void illumg_c ( ConstSpiceChar * method,
ConstSpiceChar * target,
ConstSpiceChar * ilusrc,
SpiceDouble et,
ConstSpiceChar * fixref,
ConstSpiceChar * abcorr,
ConstSpiceChar * obsrvr,
ConstSpiceDouble spoint [3],
SpiceDouble * trgepc,
SpiceDouble srfvec [3],
SpiceDouble * phase,
SpiceDouble * incdnc,
SpiceDouble * emissn )
Find the illumination angles (phase, incidence, and
emission) at a specified surface point of a target body.
The surface of the target body may be represented by a triaxial
ellipsoid or by topographic data provided by DSK files.
The illumination source is a specified ephemeris object.
DSK
FRAMES
NAIF_IDS
PCK
SPK
TIME
ANGLES
GEOMETRY
ILLUMINATION
Variable I/O Description
-------- --- --------------------------------------------------
method I Computation method.
target I Name of target body.
ilusrc I Name of illumination source.
et I Epoch in TDB seconds past J2000 TDB.
fixref I Body-fixed, body-centered target body frame.
abcorr I Aberration correction flag.
obsrvr I Name of observing body.
spoint I Body-fixed coordinates of a target surface point.
trgepc O Target surface point epoch.
srfvec O Vector from observer to target surface point.
phase O Phase angle at the surface point.
incdnc O Source incidence angle at the surface point.
emissn O Emission angle at the surface point.
method is a short string providing parameters defining
the computation method to be used. In the syntax
descriptions below, items delimited by brackets
are optional.
`method' may be assigned the following values:
"ELLIPSOID"
The illumination angle computation uses a
triaxial ellipsoid to model the surface of the
target body. The ellipsoid's radii must be
available in the kernel pool.
"DSK/UNPRIORITIZED[/SURFACES = <surface list>]"
The illumination angle computation uses
topographic data to model the surface of the
target body. These data must be provided by
loaded DSK files.
The surface list specification is optional. The
syntax of the list is
<surface 1> [, <surface 2>...]
If present, it indicates that data only for the
listed surfaces are to be used; however, data
need not be available for all surfaces in the
list. If absent, loaded DSK data for any surface
associated with the target body are used.
The surface list may contain surface names or
surface ID codes. Names containing blanks must
be delimited by escaped double quotes, for example
"SURFACES = \"Mars MEGDR 128 PIXEL/DEG\""
If multiple surfaces are specified, their names
or IDs must be separated by commas.
See the Particulars section below for details
concerning use of DSK data.
Neither case nor white space are significant in
`method', except within double-quoted strings
representing surface names. For example, the string
" eLLipsoid " is valid.
Within double-quoted strings representing surface names,
blank characters are significant, but multiple
consecutive blanks are considered equivalent to a single
blank. Case is not significant. So
\"Mars MEGDR 128 PIXEL/DEG\"
is equivalent to
\" mars megdr 128 pixel/deg \"
but not to
\"MARS MEGDR128PIXEL/DEG\"
target 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.
ilusrc is the name of the illumination source. This source
may be any ephemeris object. Case, blanks, and
numeric values are treated in the same way as for the
input `target'.
et is the epoch, expressed as seconds past J2000 TDB,
for which the apparent illumination angles at the
specified surface point on the target body, as seen
from the observing body, are to be computed.
fixref is the name of the body-fixed, body-centered
reference frame associated with the target body. The
input surface point `spoint' and the output vector
`srfvec' are expressed relative to this reference
frame. The string `fixref' is case-insensitive, and
leading and trailing blanks in `fixref' are not
significant.
abcorr is the aberration correction to be used in computing
the position and orientation of the target body and
the location of the illumination source.
For remote sensing applications, where the apparent
illumination angles seen by the observer are desired,
normally either of the corrections
"LT+S"
"CN+S"
should be used. These and the other supported options
are described below. `abcorr' may be any of the
following:
"NONE" No aberration correction.
