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ASTR 101 Astronomy
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ASTR 101 Astronomy
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Course Code: ASTR101
University: University Of Washington
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Country: United States
Question:
The Solar System has two types of planets, and any theory that aspires to explain the development of the Solar System must explain this. What is the nebular theory’s explanation for this. In a paragraph or two explain how the terrestrial planets and the gas giant planets came to be?
Answer:
Formation of terrestrial planets occurred in the inner solar system whereby the planets were formed from condensation of microscopic solid particles. These microscopic particles through electrostatic forces clumped together because of their small sizes (Montmerle, Augereau, & Chaussidon, 2006). The particles contained 0.6% of the material in the solar nebular thus not enlarging so much hence exerting little pulling effect on hydrogen and helium gases. Presence of hydrogen and helium in the terrestrial planets was eliminated by the heat from the sun due to their proximity to sun. As the particles grew in mass, their gravitational forces increased thus accelerating their growth leading to formation of planetesimals. Planetesimals enlarged to optimal size where they could not be held together by gravity anymore. After a while there was a change of orbits of the planetesimals due to gravitational encounters between them. The largest ones survived and grew into terrestrial planets which include Mercury Earth and Mars.
Gas giant planets were formed beyond the frost line. Solar nebular contained 1.4% components of hydrogen and 0.6% rock and metal. The availability of ice in plenty led to growth of planetesimals to bigger sizes (Cole, 2013). Hyrogen and helium gases were trapped by the adequately large cores which later turned out to be thick atmosphere and solid cores of Jupiter, Saturn, Uranus and Neptune.
References
Cole, G. H. (2013). Planetary Science: The Science of Planets around Stars. Michael M. Woolfson.
Montmerle, T., Augereau, J., & Chaussidon, M. (2006). Solar System Formation and Early Evolution: the First 100 Million Years. Earth, Moon, and Planets, 39–95.
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