Abstract: A method and system for processing graphics simulation data is disclosed. Initially, a group of three-dimensional visual models to be rendered in a graphics simulation are constructed. Data that are utilized to move and control elements of the graphics simulation are acquired. The acquired data are subsequently converted to an object oriented format having tables and functions by automatically resolving dependencies between inputs and outputs of each of internal objects with external inputs and external outputs, respectively. Next, a link is established between the data in the object oriented format using the independent and dependent variables and the elements of the graphics simulation. Finally, the data in the object oriented format are processed via a graphics simulation.

Abstract: A method and system for processing graphics simulation data is disclosed. Initially, a group of three-dimensional visual models to be rendered in a graphics simulation are constructed. Data that are utilized to move and control elements of the graphics simulation are acquired. The acquired data are subsequently converted to an object oriented format having tables and functions by automatically resolving dependencies between inputs and outputs of each of internal objects with external inputs and external outputs, respectively. Next, a link is established between the data in the object oriented format using the independent and dependent variables and the elements of the graphics simulation. Finally, the data in the object oriented format are processed via a graphics simulation.

Abstract: A method for simulating a celestial sphere in real-time within a data processing system is disclosed. Initially, information of an observer, such as date, time and longitude/latitude positions, are obtained. Then, a Julian Day and a Greenwich mean sidereal time are determined from the above-mentioned information. A local mean sidereal time is subsequently determined. Furthermore, a tilt angle about a celestial equator of a celestial sphere is determined by using the latitudinal position of the observer. The determined values provide a real-time representation of the position of the celestial sphere relative to the observer at a specific position on the earth.