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The Origin of Modern Astronomy  Nicolai Copernicus
The Origin of Modern Astronomy Nicolai Copernicus

... method’ (formulate an hypothesis, test the hypothesis against reality, verify or discard the hypothesis if data do not confirm it) marks the birth of Modern Science, and Astronomy ...
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... 49. The source of the Sun’s energy is combing hydrogen atoms to form helium atoms, this process is called nuclear fusion 50. The temperature/heat inside a star determines the star’s color or brightness 51. After a super giant star goes supernova it can turn into one of two things, a neutron star or ...
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... would be much more luminous than the Sun), life would be hard-pressed to evolve much even if it managed to originate. As a reminder, the earliest traces of life on Earth go back to something like 800 million years after the formation of the Solar System. Life might have originated before then, but t ...
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... 5. Galileo Galilee discovered by dropping two objects from the Leaning Tower of Pisa that objects fall at the same rate regardless of their ________. The reason that a feather and bowling ball does not fall at the same rate on earth is because of ________________________. 6. Mass is the amount of __ ...
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... For objects near the earth's surface, gravitational potential energy is usually calculated with the familiar equation Ug = mg∆y , with a zero point at some convenient location the ground, the oor, the table top, etc. For objects well above the earth's surface, in orbit or other celestial objects, ...
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... much younger than our sun. Most of them apparently are not an isolated single star as our sun is but are part of systems of two or more stars orbiting around a common center of mass. So too there are other galaxies and clusters of galaxies different from our own in size, shape, and direction of moti ...
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... • Saturn's interior composition is primarily that of simple molecules such as hydrogen and helium, which are liquids under the high pressure environments found in the interiors of the outer planets, and not solids. ...
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Formation and evolution of the Solar System



The formation of the Solar System began 4.6 billion years ago with the gravitational collapse of a small part of a giant molecular cloud. Most of the collapsing mass collected in the center, forming the Sun, while the rest flattened into a protoplanetary disk out of which the planets, moons, asteroids, and other small Solar System bodies formed.This widely accepted model, known as the nebular hypothesis, was first developed in the 18th century by Emanuel Swedenborg, Immanuel Kant, and Pierre-Simon Laplace. Its subsequent development has interwoven a variety of scientific disciplines including astronomy, physics, geology, and planetary science. Since the dawn of the space age in the 1950s and the discovery of extrasolar planets in the 1990s, the model has been both challenged and refined to account for new observations.The Solar System has evolved considerably since its initial formation. Many moons have formed from circling discs of gas and dust around their parent planets, while other moons are thought to have formed independently and later been captured by their planets. Still others, such as the Moon, may be the result of giant collisions. Collisions between bodies have occurred continually up to the present day and have been central to the evolution of the Solar System. The positions of the planets often shifted due to gravitational interactions. This planetary migration is now thought to have been responsible for much of the Solar System's early evolution.In roughly 5 billion years, the Sun will cool and expand outward many times its current diameter (becoming a red giant), before casting off its outer layers as a planetary nebula and leaving behind a stellar remnant known as a white dwarf. In the far distant future, the gravity of passing stars will gradually reduce the Sun's retinue of planets. Some planets will be destroyed, others ejected into interstellar space. Ultimately, over the course of tens of billions of years, it is likely that the Sun will be left with none of the original bodies in orbit around it.
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