Potential due to solar radiation pressure
[pot] = CL_fo_srpPot(pos, pos_sun, coefp [,ecl, er, ersun, p0])
Potential due to solar radiation pressure (SRP).
By definition, the acceleration derived from the potential is +grad(potential).
The SRP coefficient (coefp) is defined by: coefp = cp * area / mass (with cp: reflectivity coefficient, between 1 and 2).
Eclipses can be taken into account or not. If so, the acceleration is multiplied by a factor (equal to 1 if there is no eclipse and less than 1 otherwise).
Notes:
- The origins for the satellite and Sun position vectors must be the same. If eclipses are considered, this origin must be the eclipsing body (i.e. central body).
- The coordinates frame can be any frame.
- The calculation of the eclipse uses the radius of the eclipsing body (er), and the radius of the Sun (ersun). If ersun is empty ([]) then the internal value is used.
- p0 is the solar radius pressure at 1 AU. If p0 is empty ([]) then the internal value is used (equal to the total solar irradiance divided by the speed of light).
See Force models for more details.
Position vector (from any position) [m]. (3xN or 3x1)
Sun position (same origin as pos) [m]. (3xN or 3x1)
SRP coefficient (cp*area/mass) [m^2/kg]. (1xN or 1x1)
(optional, boolean) %t if eclipses are taken into account; %f otherwise. Default is %t. (1x1)
(optional) Equatorial radius of eclipsing body. Default is %CL_eqRad. [m] (1x1)
(optional) Equatorial radius of the Sun. Default is [] (internal value is used). [m] (1x1)
(optional) Solar radiation pressure at 1 AU. Default is [] (internal value is used). [N/m^2] (1x1)
Potential [m^2/s^2]. (1xN)
CNES - DCT/SB