Origin
of the Solar System
The interstellar gas cloud The collapse of the cloud caused it to rotate, increasing in speed as the cloud contracted. As the contraction continued, the cloud flattened and a disc formed around a central core of condensed matter. This configuration, known as a solar nebulae, would have resembled the shape of a typical spiral galaxy but was much smaller. As the gas and dust was pulled in toward the central condensation, the potential energy of the gas and dust was converted to kinetic energy as it was pulled towards the centre of the cloud and the temperature of the nebulae began to rise. Eventually, the temperature became great enough in the centre of the cloud for nuclear reactions to begin, thereby giving birth to a star, our Sun.
Formation of the planets and moons The planets forming close to the Sun could not hold onto their lighter more volatile molecules and elements, leaving the heavier molecules and elements like iron and the silicates to form the inner planets. There was much less heavier metals and silicate material than water available in the gas nebulae so the inner planets had less material from which to form and as a consequence formed much smaller and denser planets than their Jovian brothers. The outer Jovian planets forming in the solar nebulae at lower temperatures where ice could form were able to acquire much more mass than planets forming closer to the Sun. Once a planet achieved a large enough mass it could attract and retain large amounts of hydrogen and helium from the surrounding space. Hydrogen and helium are by far the most abundant elements in the Universe, and so planets forming further out in the nebulae become very massive indeed. The formation of the inner planets, including the Earth, was complete within 100 million years of the collapse of the interstellar gas cloud. The bombardment of planetary and satellite surfaces by debris left over from the initial formation of the planets continued for another 600 million years, adding small quantities to the original size of the planets. Such collisions still continue to take place today, but are much less frequent. Rings and moons of the gas planets Asteroids and comets The comets are representative of the material found in the outer Solar System. Most are extremely small, but some have been measured to be up to 400 kilometres in diameter. It is believed that billions of comets may exist far beyond Pluto. Pluto and Charon
It is generally agreed that the Solar System started to form around 5 billion years ago, with the Earth forming some 4.6 billion years ago. This is much younger than the Universe, which is now thought to be 12 - 15 billion years old.
|
|