Terrestrial planets vs. Jovian planets Presented by: Nikita Bogdanov Terrestrial planets vs. Jovian planets

Topics Relevance Discovery Terrestrial Planets Jovian Planets Visual Representation Why? Temperature analysis Early condensation regions Why – summary Implications Video References Text Characteristics - Characteristics Picture Graphs x 2 YouTube embedded References

Relevance Understanding planetary formation in our own solar system can help us identify planets in other solar systems. New methods can be developed based on this understanding, and we can more accurately predict which types of solar systems would have which types of planets and why. This would aid in our understanding of the formation of the universe and a search for extraterrestrial life, however it be defined.

Discovery The discovery that there are both gas planets and terrestrial planets, as well as the analysis of why and how they formed, probably resulted from the study of many individuals and groups about the formation of our solar system. By creating an accurate model of the formation and then placing in observations of the planets, a theory of why and how terrestrial and Jovian planets formed could be developed.

Terrestrial Planets Composed mostly of rock or metal Solid surfaces Slower rate of spin Weaker magnetic field Located in the inner solar system Less massive More dense Less satellites and minimal rings

Jovian Planets Mainly Hydrogen and Helium Larger in diameter Faster rate of spin More powerful magnetic fields Located in outer solar system More massive Less dense More likely to have satellites or rings

Visual representation

Why? - Distance from the sun Asteroid belt separates Jovian and Terrestrial planets - Properties of their composition Gasses are light and can be “blown away” Evaporative temperatures of gasses compared to rocks and metals (temperatures dependant on distance from sun) mean different condensation regions within the solar system, and a clear “boundary” of planet types

Solar system temperature as a function of the distance from the sun Temperature analysis Evaporation temperatures Solar system temperature as a function of the distance from the sun

Early condensation regions

Why - summary Inner solar system: - Due to heat and premature solar wind lighter elements/gasses could not condense to form planets. Heavier elements made up any planets. Terrestrial planets are smaller because gas is predominate in the solar system. Outer solar system - Colder temperatures and less extreme environment allows for condensation of lighter elements. Silicates and ice are also available to form solid cores of gaseous planets. Large cores are then able to better hold surrounding gasses.

Implications We live on an inner solar system planet. Although the solar system has “settled down” since the formation of our star, there are still many threats to our planet such as asteroids, meteors, and comets. Because gas planets are more massive, and reside in the outer solar system, they can effectively gravitationally attract space threats from the outer solar system before they can hit earth. This is good for the progression of life as it is, on our planet.

Planetary Formation

Creation of the Solar System

References http://www.pa.msu.edu/courses/2005spring/ISP205/sec-1/L02-21.pdf - Graphics: slide 2, slide 3, slide 6, slide 7 - Information http://www.nineplanets.org/overview.html - Graphics: slide 4 http://www.plutomission.com/solar-system.htm - Graphics: slide 1 http://planet.fhda.edu/DACAstr/Harr4s/TerrJov.htm http://astronomy.swin.edu.au/~lgermany/SAOprojects/Project51.htm

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