The so named Bode's Law was published as a scientific law by Johann Elert Bode, German astronomer and Director of the Observatory of Berlin. But the study was originally made by Christian Freiherr von Wolf ( 1679 - 1754 ), German mathematician and philosopher, and divulged at 1766 by Johann Daniel Dietz, also known as Titius of Wittenberg ( 1729 - 1796 ), German teacher of physics of the University of Wittenberg, who verified the validity of the Wolf 's calculation. The Titius-Bode Law or Rule is the observation that orbits of planets in the solar system follow a simple arithmetic rule quite closely.

In 1768, Bode published his popular book, "Anleitung zur Kenntnis des gestirnten Himmels" [Instruction for the Knowledge of the Starry Heavens], which was printed in a number of editions. In this book, he stressed an empirical law on planetary distances, originally found by J.D. Titius (1729-96), now called "Bode's Law" or "Titius-Bode Law".

The following table compares the law's predictions with the actual distances, where the addition of Pluto is a modern modification.

Johannes Kepler (1571 - 1630 ) was born to a poor family, whose father finally settled to become a tavern keeper. He was a sickly child, and was withdrawn from school to help in the tavern and as a laborer in the fields. Because his family was Lutheran, Kepler was destined for the ministry. He was sent as a charity student to a protestant seminary, and later to a college where he received a Bachelor`s Degree. His evident intelligence earned him a scholarship to the University of Tubingen, where he studied theology and mathematics, and earned a Master`s Degree in Philosophy.

Kepler learned privately of the heliocentric view, which is the belief that the sun is the center of the planetary system, and other Copernican theories at the university. Kepler was forced to study this view privately because the church, as well as society, was adamant in its belief of the Ptolemaic Theory of a geocentric universe. This theory states that the earth is the center around which the heavenly bodies move. Eventually, he became an outspoken supporter in defense of the Copernican system. After his studies at the university, Kepler became a professor of mathematics. In 1600 he left the teaching profession to work as an assistant to Tycho Brahe, in Prague. It was in Prague, during his tedious study of the orbit of Mars, where Kepler developed his first two laws of planetary motion.

Kepler`s laws are three mathematical statements formulated by the German astronomer Johannes Kepler that accurately describe the revolutions of the planets around the sun. Kepler`s laws opened the way for the development of celestial mechanics, i.e., the application of the laws of physics to the motions of heavenly bodies. His work shows the hallmarks of great scientific theories: simplicity and universality.
The first law states that the shape of each planet`s orbit is an ellipse with the sun at one focus. The sun is thus off-center in the ellipse and the planet`s distance from the sun varies as the planet moves through one orbit. The second law specifies quantitatively how the speed of a planet increases as its distance from the sun decreases. If an imaginary line is drawn from the sun to the planet, the line will sweep out areas in space that are shaped like pie slices. The second law states that the area swept out in equal periods of time is the same at all points in the orbit. When the planet is far from the sun and moving slowly, the pie slice will be long and narrow; when the planet is near the sun and moving fast, the pie slice will be short and fat.
The third law resulted as a searched for a principle with that in mind. The third law states that, "the squares of the periodic times are to each other as the cubes of the mean distances." Kepler announced this law in 1619, fourteen years after the first two laws. It took him years to find the law to describe the distances of the planets to the sun. After much deliberation, Kepler arrived at the law that if T is the period of revolution of any planet and D is its mean distance from the sun, then T squared is equal to k multiplied by D cubed, where k is a constant, which is the same for all the planets. This third law was published in his book, The Harmony of the World. >

This formulation of the Titius Bode Law describe the revolutions of the planets around the sun:

T(k) = [(3*bin(k)+4)/10 ]^3/2