How do planets move when they orbit the sun?

Question

I know why: the gravity pulls it in, but the question is: How does it create locamotion?

Answer 1

energy from the big bang spun a bunch of matter and a very very small portion of that energy is powering the 'Movement" of all bodiies in our universe. (except the space shuttle, which uses atittude jets..)

Answer 2

The assumption is that the rotation around the sun is the result of particles being captured during the creation of the solar system and their velocity results in an orbit when combined with the force of gravity. If a random piece of stuff is traveling in space at a few miles per hour and comes under the influence of the sun being formed, it does not drop straight in, but curves. It would head right out again, but if it hits something, the energy is shared and it may stay around, after bumping other objects ends up at the distance from the sun where its velocity and the acceleration due to gravity balance.

Answer 3

It does not at this stage. The orbital energy came from the collapse of the giant cloud of dust and gas that eventually formed our solar system.

While collapsing under its own gravity, all the particles would collide with each other, thereby distributing their kinetic energy. With time, an overall rotation was established (from the sum of all the random energies).

Once a rotation axis got fixed, the random kinetic energies distributed themselves along a disc perpendicular to the axis.

When the planets formed from the disc matter, they were already rotating at (more or less) the correct speed to remain in orbit.

Or, to rephrase it: objects that were not going at the correct speed eliminated themselves either by falling into the Sun or escaping to interstellar space.

Answer 4

Technically, they're falling, but they travel in a curved spacetime caused by the gravity of the sun. Astronauts also 'fall' by travelling in the curved spacetime caused by the gravity of the Earth.

Answer 5

Gravity doesn't "create" the locomotion of the planets.

Newton's First Law: a body in motion remains in motion.

Answer 6

Steam.

Answer 7

It is the result of the centripetal force and centrifugal force.

Answer 8

Kepler's laws of planetary motion, in their original form, describe the motion of planets around the Sun. However, not only do planets orbit the Sun, but the Moon orbits the Earth, the Galilean moons orbit Jupiter, and so forth. Since gravity, according to Newton, is universal, orbits must be a universal phenomenon. Newton was able to use his laws of motion and laws of gravity to make minor corrections to Kepler's laws of planetary motion, and to expand their scope, making them universally applicable.
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Consider Kepler's laws one by one.
FIRST LAW of planetary motion:
Kepler's version: The orbits of planets around the Sun are ellipses with the Sun at one focus.
Newton's revised version: The orbits of any pair of objects are conic sections with the center of mass at one focus.

Strictly speaking, the Earth doesn't orbit the Sun. As the Sun pulls on the Earth, the Earth pulls on the Sun with an equal but opposite force. Thus, both the Earth and the Sun are being accelerated, and both the Earth and the Sun are orbiting the center of mass of the Sun-Earth system. Imagine placing the Sun and Earth on a gigantic seesaw in a uniform gravitational field. In order for the seesaw to remain level, the balance point couldn't be midway between them; it would have to be much closer to the Sun, which is much more massive than the Earth. The center of mass is the point at which the seesaw would balance. The center of mass of a pair of objects is located on the line connecting the objects, and is closer to the more massive object. In the Sun-Earth system, the Sun is 330,000 times more massive than the Earth, and thus the center of mass is 330,000 times closer to the center of the Sun than to the center of the Earth; that's only 450 kilometers from the center of the Sun, buried deep within the Sun's interior. In the Earth-Moon system, the Earth is 81 times the mass of the Moon, and the center of mass is 4700 kilometers from the center of the Earth; it is inside the Earth, but a distant observer would be able to see the Earth going around on its tiny orbit at the same time the Moon goes around on its much larger orbit.

Newton was aware of the concept of an artificial satellite. To put an object (a cannonball or a weather satellite or a Space Shuttle) into orbit, you can launch it sideways (parallel to the surface of the Earth) with a speed v. The shape of the orbit depends on v; in every case, however, the orbit is a conic section. A conic section is one of a family of curves obtained by slicing a cone with a plane. A circle is a conic section, and so is an ellipse, a parabola, and a hyperbola.





