http://www.imdb.com/title/tt0106447/quotes
Memorable quotes for
Bodies, Rest & Motion (1993)
Beth: I have to find happiness in myself.
Sid: No, that's wrong. People tell you that, but it's wrong. I've lived with people who have that 'happiness from within', that happiness... it's just them being pleased with themselves. It's not enough. It's a lonely thing.
From 11/26/1976 to 4/9/1993 ("Bodies, Rest & Motion") is 14 days, 4 months, 16 years
'1-4416'
From 3/3/1959 to 7/16/1963 is: 4 years, 4 months, 1 week, 6 days
'4416'
http://www.imdb.com/title/tt0106447/
Bodies, Rest & Motion (1993)
Release Date: 9 April 1993 (USA)
Tagline: Nick is leaving. Beth is staying. Carol is waiting. Sid is painting.
Phoebe Cates ... Carol
http://en.wikipedia.org/wiki/Motion_%28physics%29
In physics, motion means a continuous change in the position of a body relative to a reference point, as measured by a particular observer in a particular frame of reference. Until the end of the 19th century, Isaac Newton's laws of motion, which he posited as axioms or postulates in his famous Principia were the basis of what has since become known as classical physics. Calculations of trajectories and forces of bodies in motion based on Newtonian or classical physics were very successful until physicists began to be able to measure and observe very fast physical phenomena.
At very high speeds, the equations of classical physics were not able to calculate accurate values. To address these problems, the ideas of Henri Poincaré and Albert Einstein concerning the fundamental phenomenon of motion were adopted in lieu of Newton's. Whereas Newton's laws of motion assumed absolute values of space and time in the equations of motion, the model of Einstein and Poincaré, now called the special theory of relativity, assumed values for these concepts with arbitrary zero points. Because (for example) the special relativity equations yielded accurate results at high speeds and Newton's did not, the special relativity model is now accepted as explaining bodies in motion (when we ignore gravity). However, as a practical matter, Newton's equations are much easier to work with than those of special relativity and therefore are more often used in applied physics and engineering.
In the newtonian model, because motion is defined as the proportion of space to time, these concepts are prior to motion, just as the concept of motion itself is prior to force. In other words, the properties of space and time determine the nature of motion and the properties of motion, in turn, determine the nature of force.
In the special relativistic model, motion can be thought of as something like an angle between a space direction and the time direction.
In special relativity and Euclidean space, only relative motion can be measured, and absolute motion is meaningless.
An object is in motion when its distance from another object is changing.Whether the object is moving or not depends on your point of view. For example, a woman riding in a bus is not moving in relation to the seat she is sitting on, but she is moving in relation to the buildings the bus passes. A reference point is a place or object used for comparison to determine if something is in motion. An object is in motion if it changes position relative to a reference point. You assume that the reference point is stationary, or not moving.
Types of Motion
A pendulum exhibits Simple harmonic motion, or, motion that is constantly being accelerated towards a midpoint. Other types of motion include Linear motion and Reciprocation. Examples of naturally occurring motion are Brownian Motion (the movement of particles), and the orbits of planets.
http://en.wikipedia.org/wiki/Newton%27s_laws_of_motion
Newton's laws of motion are three physical laws which provide relationships between the forces acting on a body and the motion of the body, first compiled by Sir Isaac Newton. Newton's laws were first published together in his work Philosophiae Naturalis Principia Mathematica (1687). The laws form the basis for classical mechanics. Newton used them to explain many results concerning the motion of physical objects. In the third volume of the text, he showed that the laws of motion, combined with his law of universal gravitation, explained Kepler's laws of planetary motion.
Briefly stated, the three laws are:
An object in motion will remain in motion unless acted upon by a net force.
Force equals mass multiplied by acceleration.
To every action there is an equal and opposite reaction.
http://en.wikipedia.org/wiki/Kepler%27s_laws_of_planetary_motion
In astronomy, Kepler's laws of planetary motion are three mathematical laws that describe the motion of planets in the Solar System. German mathematician and astronomer Johannes Kepler (1571–1630) discovered them.
Kepler studied the observations of the legendarily precise Danish astronomer Tycho Brahe. Around 1605, Kepler found that Brahe's observations of the planets' positions followed three relatively simple mathematical laws.
Kepler's laws challenged Aristotelean and Ptolemaic astronomy and physics. His assertion that the Earth moved, his use of ellipses rather than epicycles, and his proof that the planets' speeds varied, changed astronomy and physics. Nevertheless, the physical explanation of the planets' behavior came almost a century later, when Isaac Newton was able to deduce Kepler's laws from Newton's own laws of motion and his law of universal gravitation, using his invention of calculus. Other models of gravitation would give empirically false results.
Kepler's three laws are:
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. His third law is based on the foundation left by Copernicus, because he uses a mathematical expression to show the correlation between T (time for one revolution) and D (distance from the sun).
Kepler's laws are formulated below, and are derived from Newton's laws, using heliocentric polar coordinates . However, Kepler's laws can alternatively be formulated and derived using Cartesian coordinates.
