. ## Required_ReadingKERNEL NAIF_IDS SPK TIME ## KeywordsGEOMETRY ## Brief_I/OVariable I/O Description -------- --- -------------------------------------------------- target I Name of target body. et I Epoch in ephemeris seconds past J2000. abcorr I Desired aberration correction. obsrvr I Name of observing body. spoint I Body-fixed coordinates of a target surface point. phase O Phase angle at the surface point. solar O Solar incidence angle at the surface point. emissn O Emission angle at the surface point. ## Detailed_Inputtarget is the name of the target body. `target' is case-insensitive, and leading and trailing blanks in `target' are not significant. Optionally, you may supply a string containing the integer ID code for the object. For example both "MOON" and "301" are legitimate strings that indicate the moon is the target body. et is the epoch, specified in ephemeris seconds past J2000, at which the apparent illumination angles at the specified surface point on the target body, as seen from the observing body, are to be computed. abcorr is the aberration correction to be used in computing the location and orientation of the target body and the location of the Sun. Possible values are: "NONE" No aberration correction. "LT" Correct the position and orientation of target body for light time, and correct the position of the Sun for light time. "LT+S" Correct the observer-target vector for light time and stellar aberration, correct the orientation of the target body for light time, and correct the target-Sun vector for light time and stellar aberration. "CN" Converged Newtonian light time correction. In solving the light time equation, the "CN" correction iterates until the solution converges (three iterations on all supported platforms). Whether the "CN+S" solution is substantially more accurate than the "LT" solution depends on the geometry of the participating objects and on the accuracy of the input data. In all cases this routine will execute more slowly when a converged solution is computed. See the Particulars section of spkezr_c for a discussion of precision of light time corrections. Both the state and rotation of the target body are corrected for light time. "CN+S" Converged Newtonian light time correction and stellar aberration correction. Both the state and rotation of the target body are corrected for light time. obsrvr is the name of the observing body. This is typically a spacecraft, the earth, or a surface point on the earth. `obsrvr' is case-insensitive, and leading and trailing blanks in `obsrvr' are not significant. Optionally, you may supply a string containing the integer ID code for the object. For example both "EARTH" and "399" are legitimate strings that indicate the earth is the observer. `obsrvr' may be not be identical to `target'. spoint is a surface point on the target body, expressed in rectangular body-fixed (body equator and prime meridian) coordinates. `spoint' need not be visible from the observer's location at time `et'. ## Detailed_Outputphase is the phase angle at `spoint', as seen from `obsrvr' at time `et'. This is the angle between the spoint-obsrvr vector and the spoint-sun vector. Units are radians. The range of `phase' is [0, pi]. See Particulars below for a detailed discussion of the definition. solar is the solar incidence angle at `spoint', as seen from `obsrvr' at time `et'. This is the angle between the surface normal vector at `spoint' and the spoint-sun vector. Units are radians. The range of `solar' is [0, pi]. See Particulars below for a detailed discussion of the definition. emissn is the emission angle at `spoint', as seen from `obsrvr' at time `et'. This is the angle between the surface normal vector at `spoint' and the spoint-observer vector. Units are radians. The range of `emissn' is [0, pi]. See Particulars below for a detailed discussion of the definition. ## ParametersNone. ## Exceptions1) If `target' and `obsrvr' are not distinct, the error SPICE(BODIESNOTDISTINCT) will be signaled. 2) If no SPK (ephemeris) data are available for the observer, target, and Sun at the time specified by `et', the error will be diagnosed by routines called by this routine. If light time corrections are used, SPK data for the target body must be available at the time et - lt, where `lt' is the one-way light time from the target to the observer at `et'. Additionally, SPK data must be available for the Sun at the time et - lt - lt2, where lt2 is the light time from the Sun to the target body at time et - lt. 3) If PCK data defining the orientation or shape of the target body are unavailable, the error will be diagnosed by routines called by this routine. 4) If no body-fixed frame is associated with the target body, the error SPICE(NOFRAME) is signaled. 5) If name of `target' or `obsrvr' cannot be translated to its NAIF ID code, the error SPICE(IDCODENOTFOUND) is signaled. ## FilesNo files are input to this routine. However, ## ParticularsThe term "illumination angles" refers to following set of angles: solar incidence angle Angle between the surface normal at the specified surface point and the vector from the surface point to the Sun. emission angle Angle between the surface normal at the specified surface point and the vector from the surface point to the observer. phase angle Angle between the vectors from the surface point to the observing body and from the surface point to the Sun. The diagram below illustrates the geometric relationships defining these angles. The labels for the solar incidence, emission, and phase angles are "s.i.", "e.", and "phase". * Sun surface normal vector ._ _. |\ /| Sun vector \ phase / \ . . / . . \ ___ / . \/ \/ _\ s.i./ . / \ / . | e. \ / * <--------------- * surface point on viewing vector target body location to viewing (observer) location Note that if the target-observer vector, the target normal vector at the surface point, and the target-sun vector are coplanar, then phase is the sum of incidence and emission. This is rarely true; usually phase angle < solar incidence angle + emission angle All of the above angles can be computed using light time corrections, light time and stellar aberration corrections, or no