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The SUN
The SUN

... The diameter of the sun is 1,390,000 km The mass is 1,989,030 kg The temperature of the sun is 15,600,000 k and 9,900 f on the surface The element helium was named after the sun. The sun is about 70% hydrogen and 28% helium, the other 2% is metals. Solar winds travel through the solar system at 450 ...
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... assumed. And finally we note also that the moon and the sun appear to move at varying speeds across the starry background -- again inconsistent with simple circular motion. Here is a reminder of what we mean by retrograde loops. If you were to go out night after night and look at the motion of Jupi ...
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... considered heresy at the time. A less fortunate astronomer named Giordano Bruno was burned at the stake. To understand why Galileo was treated leniently, perhaps one should understand that Galileo was well known not only to those who practice science, but to influential people of the society and eve ...
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... area beyond the immediate solar system with objects made mostly of ice and rock. It was predicted that as many as 50 Pluto-size objects and large may exist in this belt, so when not one, but two objects larger than Pluto were discovered, it was decided to re-define what a planet is, because the alte ...
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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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