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The pressure of solar radiation on a spherical balloon satellite is proportional to its cross-sectional area. However, there is evidence to indicate that the PAGEOS satellite has not remained spherical, but is more nearly a prolate spheriod that is rotating about its minor axis. If this is true, the force of solar radiation incident upon its surface must be expressed in terms of the shape of the surface and its orientation to the sun. Furthermore, radiation reflected from the surface of an aspherical balloon will impart an additional force which can be large enough to significantly perturb the orbit. By starting with basic equations for the radiation forces on a flat plate and integrating over the sunlit portion of the surface, exact expressions are obtained for both the incident and reflected radiation forces on a stationary, prolate spheroidal satellite. These expressions are then used to develop power series expansions for the radiation forces on a rotating spheroid.
Geostationary or equatorial synchronous satellites are a daily reminder of our space efforts during the past two decades. The nightly television satellite weather picture, the intercontinental telecommunications of television transmissions and telephone conversations, and the establishrnent of educational programs in remote regions on Earth are constant reminders of the presence of these satellites. As used here, the term 'geo stationary' must be taken loosely because, in the long run, the satellites will not remain 'stationary' with respect to an Earth-fixed reference frame. This results from the fact that these satellites, as is true for all satellites, are incessantly subject to perturbations other than the central-body attraction of the Earth. Among the more predominant pertur bations are: the ellipticity of the Earth's equator, the Sun and Moon, and solar radiation pressure. Higher harmonics of the Earth's potential and tidal effects also influence satellite motion, but they are of second order when compared to the predominant perturbations. This volume deals with the theory of geostationary satellites. It consists of seven chapters. Chapter 1 provides a general discussion including a brief history of geostationary satellites and their practical applications. Chapter 2 describes the Earth's gravitational potential field and the methodology of solving the geostationary satellite problem. Chapter 3 treats the effect of Earth's equatorial ellipticity (triaxiality) on a geostationary satellite. Chapter 4 deals with the effects of the Sun and Moon on the satellite's motion while Chapter 5 presents the combined influences of the Sun, Moon and solar radiation pressure. Chapter 6 describes various station-keeping techniques which may be used to make geostationary satellites practically stationary. Finally, Chapter 7 describes the verification of the theory developed in Chapters 3, 4 and 5 by utilizing the Early Bird synchronous satellite observed data as well as its numerically integrated results.