aberration corrections. The way aberration corrections are used is described below. Care must be used in computing light time corrections. The guiding principle used here is "describe what appears in an image." We ignore differential light time; the light times from all points on the target to the observer are presumed to be equal. Observer-target body vector --------------------------- Let `et' be the epoch at which an observation or remote sensing measurement is made, and let et - lt ("lt" stands for "light time") be the epoch at which the photons received at `et' were emitted from the body (we use the term "emitted" loosely here). The correct observer-target vector points from the observer's location at `et' to the target body's location at et - lt. The target-observer vector points in the opposite direction. Since light time corrections are not symmetric, the correct target-observer vector CANNOT be found by computing the light time corrected position of the observer as seen from the target body. Target body's orientation ------------------------- Using the definitions of `et' and `lt' above, the target body's orientation at et - lt is used. The surface normal is dependent on the target body's orientation, so the body's orientation model must be evaluated for the correct epoch. Target body -- Sun vector ------------------------- All surface features on the target body will appear in a measurement made at `et' as they were at et-lt. In particular, lighting on the target body is dependent on the apparent location of the Sun as seen from the target body at et-lt. So, a second light time correction is used in finding the apparent location of the Sun. Stellar aberration corrections, when used, are applied as follows: Observer-target body vector --------------------------- In addition to light time correction, stellar aberration is used in computing the apparent target body position as seen from the observer's location at time `et'. This apparent position defines the observer-target body vector. Target body-Sun vector ---------------------- The target body-Sun vector is the apparent position of the Sun, corrected for light time and stellar aberration, as seen from the target body at time et-lt. Note that the target body's position is not affected by the stellar aberration correction applied in finding its apparent position as seen by the observer. Once all of the vectors, as well as the target body's orientation, have been computed with the proper aberration corrections, the element of time is eliminated from the computation. The problem becomes a purely geometric one, and is described by the diagram above. ## ExamplesThe numerical results shown for this example may differ across platforms. The results depend on the SPICE kernels used as input, the compiler and supporting libraries, and the machine specific arithmetic implementation. In the following example program, the file spk_m_031103-040201_030502.bsp is a binary SPK file containing data for Mars Global Surveyor, Mars, and the Sun for a time interval bracketing the date 2004 JAN 1 12:00:00 UTC. pck00007.tpc is a planetary constants kernel file containing radii and rotation model constants. naif0007.tls is a leapseconds kernel. Find the phase, solar incidence, and emission angles at the sub-solar and sub-spacecraft points on Mars as seen from the Mars global surveyor spacecraft at a user-specified UTC time. Use light time and stellar aberration corrections. #include <string.h> #include <stdio.h> #include "SpiceUsr.h" int main() { /. Local variables ./ SpiceChar * obsrvr; SpiceChar * target; SpiceChar * utc; SpiceDouble alt; SpiceDouble et; SpiceDouble sscemi; SpiceDouble sscphs; SpiceDouble sscsol; SpiceDouble sslphs; SpiceDouble sslsol; SpiceDouble sslemi; SpiceDouble ssolpt [3]; SpiceDouble sscpt [3]; /. Load kernel files. ./ furnsh_c ( "naif0007.tls" ); furnsh_c ( "pck00007.tpc" ); furnsh_c ( "spk_m_031103-040201_030502.bsp" ); /. Convert the UTC request time to ET (seconds past J2000 TDB). ./ utc = "2004 JAN 1 12:00:00"; str2et_c ( utc, &et ); /. Assign observer and target names. The acronym MGS indicates Mars Global Surveyor. See NAIF_IDS for a list of names recognized by SPICE. ./ target = "Mars"; obsrvr = "MGS"; /. Find the sub-solar point on the Earth as seen from the MGS spacecraft at et. Use the "near point" style of sub-point definition. This makes it easy to verify the solar incidence angle. ./ subsol_c ( "near point", target, et, "LT+S", obsrvr, ssolpt ); /. Now find the sub-spacecraft point. Use the "nearest point" definition of the sub-point here---this makes it easy to verify the emission angle. ./ subpt_c ( "near point", target, et, "LT+S", obsrvr, sscpt, &alt ); /. Find the phase, solar incidence, and emission angles at the sub-solar point on the Earth as seen from Mars Observer at time et. ./ ## RestrictionsNone. ## Literature_ReferencesNone. ## Author_and_InstitutionC.H. Acton (JPL) N.J. Bachman (JPL) ## Version-CSPICE Version 1.0.5, 10-JUL-2014 (NJB) Discussion of light time corrections was updated. Assertions that converged light time corrections are unlikely to be useful were removed. -CSPICE Version 1.0.4, 19-MAY-2010 (BVS) Index lines now state that this routine is deprecated. -CSPICE Version 1.0.3, 07-FEB-2008 (NJB) Abstract now states that this routine is deprecated. -CSPICE Version 1.0.2, 22-JUL-2004 (NJB) Updated header to indicate that the `target' and `observer' input arguments can now contain string representations of integers. -CSPICE Version 1.1.2, 27-JUL-2003 (NJB) (CHA) Various header corrections were made. The example program was upgraded to use real kernels, and the program's output is shown. -CSPICE Version 1.1.1, 04-SEP-2002 (NJB) Updated Index_Entries header section. Corrected error in erract_c call in header example. -CSPICE Version 1.1.0, 24-JUL-2001 (NJB) Changed prototype: input spoint is now type (ConstSpiceDouble [3]). Implemented interface macro for casting spoint array to const. -CSPICE Version 1.0.0, 25-MAY-1999 (NJB) ## Index_EntriesDEPRECATED illumination angles DEPRECATED lighting angles DEPRECATED phase angle DEPRECATED emission angle DEPRECATED solar incidence angle |

Wed Apr 5 17:54:36 2017