Johannes Kepler Research Paper
Johannes Kepler, who was born December 27, 1571 and died on November 15, 1630. He created the three major laws of planetary motion. These three laws are called the Law of Ellipses, the Law of Equal Areas, and the Law of Harmonies.
Kepler's first law is called the Law of Ellispes or the Law of Orbits. This law states that planets move in elliptical orbits with the sun at one focus. Think of the elliptical shape as a part of a cone. This is the shape of the orbit that becomes an inverse square force, which is an intensity in the gravity field. The eccentricity is the ratio of the distance between the foci to the major axis of the ellispe, which is basically the orbit of each planet. Since the formula is Ra= a(1+e) and Rp= a(1-e), when e=0 for the orbit, we can then calculate the orbit for each planet. These measurements go from largest to smallest. Let's say Mecury's orbit eccentricity is 0.206. Mecury has the shorter orbit than Pluto, who has an orbit eccentricity of 0.25. It has a longer orbit.
Kepler's second law is called the Law of Equal Areas or the Law of Areas. This law states the closer a planet is to the sun, the faster it orbits. The further the planet is away from the sun, the slower it orbits. The equation that is used for this law is C= r x r' = r x v. This law has been proven by going to space and by scientific calculation over …show more content…
This law states that the orbital period of a planet is proportional to the cube of the semi-major axis of the ellipse. This law's equation consists of calculating the planet's orbital period and average distance. This law calculates the speed of a planet's orbit. This law also describes that there is a T^2/R^3 for any satellite for any planet. The equation Kepler used for this law is T^2= 4(3.14)^2/GM (a^3). Even though this is a good approximation for the orbit, there is a more precise equation that we use today, T^2=
Kepler's first law is called the Law of Ellispes or the Law of Orbits. This law states that planets move in elliptical orbits with the sun at one focus. Think of the elliptical shape as a part of a cone. This is the shape of the orbit that becomes an inverse square force, which is an intensity in the gravity field. The eccentricity is the ratio of the distance between the foci to the major axis of the ellispe, which is basically the orbit of each planet. Since the formula is Ra= a(1+e) and Rp= a(1-e), when e=0 for the orbit, we can then calculate the orbit for each planet. These measurements go from largest to smallest. Let's say Mecury's orbit eccentricity is 0.206. Mecury has the shorter orbit than Pluto, who has an orbit eccentricity of 0.25. It has a longer orbit.
Kepler's second law is called the Law of Equal Areas or the Law of Areas. This law states the closer a planet is to the sun, the faster it orbits. The further the planet is away from the sun, the slower it orbits. The equation that is used for this law is C= r x r' = r x v. This law has been proven by going to space and by scientific calculation over …show more content…
This law states that the orbital period of a planet is proportional to the cube of the semi-major axis of the ellipse. This law's equation consists of calculating the planet's orbital period and average distance. This law calculates the speed of a planet's orbit. This law also describes that there is a T^2/R^3 for any satellite for any planet. The equation Kepler used for this law is T^2= 4(3.14)^2/GM (a^3). Even though this is a good approximation for the orbit, there is a more precise equation that we use today, T^2=