Let `lt' represent the one-way light time between the
observer and the input surface point `spoint' (note: NOT
between the observer and the target body's center). The
following values of `abcorr' apply to the "reception"
case in which photons depart from `spoint' at the
light-time corrected epoch et-lt and *arrive* at the
observer's location at `et':
"LT" Correct both the position of `spoint' as
seen by the observer, and the position
of the illumination source as seen by
the target, for light time. Correct the
orientation of the target for light
time.
"LT+S" Correct both the position of `spoint' as
seen by the observer, and the position
of the illumination source as seen by
the target, for light time and stellar
aberration. Correct the orientation of
the target for light time.
"CN" Converged Newtonian light time
correction. In solving the light time
equations for `spoint' and the
illumination source, the "CN"
correction iterates until the solution
converges.
"CN+S" Converged Newtonian light time and
stellar aberration corrections. This
option produces a solution that is at
least as accurate at that obtainable
with the "LT+S" option. Whether the
"CN+S" solution is substantially more
accurate 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.
The following values of `abcorr' apply to the
"transmission" case in which photons *arrive* at
`spoint' at the light-time corrected epoch et+lt and
*depart* from the observer's location at `et':
"XLT" "Transmission" case: correct for
one-way light time using a Newtonian
formulation. This correction yields the
illumination angles at the moment that
`spoint' receives photons emitted from the
observer's location at `et'.
The light time correction uses an
iterative solution of the light time
equation. The solution invoked by the
"XLT" option uses one iteration.
Both the target position as seen by the
observer, and rotation of the target
body, are corrected for light time.
"XLT+S" "Transmission" case: correct for
one-way light time and stellar
aberration using a Newtonian
formulation This option modifies the
angles obtained with the "XLT" option
to account for the observer's and
target's velocities relative to the
solar system barycenter (the latter
velocity is used in computing the
direction to the apparent illumination
source).
"XCN" Converged Newtonian light time
correction. This is the same as XLT
correction but with further iterations
to a converged Newtonian light time
solution.
"XCN+S" "Transmission" case: converged
Newtonian light time and stellar
aberration corrections. This option
produces a solution that is at least as
accurate at that obtainable with the
"XLT+S" option. Whether the "XCN+S"
solution is substantially more accurate
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.
Neither case nor white space are significant in
`abcorr'. For example, the string
"Lt + s"
is valid.
obsrvr is the name of the observing body. The observing body
is an ephemeris object: it typically is 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 "MOON" and "301" are
legitimate strings that indicate the moon is the
observer.
`obsrvr' may be not be identical to `target'.
spoint is a surface point on the target body, expressed in
Cartesian coordinates, relative to the body-fixed
target frame designated by `fixref'.
`spoint' need not be visible from the observer's
location at the epoch `et'.
The components of `spoint' have units of km.
trgepc is the "target surface point epoch." `trgepc' is defined
as follows: letting `lt' be the one-way light time
between the observer and the input surface point
`spoint', `trgepc' is either the epoch et-lt or `et'
depending on whether the requested aberration correction
is, respectively, for received radiation or omitted.
`lt' is computed using the method indicated by `abcorr'.
`trgepc' is expressed as TDB seconds past J2000 TDB.
srfvec is the vector from the observer's position at `et' to
the aberration-corrected (or optionally, geometric)
position of `spoint', where the aberration corrections
are specified by `abcorr'. `srfvec' is expressed in the
target body-fixed reference frame designated by
`fixref', evaluated at `trgepc'.
The components of `srfvec' are given in units of km.