Low initial speed for the satellite: closed orbit (circle or ellipse)
High initial speed for the satellite: open orbit (parabola or hyperbola)
So, not all orbits, as Newton recognized, are closed loops (an ellipse or circle). If an artificial satellite is launched at a high enough speed, it escapes the Earth altogether, and the path it traces is an open curve (a hyperbola or parabola, technically speaking).
Most artificial satellites are on nearly circular orbits. We can compute the speed at which a satellite must travel if it is on a circular orbit. This speed is called the circular speed, and is designated by the symbol vc. The gravitational acceleration felt by the satellite will be, from Newton's Law of Gravity and Second Law of Motion,
a = G m / r2
where m is the mass of the planet that the satellite is orbiting, and r is its distance of the satellite from the center of mass. (Since artificial satellites are always much much less massive than the Earth, in the case of a satellite orbiting Earth, it is safe to say that the center of mass is indistinguishable from the center of the Earth.) The acceleration required to keep a satellite with speed vc on a circular orbit of radius r is
a = vc2 / r
Set the two accelerations equal, and you find
vc2 / r = G m / r2
or, with a bit of algebra,
vc = (Gm/r)1/2 .

To take an example, the International Space Station is in a circular orbit about 370 kilometers above the Earth's surface (only 230 miles). Since the radius of the Earth is 6380 kilometers, that means the distance of the Space Station from the center of the Earth is r = 370 km + 6380 km = 6750 km = 6,750,000 meters. Using the mass of the Earth and G, you can compute the circular speed for the International Space Station:

vc = 7680 meters/second = 7.68 kilometers/second = 17,000 mph.
At this speed, it takes the Space Station only 92 minutes to complete one orbit.
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SECOND LAW of planetary motion:
Kepler's version: A line from a planet to the Sun sweeps out equal areas in equal time intervals.
Newton's revised version: Angular momentum is conserved.
Newton's revised version doesn't sound anything like Kepler's initial version! Nevertheless, Kepler's second law of planetary motion is the inevitable consequence of the conservation of angular momentum.

The angular momentum of an orbiting object is given by a simple formula:

L = m v r
where
L = angular momentum
m = mass of orbiting object
v = orbital speed of object
r = distance of object from center of mass
The statement ``angular momentum is conserved'' simply means that L remains constant as an object moves along its orbit. Since the mass m is also constant, this means that the product of the orbital speed v and the distance r must remain constant. As r gets smaller, the speed v must get bigger. As r gets larger, the speed v gets smaller. [The customary analogy is a spinning ice skater, who spins faster and faster as she pulls in her arms closer to her body.] Thus, conservation of angular momentum implies that PLANETS MOVE FASTEST WHEN THEY ARE CLOSEST TO THE SUN. Moreover, a careful mathematical analysis reveals that r and v vary in such a way that a line between an orbiting object and the center of mass sweeps out equal areas in equal times.
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THIRD LAW of planetary motion:
Kepler's version: P2 = a3 (when P is measured in years, and a in A.U.)
Newton's revised version: P2 = { 4 pi2 / [ G (m1+m2) ] } a3
In the above equations,

P = orbital period
a = semimajor axis of orbit
G = gravitational constant (6.7 x 10-11 in metric units)
m2 = mass of orbiting body
m1 = mass of other body in system
pi = 3.14159265...
The original version of Kepler's third law applies ONLY to objects orbiting the Sun. Newton's revision applies to ALL pairs of objects orbiting their center of mass. For planets orbiting the Sun, the mass of the planet (m2) is negligibly small compared to the mass of the Sun (m1). Even Jupiter, the biggest planet, has a mass which is only 1/1000 of the Sun's mass. Thus, the factor inside the curly brackets in Newton's revised formula reduces to
4 pi2 / ( G m1 )
where m1 is the mass of the Sun. This number is the same for all objects orbiting the Sun, and when you measure time in years and distances in astronomical units, it is equal to ONE. Thus, Kepler's third law in its original form is merely a special case of Newton's more general formula.
Note that Newton's form of Kepler's third law can be used to determine the mass of distant objects. For the Galilean moons of Jupiter, for example, we can measure their orbital periods (P) and the sizes of their orbits (a). Assuming that the masses of the Galilean moons are much smaller than the mass of Jupiter (which is quite correct), we can use Newton's form of the third law to find the mass m1 of Jupiter.


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(2) Kepler described HOW planets move; Newton explained WHY they move the way they do.
Kepler's laws are purely descriptive; they tell us how the planets move, but do not provide an explanation of the forces which affect their motion. On the other hand, Newton's laws of motion and law of gravity explain why the planets move the way they do.
Newton, using his UNIVERSAL laws of motion and law of gravity, was able to modify Kepler's laws of planetary motion so that they too are UNIVERSAL. They're not just for planets any more; in the revised form, they apply to any pair of objects moving freely under their mutual gravitational attraction.

Answer 9

idk????