Simulum 


Here the physical and mathematical background of the first simulation are sketched. Star distributionWhat is the initial star distribution? The first simple approch is a homogen (but random) distribution on a three dimensional sphere. All stars are of equal mass and brightness. ProjectionTo get an visual impression we must choose a viewpoint. We also have to decide about our viewing direction and orientation. These informations fix the position of our virtual photo plate. Now each star position is mapped through the viewpoint onto the photo plate.
BrightnessThe brightness of the star makes an little spot on our virtual photo plate. The brightness of the spot depends only from the distance between star and viewpoint. The photo plate is a pixel matrix, that has some implications:
Movement of viewpointCurrently the viewpoint simply circles around the middle of the sphere. Movement of starsThe stars will have to move according to Newton's gravitional law. Because there is no analytical solution for the differential calculus problem, we have to use approximations. With a small time unit we calculate the star movements. We have to be carefull, that the stars don't get to close to each other. If this happens the calculation error has a great impact on our dynamical system. To renormalize the system we use the conservational laws of energy and impulse. Currently we are not carefull. We just use Euler's method to calculate star positions and velocities. The following formulas are used:
This is a very simple single step method. Some more information about better approximation methods to solve the Nbody problem can be found at Bob Jenkins' web site and parallel Nbody simulations. 