One can use the CSPICE function vnorm_c to obtain the
distance between the observer and `spoint':
dist = vnorm_c ( srfvec );
The observer's position `obspos', relative to the
target body's center, where the center's position is
corrected for aberration effects as indicated by
`abcorr', can be computed via the call:
vsub_c ( spoint, srfvec, obspos );
To transform the vector `srfvec' from a reference frame
`fixref' at time `trgepc' to a time-dependent reference
frame `ref' at time `et', the routine pxfrm2_c should be
called. Let `xform' be the 3x3 matrix representing the
rotation from the reference frame `fixref' at time
`trgepc' to the reference frame `ref' at time `et'. Then
`srfvec' can be transformed to the result `refvec' as
follows:
pxfrm2_c ( fixref, ref, trgepc, et, xform );
mxv_c ( xform, srfvec, refvec );
phase 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-illumination source vector. Units
are radians. The range of `phase' is [0, pi]. See
Particulars below for a detailed discussion of the
definition.
incdnc is the illumination source 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-illumination source vector. Units are radians.
The range of `incdnce' 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.
None.
1) If the specified aberration correction is relativistic or
calls for stellar aberration but not light time correction,
the error SPICE(NOTSUPPORTED) is signaled. If the specified
aberration correction is any other unrecognized value, the
error will be diagnosed and signaled by a routine in the call
tree of this routine.
2) If any of the target, observer, or illumination source
input strings cannot be converted to an integer ID code, the
error SPICE(IDCODENOTFOUND) is signaled.
3) If `obsrvr' and `target' map to the same NAIF integer ID code,
the error SPICE(BODIESNOTDISTINCT) is signaled.
4) If the input target body-fixed frame `fixref' is not
recognized, the error SPICE(NOFRAME) is signaled. A frame
name may fail to be recognized because a required frame
specification kernel has not been loaded; another cause is a
misspelling of the frame name.
5) If the input frame `fixref' is not centered at the target body,
the error SPICE(INVALIDFRAME) is signaled.
6) If the input argument `METHOD' is not recognized, the error
SPICE(INVALIDMETHOD) is signaled.
7) If insufficient ephemeris data have been loaded prior to
calling illumg_c, the error will be diagnosed and signaled by a
routine in the call tree of this routine. Note that when
light time correction is used, sufficient ephemeris data must
be available to propagate the states of observer, target, and
the illumination source to the solar system barycenter.
8) If the computation method specifies an ellipsoidal target
shape and triaxial radii of the target body have not been
loaded into the kernel pool prior to calling illumg_c, the
error will be diagnosed and signaled by a routine in the call
tree of this routine.
9) The target must be an extended body: if any of the radii of
the target body are non-positive, the error will be
diagnosed and signaled by routines in the call tree of this
routine.
10) If PCK or CK data specifying the target body-fixed frame
orientation have not been loaded prior to calling illumg_c,
the error will be diagnosed and signaled by a routine in the
call tree of this routine.
11) If ``method'' specifies that the target surface is represented by
DSK data, and no DSK files are loaded for the specified
target, the error is signaled by a routine in the call tree
of this routine.
12) If `method' specifies that the target surface is represented
by DSK data, and data representing the portion of the surface
on which `spoint' is located are not available, an error will
be signaled by a routine in the call tree of this routine.
13) If `method' specifies that the target surface is represented
by DSK data, `spoint' must lie on the target surface, not above
or below it. A small tolerance is used to allow for round-off
error in the calculation determining whether `spoint' is on the
surface. If, in the DSK case, `spoint' is too far from the
surface, an error will be signaled by a routine in the call
tree of this routine.
If the surface is represented by a triaxial ellipsoid, `spoint'
is not required to be close to the ellipsoid; however, the
results computed by this routine will be unreliable if `spoint'
is too far from the ellipsoid.
Appropriate kernels must be loaded by the calling program before
this routine is called.
The following data are required:
- SPK data: ephemeris data for target, observer, and the
illumination source must be loaded. If aberration corrections
are used, the states of target, observer, and the illumination
source relative to the solar system barycenter must be
calculable from the available ephemeris data. Ephemeris data
are made available by loading one or more SPK files via
furnsh_c.
