Keplar showed that there is a relationship between the planets distance from the sun and the time taken for one orbit (planets year). This is described in Keplars third law; the square root of the time taken to orbit the sun is proportional to the cube of the average distance between the sun.
Not at all. The planet's daily rotation is independent of its distance from the Sun.
The time gets longer. That's because the planets travel more slowly and they also have further to travel. The mathematical formula for this is in "Kepler's Third Law of Planetary Motion".
By this: The orbit of every planet is an ellipse with the sun at one of the foci. An ellipse is characterized by its two focal points; see illustration. Thus, Kepler rejected the ancient Aristotelean and Ptolemaic and Copernican belief in circular motion. A line joining a planet and the sun sweeps out equal areas during equal intervals of time as the planet travels along its orbit. This means that the planet travels faster while close to the sun and slows down when it is farther from the sun. With his law, Kepler destroyed the Aristotelean astronomical theory that planets have uniform velocity. The squares of the orbital periods of planets are directly proportional to the cubes of the semi-major axes (the "half-length" of the ellipse) of their orbits. This means not only that larger orbits have longer periods, but also that the speed of a planet in a larger orbit is lower than in a smaller orbit.
The speed of a planet varies with the distance from the Sun according to Kepler's Third Law, so that the planets closer to the Sun have higher orbital velocities. Since the gravitational effect of the Sun decreases with distance from it, the planets farther from the Sun do not have to move as rapidly to remain in orbit. (In fact, the speed is what establishes the orbit, not the other way around.) So the outer planets, in addition to having much farther to travel in their orbits, are also moving more slowly. This combination means that outer planets take very much longer to orbit the Sun than do the inner planets such as Earth. By comparison, the length of time it takes (in Earth years) for each of the outer planets to make one complete revolution around the Sun: Jupiter - 11.9 Earth years Saturn - 29.5 Earth years Uranus - 84 Earth years Neptune - 165 Earth years
The further a planet is from the sun the larger it's orbit is around the sun. Mercury's orbit is 223,700,000 miles and takes three Earth months to complete, while Jupiter's orbit is 3,037,000,000 miles and takes almost eleven Earth years to complete.
YES. However the relationship is not quite that simple. This is Kepler's third law. I'll give you a simplified version which assumes the planets orbits are circular, instead of being ellipses : The square of the length of the year is proportional to the cube of the planet's distance from the Sun.
There is a relationship between the planets distance from the sun and the time taken for one orbit (planets year), described in Keplers third law. The square root of the time taken to orbit the sun is proportional to the cube of the average distance between the sun.
Not at all. The planet's daily rotation is independent of its distance from the Sun.
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The answer depends on what characteristic of the planets you are interested in: their mass, radius, volume, length of orbit, average distance from the sun, etc.
The time gets longer. That's because the planets travel more slowly and they also have further to travel. The mathematical formula for this is in "Kepler's Third Law of Planetary Motion".
There is no direct relationship between the rotation of a planet (which governs day length) and a planets distance from the sun. The nature of the planets spin is more to do with the formation of the system early on, by large impacts of the more numerous bodies that would have been around.
By this: The orbit of every planet is an ellipse with the sun at one of the foci. An ellipse is characterized by its two focal points; see illustration. Thus, Kepler rejected the ancient Aristotelean and Ptolemaic and Copernican belief in circular motion. A line joining a planet and the sun sweeps out equal areas during equal intervals of time as the planet travels along its orbit. This means that the planet travels faster while close to the sun and slows down when it is farther from the sun. With his law, Kepler destroyed the Aristotelean astronomical theory that planets have uniform velocity. The squares of the orbital periods of planets are directly proportional to the cubes of the semi-major axes (the "half-length" of the ellipse) of their orbits. This means not only that larger orbits have longer periods, but also that the speed of a planet in a larger orbit is lower than in a smaller orbit.
The speed of a planet varies with the distance from the Sun according to Kepler's Third Law, so that the planets closer to the Sun have higher orbital velocities. Since the gravitational effect of the Sun decreases with distance from it, the planets farther from the Sun do not have to move as rapidly to remain in orbit. (In fact, the speed is what establishes the orbit, not the other way around.) So the outer planets, in addition to having much farther to travel in their orbits, are also moving more slowly. This combination means that outer planets take very much longer to orbit the Sun than do the inner planets such as Earth. By comparison, the length of time it takes (in Earth years) for each of the outer planets to make one complete revolution around the Sun: Jupiter - 11.9 Earth years Saturn - 29.5 Earth years Uranus - 84 Earth years Neptune - 165 Earth years
The further a planet is from the sun the larger it's orbit is around the sun. Mercury's orbit is 223,700,000 miles and takes three Earth months to complete, while Jupiter's orbit is 3,037,000,000 miles and takes almost eleven Earth years to complete.
The answer is given by Kepler's third law, which says that the length of the planet's year can be found from the average distance from the Sun. If T is the orbital period (the planet's "year") and D the average distance from the Sun: T2 is proportional to D3. By using the correct units this becomes simply T2 = D3 Thus: T = D1.5 This means, for example, that a planet at 4 astronomical units from the Sun would have a year length of 8 Earth years.
Different planets have different length orbits because they are at varying distances from the sun. The farther a planet is from the sun, the longer it takes to complete an orbit. This is due to the gravitational pull of the sun, which affects the speed at which planets travel around it.