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| celestial body orbiting a star that is massive enough to be rounded by its own gravity, is not massive enough to cause thermonuclear fusion, and has cleared its neighbouring region of planetesimals. |
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| solid bodies orbiing around the planets |
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| four inner planets that are generally, smaller, densers, and are less massive |
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| large gassy planets rich in icy or gaseous hydrogen compounds |
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| large asteroid 1003 km in diameter that orbits the sun between mars and jupiter |
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| planets that are closer to the sun thatn earth; mercury and venus |
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| the passage of an inferior planet between the earth and the sun |
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| apparent retrograde motion |
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| phenomenon that occurs when mars seems to spin backwards for a short period before returning to normal orbit |
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| apparent retrograde motion |
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| phenonmenon that occurs when the earth passes mars in orbit for a short period, before falling back behind it again. |
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| epiycle model, extremely complicated, and needed to be constantly adjested for acuracy |
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| proposed circular motions of planets around the sun |
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| recorded planets' position into a vast data bank |
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| analyzed tycho's records; deduced elliptical orbits and laws of planetary motion |
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| made telescopic discoveries supporting Copernican model |
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| formulated laws of gravity and used them to explain elliptical planitary orbits |
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| kepler's first law of planetary motion |
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| each planet moces in an ellipse with the sun at one focus |
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| kepler's second law of planetary motion |
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| the line between the sun and planet sweeps over equal areas in equal intervals of time |
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| kepler's third law of planetary motion |
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| the ration of the cube of the semi major axis to the square of the planet 9 of revolution is the same for each planet |
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| what kepler's third law is also known as |
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| first write a row of 4s for each planet, then add the sequence 0,3,6,12, and so on doubling each time until you reach pluto. If you put the decimal point in the right place, you will get the acerage distance from the sun in AU approximately. |
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| newton's law of gracitation |
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| every particle in the universe attracts everyother particle with a force proportional to the product of their masses, and inversely proportional to the square distance between them |
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