- Target body orientation data: these may be provided in a text or
binary PCK file. In some cases, target body orientation may
be provided by one more more CK files. In either case, data
are made available by loading the files via furnsh_c.
- Shape data for the target body:
PCK data:
If the target body shape is modeled as an ellipsoid,
triaxial radii for the target body must be loaded into
the kernel pool. Typically this is done by loading a
text PCK file via furnsh_c.
Triaxial radii are also needed if the target shape is
modeled by DSK data, and the DSK NADIR method is
selected.
DSK data:
If the target shape is modeled by DSK data, DSK files
containing topographic data for the target body must be
loaded. If a surface list is specified, data for at
least one of the listed surfaces must be loaded. DSK
files are loaded via furnsh_c.
The following data may be required:
- Frame data: if a frame definition is required to convert the
observer and target states to the body-fixed frame of the
target, that definition must be available in the kernel
pool. Typically the definition is supplied by loading a
frame kernel via furnsh_c.
- Surface name-ID associations: if surface names are specified
in `method', the association of these names with their
corresponding surface ID codes must be established by
assignments of the kernel variables
NAIF_SURFACE_NAME
NAIF_SURFACE_CODE
NAIF_SURFACE_BODY
Normally these associations are made by loading a text
kernel containing the necessary assignments. An example
of such assignments is
NAIF_SURFACE_NAME += 'Mars MEGDR 128 PIXEL/DEG'
NAIF_SURFACE_CODE += 1
NAIF_SURFACE_BODY += 499
- SCLK data: if the target body's orientation is provided by
CK files, an associated SCLK kernel must be loaded.
In all cases, kernel data are normally loaded once per program
run, NOT every time this routine is called.
CSPICE contains four routines that compute illumination angles:
illumf_c (same as this routine, except that illumination
and visibility flags are returned)
illumg_c (this routine)
ilumin_c (same as illumg_c, except that the sun is fixed
as the illumination source)
illum_c (deprecated)
illumf_c is the most capable of the set.
Illumination angles
===================
The term "illumination angles" refers to the following set of
angles:
phase angle Angle between the vectors from the
surface point to the observer and
from the surface point to the
illumination source.
incidence angle Angle between the surface normal at
the specified surface point and the
vector from the surface point to the
illumination source.
emission angle Angle between the surface normal at
the specified surface point and the
vector from the surface point to the
observer.
The diagram below illustrates the geometric relationships
defining these angles. The labels for the incidence, emission,
and phase angles are "inc.", "e.", and "phase".
*
illumination source
surface normal vector
._ _.
|\ /| illumination
\ phase / source vector
\ . . /
. .
\ ___ /
. \/ \/
_\ inc./
. / \ /
. | 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-illumination source vector
are coplanar, then phase is the sum of the incidence and emission
angles. This rarely occurs; usually
phase angle < 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. In order to describe apparent geometry as
observed by a remote sensing instrument, both light time and
stellar aberration corrections should be used.
The way aberration corrections are applied by this routine
is described below.
Light time corrections
======================
Observer-target surface point 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 surface point `spoint'.
Note that the light time between the surface point and
observer will generally differ from the light time between
the target body's center and the observer.
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 -- illumination source vector
-----------------------------------------
The surface features on the target body near `spoint' 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 illumination source as seen
from the target body at et-lt. So, a second light time
correction is used to compute the position of the
illumination source relative to the surface point.
Stellar aberration corrections
==============================
Stellar aberration corrections are applied only if
light time corrections are applied as well.
Observer-target surface point body vector
-----------------------------------------
When stellar aberration correction is performed, the
direction vector `srfvec' is adjusted so as to point to the
apparent position of `spoint': considering `spoint' to be an
ephemeris object, `srfvec' points from the observer's
position at `et' to the light time and stellar aberration
corrected position of `spoint'.
Target body-illumination source vector
--------------------------------------
The target body-illumination source vector is the apparent
position of the illumination source, corrected for light
time and stellar aberration, as seen from the target body
at time et-lt.
