I , <¡2^2*



(12-24d) (12-24e)

12.2 Three-Axis Attitude Determination

Gerald M. Lemer

Three-axis attitude determination, which is equivalent to the complete specification of the attitude matrix. A, is accomplished either by an extension of the geometric techniques described in Chapter 11 or by a direct application of the concept of attitude as a rotation matrix. If the spacecraft has a preferred axis, such as the angular momentum vector of a spinning spacecraft or the boresight of a payload sensor, it is usually convenient to specify three-axis attitude in terms of the attitude of the preferred axis plus a phase angle about that axis. This asymmetric treatment of the attitude angles is usually justified by the attitude sensor configuration and the attitude accuracy requirements, which are generally more severe for the preferred axis. We refer to this method as geometric three-axis attitude determination because the phase angle is computed most conveniently using spherical trigonometry. Alternatively, in the algebraic method, the attitude matrix is determined directly from two vector observations without resorting to any angular representation. Finally, the q method provides a means for computing an optimal three-axis attitude from many vector observations. In this section we describe these methods for the computation of three-axis attitude.

12.2.1 Geometric Method

The geometric method is normally used when there is a body axis—such as the spin axis of a momentum wheel, a wheel-mounted sensor, or the spacecraft itself, about which there is preferential attitude data. Either deterministic techniques, as described in Chapter 11, or differential correction techniques, as will be described in Chapter 13, may be used to compute the attitude of the preferred axis. The phase angle about the preferred axis is then computed from any measurement which provides an angle about that axis.

In many cases, the geometric method is required because the sensor measurements themselves (e.g., spinning Sun sensors or horizon scanners) define a preferred spacecraft axis and provide only poor azimuthal information about that axis.

Figure 12-5 illustrates^ the^ geometric method. The reference axes are the celestial coordinates axes, X7, Y„ and Z7. We wish to compute the 3-1-3 Euler angles, <f>, 9, and ip, which define the transformation from the celestial to the body

Shapes Sphere
Fig. 12-5. Détermination of the Phase Angle, +

coordinates, XB, Yfl, and ZB. The Guler angles <f> and 0 are related to the attitude (a, 6) of the preferred body axis, ZB, by

where the right ascension, a, and the declination, 8, are obtained by using any one-axis attitude determination method. <j> defines the orientation of the node, N. The phase angle, is computed from the azimuth, if/s, of the projection of a measured vector, S (e.g., the Sun or magnetic field) on the plane normal to ZB. Let M be the projection of S on the plane normal to ZB and P=ZflxN. Application of Napier's niles (Appendix A) to the right spherical triangles SMN and SMP yields

P ■ S = M • S cos(90° - = M • S sin <p0 (12-26b)

which may be rewritten as*


P = ( - cos 0 sin <t>, cos 0 cos <j>, sin 0 )T (12-28b) The phase angle, if/, is then given by

As a more complex example of the geometric technique, we consider the three-axis attitude determination for the CTS spacecraft during attitude acquisition as illustrated in Fig. 12-6. The spacecraft Z axis is along the sunline and the spacecraft Y axis (the spin axis of a momentum wheel) is fixed in inertial space on a great circle 90 deg from the Sun.. An infrared Garth horizon sensor has its boresight along the spacecraft Z axis and measures both the rotation angle, QE, from the Sun to the nadir about the spacecraft Y axis and the nadir angle, % from the spacecraft Y axis to the Earth's center. We wish to compute the rotation angle, about the sunline required to place the spacecraft Y axis into the celestial X- Y plane as a function of the following angles: the Sun declination in celestial coordinates, 8S; the clock anglelf or difference between the Earth and Sun azimuth in celestial coordinates, Aa = a£—as; and either measurement SlE or i). As shown in Fig. 12-6, <bs is 180 deg minus the sum of three angles:

*Note that M-S>0 by the definition of M. If M-S = 0, \f/a is indeterminate because S provides no phase information about ZB. If M-S>0, ifo is obtained unambiguously because the quadran's of both sini/ia and cosi/>0 are known.

t For the synchronous CTS orbit, the azimuthal difference or clock angle is zero at local midnight and decreases by 15 dep/hnur.

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