An analysis of the evolution of solar system and the theories of the origin of the moon

describe the steps in the formation of the solar system according to the nebular theory

Material joining the central condensation gradually spirals inwards so that it is always in a near-Keplerian orbit around the central mass. Jeans found how a tidally affected star would distort and eventually lose a filament of material from the tidal tip.

Gases that didn't condense into grains were swept outward by radiation pressure and the stellar wind of the new Sun.

nebular theory of solar system formation

Google Scholar Goldreich, P. Various mechanisms have been suggested for transferring angular momentum Larson Tidal theory[ edit ] Attempts to resolve the angular momentum problem led to the temporary abandonment of the nebular hypothesis in favour of a return to "two-body" theories.

III ed. It is concluded that in many cases the resonances must already be produced at the times when the bodies formed.

Five origins of solar system

In the final stage, planetesimals merged to form the small handful of terrestrial planets. The initial system would not have been coplanar and indeed there could have been retrograde orbits although, with motion in a resisting medium and collisions to remove a minority population of retrograde objects, the system could have evolved to the present state. In the original form of the theory, each floccule had about three times the mass of the Earth so many of them had to combine to form the giant planets. McCrea turned this apparent problem into an asset. McCrea's starting point was a cloud of gas and dust that was to form a galactic cluster. They are separated into groups according to whether they are gross features or relate to details of the system. Urey's model[ edit ] American chemist Harold Urey , who founded cosmochemistry, put forward a scenario [3] in , , , and based largely on meteorites and using Chandrasekhar's stability equations and obtained density distribution in the gas and dust disk surrounding the primitive Sun. The temperature of the cloud was 3. Google Scholar Hirayama, K.
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Structure and evolutionary history of the solar system, I