Using DSK data
==============
DSK loading and unloading
-------------------------
DSK files providing data used by this routine are loaded by
calling furnsh_c and can be unloaded by calling unload_c or
kclear_c. See the documentation of furnsh_c for limits on numbers
of loaded DSK files.
For run-time efficiency, it's desirable to avoid frequent
loading and unloading of DSK files. When there is a reason to
use multiple versions of data for a given target body---for
example, if topographic data at varying resolutions are to be
used---the surface list can be used to select DSK data to be
used for a given computation. It is not necessary to unload
the data that are not to be used. This recommendation presumes
that DSKs containing different versions of surface data for a
given body have different surface ID codes.
DSK data priority
-----------------
A DSK coverage overlap occurs when two segments in loaded DSK
files cover part or all of the same domain---for example, a
given longitude-latitude rectangle---and when the time
intervals of the segments overlap as well.
When DSK data selection is prioritized, in case of a coverage
overlap, if the two competing segments are in different DSK
files, the segment in the DSK file loaded last takes
precedence. If the two segments are in the same file, the
segment located closer to the end of the file takes
precedence.
When DSK data selection is unprioritized, data from competing
segments are combined. For example, if two competing segments
both represent a surface as a set of triangular plates, the
union of those sets of plates is considered to represent the
surface.
Currently only unprioritized data selection is supported.
Because prioritized data selection may be the default behavior
in a later version of the routine, the UNPRIORITIZED keyword is
required in the `method' argument.
Syntax of the `method' input argument
-----------------------------------
The keywords and surface list in the `method' argument
are called "clauses." The clauses may appear in any
order, for example
"DSK/<surface list>/UNPRIORITIZED"
"DSK/UNPRIORITIZED/<surface list>"
"UNPRIORITIZED/<surface list>/DSK"
The simplest form of the `method' argument specifying use of
DSK data is one that lacks a surface list, for example:
"DSK/UNPRIORITIZED"
For applications in which all loaded DSK data for the target
body are for a single surface, and there are no competing
segments, the above string suffices. This is expected to be
the usual case.
When, for the specified target body, there are loaded DSK
files providing data for multiple surfaces for that body, the
surfaces to be used by this routine for a given call must be
specified in a surface list, unless data from all of the
surfaces are to be used together.
The surface list consists of the string
"SURFACES ="
followed by a comma-separated list of one or more surface
identifiers. The identifiers may be names or integer codes in
string format. For example, suppose we have the surface
names and corresponding ID codes shown below:
Surface Name ID code
------------ -------
"Mars MEGDR 128 PIXEL/DEG" 1
"Mars MEGDR 64 PIXEL/DEG" 2
"Mars_MRO_HIRISE" 3
If data for all of the above surfaces are loaded, then
data for surface 1 can be specified by either
"SURFACES = 1"
or
"SURFACES = "\"Mars MEGDR 128 PIXEL/DEG\""
Escaped double quotes are used to delimit the surface name
because it contains blank characters.
To use data for surfaces 2 and 3 together, any
of the following surface lists could be used:
"SURFACES = 2, 3"
"SURFACES = \"Mars MEGDR 64 PIXEL/DEG\", 3"
"SURFACES = 2, Mars_MRO_HIRISE"
"SURFACES = \"Mars MEGDR 64 PIXEL/DEG\", Mars_MRO_HIRISE"
An example of a `method' argument that could be constructed
using one of the surface lists above is
"DSK/UNPRIORITIZED/SURFACES = \"Mars MEGDR 64 PIXEL/DEG\", 3"
Aberration corrections using DSK data
-------------------------------------
For irregularly shaped target bodies, the distance between the
observer and the nearest surface intercept need not be a
continuous function of time; hence the one-way light time
between the intercept and the observer may be discontinuous as
well. In such cases, the computed light time, which is found
using an iterative algorithm, may converge slowly or not at all.
