Cool Software

A free, open-source software called Stellarium is probably a good place to start. Another free planetarium software is Celestia. It runs on Windows, Linux and Mac. This software not only shows you the sky from Earth, but also allows you to 'fly' to other locations and view the sky from there. For example, if copying a 500MB file from internal hard disk to USB drive, the data might be 'read' into the OS's RAM cache, and being written to the USB drive, and while it is still writing, the file is already reported as 'finished copying' and the speeding of copying is therefore stated inaccurately high.) – nonopolarity Jun 27 '12 at 2:14. 'Much like the Sun uses its gravity to pull the planets towards it, GRAVITY pulls you in and makes you want to play with it. Mac: OS X 10.10 or higher, Intel Core 2 Duo, 4 GB RAM; PC: Windows 7 or higher. And over 500 single-shot elements, recorded in up to seven velocity layers and with up to nine round-robins per drum. $ 149.00 Add to.

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Later the contains of this disk were pulled back towards the sun starting an orbit from the planets. The asteroids began to orbit in the asteroid belt and the moons found planets to orbit. This hypothesis, known as the nebular hypothesis, was first developed in the 18th century by Emanuel Swedenborg, Immanuel Kant, and Pierre-Simon Laplace.
The Solar System has done a lot of evolving since its initial form. Many moons have formed from circling discs of gas and dust around their parent planets, while other moons are believed to have formed independently and later been captured by their planets. Still others, as Earth's moon, may be the result of giant collisions. Collisions between bodies have occurred continually up to the present day and have been very important to the evolution of the Solar System.
The positions of the planets often shifted, and planets have switched places. This planetary migration now is believed to have been responsible for much of the Solar System's early evolution. The original placement of the planets is still unknown.
The final result of the migration has left us with eight planets. These eight, although very different in their own ways, can be separated into two groups, the inner and outer planets.
The inner planets are very small compared to the outer ones, Earth being the biggest with a diameter of 7,926 miles. Mercury is the smallest in the solar system with a diameter of 3,031 miles.
The outer planets, all made of gas are very large. Jupiter is the biggest planet in our solar system with a diameter of 88,846 miles, Neptune is the smallest of the outer planets with a diameter of 30,779 miles. Neptune being the smallest of the outer planets is still over 23,000 miles bigger in diameter than the largest of the inner planets Earth.
The main reason for the major differences in size between the inner and outer planets is because the inner planets are very dense caused by the density of the elements that make them up. Because the inner planets are so densely packed together, they are small but they are solid making them much easier to study because they have an actual surface. Although all inner planets can be stood on, only Earth has a survivable atmosphere.

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The atmospheres of the Outer Planets consist mostly of Hydrogen and Helium, with Methane also being present in the atmospheres of Uranus and Neptune. Other gases are present although in much smaller quantities. The outer planets do not have a solid surface, they are all made of gas, hence the nickname 'Gas Giants'.
The inner planets have a faster year just because they are closer to the sun making their lap shorter. Although a day on an inner planet is much slower then one on an outer ones. Uranus spins slowest, taking 17 hours and 14 minutes to spin on its axis. Jupiter takes only 9 hours and 55 minutes to spin on its axis. This rapid rotation causes Jupiter and Saturn to appear squashed, wider across the equator than from top to bottom.
The inner planets spin quite slowly compared to the outer ones. Earth spins the quickest, taking 23 hours and 56 minutes to spin on its axis. Venus takes 243 days to spin on its axis, spinning in an opposite direction to the other planets.
As incredible as these planets are their future is completely dependant on our sun's future. In about 5 billion years the Sun will burn all of the hydrogen in its core. Once this happens, the core will shrink under its own gravity, until it becomes so dense that the helium atoms will begin to collide to form carbon and oxygen. These collisions produce much more energy than the hydrogen fusion that powers the Sun today.

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The extra energy will cause big changes in the Sun. The core will become much hotter, causing the Sun to swell to over one hundred times its present size, swallowing up the planets Mercury and Venus. Even though the core will be hotter, the surface will be cooler than it is today, changing in color from yellow to red, becoming a red giant.
It will then cast off its outer layers as a planetary nebula, and leave behind it's corpse known as a white dwarf. But before that, the gravity of passing stars will gradually pull the outer planets away from the sun. Some planets will be destroyed, others ejected into space. Over the course of trillions of years, when a white dwarf, it is likely that the Sun will be left with none of the original planets, asteroids, or moons in orbit today.
'A Glimpse at the Future of Our Sun.' Universe Today. N.p., n.d. Web. 14 Feb. 2011.

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'How Did the Sun Form - Formation of the Sun & The Solar System.' Lifestyle Lounge - Online Lifestyle Magazine - Lifestyle Management Tips. N.p., n.d. Web. 14 Feb. 2011. .
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