CL_fo_srpAcc

Description

• Perturbing acceleration (relative to an inertial frame) due to solar radiation pressure (SRP).

  The acceleration is directed from the Sun to the considered position and is inversely proportional to the distance squared.

  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 they are, 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.

Parameters

pos:

Position vector (from any position) [m]. (3xN or 3x1)

pos_sun:

Sun position (same origin as pos) [m]. (3xN or 3x1)

coefp:

SRP coefficient (cp*area/mass) [m^2/kg]. (1xN or 1x1)

ecl:

(optional, boolean) %t if eclipses are taken into account; %f otherwise. Default is %t. (1x1)

er:

(optional) Equatorial radius of eclipsing body. Default is %CL_eqRad. [m] (1x1)

ersun:

(optional) Equatorial radius of the Sun. Default is [] (internal value is used). [m] (1x1)

p0:

(optional) Solar radiation pressure at 1 AU. Default is [] (internal value is used). [N/m^2] (1x1)

acc:

Acceleration [m/s^2]. (3xN)

Authors

• CNES - DCT/SB

See also

• CL_fo_srpPot

• CL_gm_eclipseCheck

Examples

pos = [7000.e3; 0; 0]; // ECI pos_sun = CL_eph_sun(CL_dat_cal2cjd(2000,3,21)); // ECI coefp = 1.5 * 10 / 1000; CL_fo_srpAcc(pos, pos_sun, coefp, %t)