In all cases, the light time computation will terminate, but
the result may be less accurate than expected.
The 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.
1) 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 specified UTC time.
Use both an ellipsoidal Mars shape model and topographic data
provided by a DSK file. For both surface points, use the "near
point" and "nadir" definitions for ellipsoidal and DSK shape
models, respectively.
Use converged Newtonian light time and stellar aberration
corrections.
The topographic model is based on data from the MGS MOLA DEM
megr90n000cb, which has a resolution of 4 pixels/degree. A
triangular plate model was produced by computing a 720 x 1440
grid of interpolated heights from this DEM, then tessellating
the height grid. The plate model is stored in a type 2 segment
in the referenced DSK file.
Use the meta-kernel shown below to load the required SPICE
kernels.
KPL/MK
File: illumg_ex1.tm
This meta-kernel is intended to support operation of SPICE
example programs. The kernels shown here should not be
assumed to contain adequate or correct versions of data
required by SPICE-based user applications.
In order for an application to use this meta-kernel, the
kernels referenced here must be present in the user's
current working directory.
The names and contents of the kernels referenced
by this meta-kernel are as follows:
File name Contents
--------- --------
de430.bsp Planetary ephemeris
mar097.bsp Mars satellite ephemeris
pck00010.tpc Planet orientation and
radii
naif0011.tls Leapseconds
mgs_ext12_ipng_mgs95j.bsp MGS ephemeris
megr90n000cb_plate.bds Plate model based on
MEGDR DEM, resolution
4 pixels/degree.
\begindata
KERNELS_TO_LOAD = ( 'de430.bsp',
'mar097.bsp',
'pck00010.tpc',
'naif0011.tls',
'mgs_ext12_ipng_mgs95j.bsp',
'megr90n000cb_plate.bds' )
\begintext
Example code begins here.
/.
Program illumg_ex1
./
#include <stdio.h>
#include "SpiceUsr.h"
int main()
{
/.
Local constants
./
#define META "illumg_ex1.tm"
#define MTHLEN 81
#define NMETH 2
/.
Local variables
./
SpiceChar * abcorr;
SpiceChar * fixref;
SpiceChar ilumth [NMETH][MTHLEN] =
{"Ellipsoid", "DSK/Unprioritized" };
SpiceChar * ilusrc;
SpiceChar * target;
SpiceChar * obsrvr;
SpiceChar submth [NMETH][MTHLEN] =
{"Near Point/Ellipsoid", "DSK/Nadir/Unprioritized" };
SpiceChar * utc;
SpiceDouble et;
SpiceDouble srfvec [3];
SpiceDouble sscemi;
SpiceDouble sscphs;
SpiceDouble sscpt [3];
SpiceDouble sscsol;
SpiceDouble sslemi;
SpiceDouble sslphs;
SpiceDouble sslsol;
SpiceDouble ssolpt [3];
SpiceDouble trgepc;
SpiceInt i;
/.
Load kernel files.
./
furnsh_c ( META );
/.
Convert the UTC request time string to seconds past
J2000 TDB.
./
utc = "2003 OCT 13 06:00:00 UTC";
str2et_c ( utc, &et );
printf ( "\n"
"UTC epoch is %s\n", utc );
/.
Assign observer, target, and illumination source
names. The acronym MGS indicates Mars Global
Surveyor. See NAIF_IDS for a list of names
recognized by SPICE.
Also set the target body-fixed frame and
the aberration correction flag.
./
target = "Mars";
obsrvr = "MGS";
fixref = "IAU_MARS";
abcorr = "CN+S";
ilusrc = "Sun";
for ( i = 0; i < NMETH; i++ )
{
/.
Find the sub-solar point on Mars as
seen from the MGS spacecraft at `et'. Use the
"near point" style of sub-point definition
when the shape model is an ellipsoid, and use
the "nadir" style when the shape model is
provided by DSK data. This makes it easy to
verify the solar incidence angle when
the target is modeled as an ellipsoid.
