Universal law of gravitation distance,numerology soul mate prediction,make a free call online no download,jyotish astrology in hindi 720p - 2016 Feature

06.03.2014
The Sun's gravitational pull keeps the planets of the Solar System orbiting around it.
Newton did not discover gravity, as the popular belief holds, but expanded on the work of earlier scientists such as Galileo. In the centuries after Newton’s lifetime, the law of universal gravitation was used to predict the locations of planets and natural satellites that had not yet been discovered. By the 20th century, scientists had discovered minor inconsistencies in the law of universal gravitation. The drawback to Einstein’s Special Theory of Relativity, however, is that it is “special” in the respect that it only considers the effects of relativity to an observer moving at constant speed. At around this time (1907), he also started to wonder how Newtonian gravitation would have to be modified to fit in with special relativity, and how the effects of gravity could be incorporated into the formulation. Initially, Einstein had been puzzled by the fact that Sir Isaac Newton’s Law of Universal Gravitation, which had stood undisputed since 1687, appeared to be fundamentally incompatible with his own Special Theory.
Thus, according to this theory, gravity is relatively strong when objects are near each other, but weakens with distance, and the bigger the bodies, the more their force of mutual attraction. Gravity is the organizing force for the cosmos, crucial in allowing structure to unfold from an almost featureless Big Bang origin. Even before Newton, the great 17th Century Italian physicist Galileo Galilei had shown that all bodies fall at the same rate, any perceived differences in practice being caused by differences in air resistance and drag. Newton, however, had assumed that the force of gravity acts instantaneously, and Einstein had already shown that nothing can travel at infinite speed, not even gravity, being limited by the de facto universal speed limit of the speed of light. Einstein’s ground-breaking realization (which he called “the happiest thought of my life”) was that gravity is in reality not a force at all, but is indistinguishable from, and in fact the same thing as, acceleration, an idea he called the “principle of equivalence”. The influence of gravity also creates effects of time dilation (see the section on the Special Theory of Relativity for a more detailed discussion of time dilation), sometimes referred to as "gravitational time dilation". On a much smaller scale, because gravity is slightly stronger closer to the centre of the Earth, then theoretically time passes more slowly for someone living on the first floor of an apartment block than for someone living at the top. So, gravity, Einstein realized, is not really a force at all, but just the result of our surroundings accelerating relative to us.
In essence, the law states that all objects exert a gravitational pull on all other objects. Motion at constant speed is clearly a very special case, and in practice bodies change their speed with time.


His resulting General Theory of Relativity, over ten years in the making (it was published in 1916), has been called the greatest contribution to science by a single human mind. Newton’s theory (permanently linked, at least in the popular mind, with his observation of an apple falling from a tree) stated that every massive body exerts an attractive force on every other massive body, a force which is proportional to the product of the two masses and inversely proportional to the square of the distance between the bodies. This “inverse-square law” is quite sophisticated enough to explain why a cannonball fired horizontally travels further before hitting the ground the faster it is launched, why a certain minimum speed (about 11.2 kilometres per second) would be required to allow objects to break out of Earth’s gravity and into orbit and why the planets travel in an elliptical orbit around the Sun (although not quite sophisticated enough to predict the slight anomaly in Mercury’s orbit). Although it is a very weak force (feebler than the other fundamental forces which govern the sub-atomic world by a factor of 1036 or 1,000,000,000,000,000,000,000,000,000,000,000,000), it is a cumulative and consistent force which acts on everything and can act over large distances. Galileo’s famous (and probably apocryphal) experiment involving the dropping of two balls of different masses from the Leaning Tower of Pisa was repeated with even more dramatic results in 1972 when a hammer and a feather were dropped together on the airless Moon and, just as Galileo had predicted, both hit the ground together.
Furthermore, Newton had assumed that the force of gravity was purely generated by mass, whereas Einstein had shown that all forms of energy had effective mass and must therefore also be sources of gravity. He realized that if he were to fall freely in a gravitational field (such as a skydiver before opening his parachute, or a person in an elevator when its cable breaks), he would be unable to feel his own weight, a rather remarkable insight in 1907, many years before the idea of freefall of astronauts in space became commonplace. That, and the feeling of his feet being glued to the ground just as they would be in Earth’s gravity, would be enough to convince the astronaut that the acceleration of the spaceship was indistinguishable from the pull of gravity on the Earth. As Einstein predicted, the closer a body is to a large mass, with a commensurately large gravitational pull, the slower time runs for it. With modern atomic clocks of sufficient accuracy, differences in the passage of time at different altitudes above sea level (and therefore different distances from the Earth's centre of gravity) can be measured, and even the tiny differences due to the changing shape of the Earth as the tidal force of the Moon pulls and stretches it. Or, perhaps a better way of looking at it, gravity is a kind of inertial force, in the same way as the so-called centrifugal force is not a force in itself, merely the effect of a body’s inertia when forced into a circular path.
It states that all objects are attracted to each other by gravity; the force of the attraction depends on the mass of the objects and decreases based on the distance between them.
Instead, he used the moon’s orbit around the Earth to check and confirm his calculations over a span of 20 years. Objects with a great deal of mass have stronger areas of gravity, or gravitational fields, which is why objects and people are attracted to the Earth, but not noticeably to each other.
One aspect of the law Newton could not explain was how gravitational force is conveyed between objects. Einstein realized that, in effect, the masses of celestial bodies not only affect each other, but the fabric of space-time around them. Einstein wanted to generalize his theory to consider how a person sees another person who is accelerating relative to them.


So, even though gravity can be effectively ignored by chemists studying how groups of atoms bond together, for bodies more massive than the planet Jupiter the effects of gravity overwhelm the other forces, and it is largely responsible for building the large-scale structures in the universe. A real-life example of gravitational time dilation can be seen in GPS systems in geo-synchronous orbits above the Earth, which need to constantly adjust their clocks to account for time differences due to the weaker gravity they experience compared to that on the Earth's surface (it is estimated that their accuracy would be out by as much as 10 kilometers a day without this adjustment).
In order to rationalize this situation, though, Einstein was to turn our whole conception of space on its head, as we will see in the next section. The law of universal gravitation was detailed in his groundbreaking book Principia Mathematica, published in 1687. The gravitational pull decreases as distance increases; this decrease can be precisely measured, and is known in physics as an inverse-square law. Other fundamental forces, such as electromagnetism, work because sub-atomic particles travel between the objects, attracting them to each other. The body of mass m2 in turn attracts the body of mass m1 with the same force F towards its centre O2.
Thus, gravity squeezes together massive bodies like our own Sun, and it is only the explosive outward energy in the Sun’s ultra-hot core that holds it in hydrostatic equilibrium and stops it from collapsing into a super-dense white dwarf star. Universal gravitation is the force that keeps planets and satellites locked in orbit, rather than traveling freely about the universe. A similar particle for conveying gravity, the graviton, has been described in theory, but remains undiscovered more than 300 years after Newton’s work.
For practical applications such as rocket launches, the law of universal gravitation is still accurate and much easier to calculate than the effects of relativity.
Suppose the distance between their centers is‘d’ then, according to Newton’s universal law of gravitation, we have:Where G is called a proportionally constant or universal gravitational constant.
For example, if a spaceship were to orbit close enough (but not too close!) to a hugely massive object such as a supermassive black hole, the gravitational effects may be significant enough to slow down time for the occupants compared to elsewhere, effectively allowing them to travel into the future.



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