Physics Of Kepler 's 3rd Law

the moon 's orbit around the Earth, and the planets ' motions around the Sun. The

For Body 2 T^2/r^3 was 1.99E-5, for Body 3 it was 1.97E-5 and for Body 3 is was 1.97E-5. For Body 4 this was 1.85E-5. The data helps support the fact that the T^2/r^3 should be the same for all planets because the numbers were all relatively similar, especially for Bodies 2 and 3 which were identical and thus proved Kepler’s Law of Harmony, which states that T^2/r^3 should be the same for all planets orbiting the same central body.

The Law of ellipses, which means that each planet travels around the sun in an ellipses.

And in 1618 Johannes Kepler confirms his previously rejected discovery of the third law of planetary motion (he first discovered it on March 8 but soon rejected the idea after some initial calculations were made).

One of the first thing that he came up with was he made three laws, later known to be called Kepler’s laws. The first law he came up with is that planets rotate in elliptical paths around the sun. Which leads to his second finding and then later became known as his second law, he figured out that planets rotations are faster as they get more near the sun, then slower as they get further away from the sun. His third and final law dealt with the distance between the planet and the sun and how long it completed an orbit around the sun. Kepler used basic and simple mathematics to figure out how planets move, which proves him to be a very intelligent man at his time and in history. Kepler’s discoveries as well as many other astronomers put him and

This star catalog relies heavily on that of Hipparchus (129 BC), and in the majority of cases Ptolemy simply converted Hipparchus’s description of the location of each star to ecliptic coordinates and then shifted these values by a constant to account for precession over the intervening centuries. These two books also discuss the construction of a star globe that adjusts for precession. The remaining five books, the most original, set forth in detail geometric models for the motion of the five planets visible to the naked eye, together with tables for predicting their positions at any given time.” (The Editors of Encyclopædia Britannica,

Kepler used Mars to find out that when it was closer to the sun, it moved faster than when it was farther away, therefore forming the second law. The second law, known as the law of areas, states that a line drawn from planet to sun sweeps out equal areas in equal time. The third law, known as the law of period, states that the square of any period of any planet is proportional to the cube of the semimajor axis of its origin. These laws helped describe the motion of the planets and are still in effect

That's when his first law was made and explained in his book Astronomia Nova. Kepler took all of the information from his years of research, and used it to explain the orbits of the planets. He discovered that all planets orbit in ellipses (which means they move in an oval rotation) and that the sun was rotates on its own axis. These three statements later became known as Kepler's Laws of Planetary Motion. The laws state that the planets move around the sun in elliptical orbits, that the further away a planet was from the sun, the slower it would move, and some information about gravity.

“Oh no, a small field of asteroid the size of Pluto is heading towards Earth on a direct collision course!” The Earth and all of its inhabitants are now facing certain extinction. What are the Earth’s inhabitants to do? Is it possible to move the planet out of the way in time? Fortunately for humanity, there are many ways to actually change the Earth’s orbit both plausible and unrealistic, but one must completely understand the physics behind each option so that no mistakes are made and we fully avoid suffering any consequences. First background information on our planet needed, Earth has been around for 4.54 billion years, it has a mass of 5.98x10^24 kg, a diameter of 12756 km, a velocity of about 67000 mph, and is about 149,597,890 km away from the Sun. To most this doesn’t sound like a simple task, not knowing the trick is using Earth’s orbit. An orbit is the gravitationally curved path of an object around a point in space, for example the path of a planet around the center of a star system, like in our Solar System (Encyclopedia). In order to change the orbit of a planet, one must consider the difference forces that can influence the planet’s orbit: direct contact, gravitational assistance, solar sails, and the possible but not exactly plausible forces.

In today's world, we have very advanced technology. There have been many new technological and medical advancements as we entered the new century. The Internet allows us to shop, talk, and find valuable information on very scarce topics, and even check stocks with a simple click of a button. Medical advancements had recently been discovered on "The Human Genome Projects," the first gene was mapped and within a short period of time we will have mapped out all the genes in a human chromosome. This is absolutely amazing because we will now be able to reveal the many causes of serious deadly diseases. Throughout the years, we have gained the technology to send astronauts into space to gather new information about our

With the calculations above and the findings from the lab experiment, it can be concluded that an increase in acceleration due gravity results in an overall increase in energy. Using the calculations for Earth as our baseline, it was found that the increased acceleration due to gravity found on Jupiter resulted in an increase in energy while the decreased acceleration due to gravity found on the Moon resulted in the lowest amount of energy. Interestingly, when looking at the final values of kinetic and gravitational potential energy on Earth and on the Moon, it is found that the former is lower than the latter. However, when analyzing the data taken from the simulation on Jupiter, it is found that the kinetic energy is actually less than the gravitational potential. This possibly occurred as the

His first law states, “The orbits of the planets are ellipses, with the Sun at one focus of the ellipse.” As shown in Figure 1, The Sun is not at the focus of the ellipse, but is instead at one focus [usually there is nothing at the other focus of the ellipse]. The planet then trails the ellipse in its orbit, which implies that the Earth-Sun distance is continually changing as the planet goes around its orbit. Kepler’s second law states, “The line joining the planet to the Sun sweeps out equal areas in equal times as the planet travels around the ellipse.” As shown in Figure 2, an imaginary line from the center of the sun to the center of a planet sweeps out the same area in a given time. This means that planets move faster when they are closer to the sun. Kepler’s third and final law states, “The time taken by a planet to make one complete trip around the sun is its period. The ratio of the squares of periodic times for two planets is equal to the ratio of the cubes of their mean distances from the sun.” Kepler’s third law indicates that the time taken by a planet to orbit the Sun increases quickly with the radius of its orbit ("Johannes Kepler: The” 1-4). Kepler’s laws challenged Aristotelean and Ptolemaic astronomy. His statement that the Earth

Planets have mass and therefore have an effect on their stars orbit causing it to wobble. The wobble in the case of a pulsar star is seen as the periodic delay in the arrival of the pulses from the pulsar star (Wolszczan 1994). Due to the nature of a Pulsar star we can detect perturbations in its orbit through its pulses but to detect perturbations in other stars orbits, astronomers use a stars radial velocity.

After Tycho’s death, his assistant, young mathematician Johannes Kepler used Tycho’s observations and came up with his First Law that orbits of the planets are elliptical instead of round like Copernicus believed. With his Second Law, Kepler stated that the speed of the planets depends on their distance from the sun which helped English astronomer and physicist Isaac Newton, to come up with his Law of Universal Gravitation.

Orbital mechanics is the application of ballistic and celestial mechanics to motion, especially pertaining to rockets and spacecraft. Many famous physicists and mathematicians have helped develop equations, formulas, and laws to understand different aspects of orbital mechanics; such as Newton with centripetal force and the gravitational constant (GM) and also Kepler and his three laws of planetary motion. Though my interest did not sprout from who was involved with orbital mechanics, but the orbital mechanics themselves. I’ve always had an interest in astronomy and physics, and this seems like the perfect combinations of both.