./
subslr_c ( submth[i], target, et,
fixref, abcorr, obsrvr,
ssolpt, &trgepc, srfvec );
/.
Now find the sub-spacecraft point.
./
subpnt_c ( submth[i], target, et,
fixref, abcorr, obsrvr,
sscpt, &trgepc, srfvec );
/.
Find the phase, solar incidence, and emission
angles at the sub-solar point on Mars as
seen from MGS at time `et'.
./
illumg_c ( ilumth[i], target, ilusrc,
et, fixref, abcorr,
obsrvr, ssolpt, &trgepc,
srfvec, &sslphs, &sslsol,
&sslemi );
/.
Do the same for the sub-spacecraft point.
./
illumg_c ( ilumth[i], target, ilusrc,
et, fixref, abcorr,
obsrvr, sscpt, &trgepc,
srfvec, &sscphs, &sscsol,
&sscemi );
/.
Convert the angles to degrees and write them out.
./
sslphs *= dpr_c();
sslsol *= dpr_c();
sslemi *= dpr_c();
sscphs *= dpr_c();
sscsol *= dpr_c();
sscemi *= dpr_c();
printf ( "\n"
" illumg_c method: %s\n"
" subpnt_c method: %s\n"
" subslr_c method: %s\n"
"\n"
" Illumination angles at the "
"sub-solar point:\n"
"\n"
" Phase angle (deg): %15.9f\n"
" Solar incidence angle (deg): %15.9f\n"
" Emission angle (deg): %15.9f\n",
ilumth[i],
submth[i],
submth[i],
sslphs,
sslsol,
sslemi );
if ( i == 0 )
{
printf ( " The solar incidence angle "
"should be 0.\n"
" The emission and phase "
"angles should be equal.\n" );
}
printf ( "\n"
" Illumination angles at the "
"sub-s/c point:\n"
"\n"
" Phase angle (deg): %15.9f\n"
" Solar incidence angle (deg): %15.9f\n"
" Emission angle (deg): %15.9f\n",
sscphs,
sscsol,
sscemi );
if ( i == 0 )
{
printf ( " The emission angle "
"should be 0.\n"
" The solar incidence "
"and phase angles should be equal.\n" );
}
}
printf ( "\n" );
return ( 0 );
}
When this program was executed on a PC/Linux/gcc/64-bit platform,
the output was:
UTC epoch is 2003 OCT 13 06:00:00 UTC
illumg_c method: Ellipsoid
subpnt_c method: Near Point/Ellipsoid
subslr_c method: Near Point/Ellipsoid
Illumination angles at the sub-solar point:
Phase angle (deg): 138.370270685
Solar incidence angle (deg): 0.000000000
Emission angle (deg): 138.370270685
The solar incidence angle should be 0.
The emission and phase angles should be equal.
Illumination angles at the sub-s/c point:
Phase angle (deg): 101.439331040
Solar incidence angle (deg): 101.439331041
Emission angle (deg): 0.000000002
The emission angle should be 0.
The solar incidence and phase angles should be equal.
illumg_c method: DSK/Unprioritized
subpnt_c method: DSK/Nadir/Unprioritized
subslr_c method: DSK/Nadir/Unprioritized
Illumination angles at the sub-solar point:
Phase angle (deg): 138.387071677
Solar incidence angle (deg): 0.967122745
Emission angle (deg): 137.621480599
Illumination angles at the sub-s/c point:
Phase angle (deg): 101.439331359
Solar incidence angle (deg): 101.555993667
Emission angle (deg): 0.117861156
None.
None.
N.J. Bachman (JPL)
B.V. Semenov (JPL)
-CSPICE Version 1.0.0, 04-APR-2017 (NJB) (BVS)
16-AUG-2016
Original version.
illumination angles general source
lighting angles general source
phase angle general source
incidence angle general source
emission angle general source
Link to routine illumg_c source file illumg_c.c
|