Genetologic Research

The Three Body Problem is the mathematical problem of finding the positions and velocities of three massive bodies, which are interacting each other gravitationally, at any point in the future or the past, given their present positions, masses, and velocities. An example would be to completely solve the behavior of the Sun-Jupiter-Saturn system, or that of three mutually orbiting stars. It is a vastly more difficult exercise than the two-body problem. In fact, as Henri Poincaré (1854-1912) and others showed, the three-body problem is impossible to solve in the general case; that is, given three bodies in a random configuration, the resulting motion nearly always turns out to be chaotic: no one can predict precisely what paths those bodies would follow.

Watch here: The Tree Body Problem animation

Genetologic Research Nr. 6, 2003 (300cm x 300cm x 300cm)

Maarten Vanden Eynde

Three wooden (oak) beams are manually bended by fire and water during a three week lasting ‘torture-session’. After being liberated from the bending-machine, the beams stay in their forced position. The thee bodies are photographed in a certain way, but can change position without loosing their inter-relating balance. Various positions have been tried and just a few points of view bring them into a harmonious equilibrium. Any change or random elaboration creates chaos or disharmony.

The Universal Law of Gravitation has several important features. First, it is an inverse square law, meaning that the strength of the force between two massive objects decreases in proportion to the square of the distance between them as they move farther apart. Second, the direction in which the force acts is always along the line (or vector) connecting the two gravitating objects.
In 1687 Sir Isaac Newton first published his Philosophiae Naturalis Principia Mathematica (Mathematical Principles of Natural Philosophy) which was a radical treatment of mechanics, establishing the concepts which were to dominate physics for the next two hundred years. Among the book’s most important new concepts was Newton’s Universal Law of Gravitation. Newton managed to take Kepler’s Laws governing the motion of the planets and Galileo’s ideas about kinematics and projectile motion and synthesize them into a law which governed both motion on earth and motion in the heavens. This was an achievement of enormous importance for physics; Newton’s discoveries meant that the universe was a rational place in which the same principles of nature applied to all objects.

Maarten Vanden Eynde

‘Between two objects, let’s say A and B, there is a point where the gravitation of both objects is working with equal force (L1 point, named after Lagrange). This point is balancing between the two attracting masses. If it is slightly bending towards A or B is will be attracted more by either one of them. It can only move from it’s frozen position, without loosing it’s equal balance, if A and B change mass simultaneously. The mass A is loosing, B has to gain.

Time is always moving. When you read this word, it became history already. The future is catching up instantly. The present is an untouchable point always on the move.
If time would be a linear experience, and A would be the past and B the future, than the point hanging in the middle would be the present. The past is getting longer and longer (or bigger and bigger) so in order for this point to be equally drawn to both A and B, it needs to be moving towards the future. The past is getting bigger and the future is getting smaller. And on top of that the speed of this process is accelerating. Just like the birth of matter during the big bang, time was created at the same time and moves equally with the expanding universe; faster and faster to it’s final destiny. Will this be the end or a new beginning?’

The Lagrangian points (also Lagrange point, L-point, or libration point), are the five positions in interplanetary space where a small object affected only by gravity can theoretically be stationary relative to two larger objects (such as a satellite with respect to the Earth and Moon). They are analogous to geosynchronous orbits in that they allow an object to be in a “fixed” position in space rather than an orbit in which its relative position changes continuously.

Read the rest of this entry »