╨╧рб▒с>■  "$■   !                                                                                                                                                                                                                                                                                                                                                                                                                                                ье┴ ┐Єjbjbjкjк д╚╚Є      ]ЇЇЇЇЇЇЇ$$$$$ 0 $ъHHHHHHHH╤╙╙╙╙╙╙,■ЇЄ № ЇHHHHH ╚ЇЇHHH╚╚╚HjЇHЇH╤ЇЇЇЇH╤╚╚╚РVЕ@ЇЇ╤< с*▄╢$$▓┼ PHY111 Seat Activity: Johannes Kepler's Third Law of Planetary Motion Write out and briefly explain in your own words the equations for centripetal force and Newton's Law of Universal Gravitation. Include a sketch for each explanation. Set them equal to one another, and solve for orbital velocity of an object in circular orbit. Use circular geometry to determine v for Uniform Circular Motion and set this v2 equal to that from part 1. Jupiter's four largest moons were discovered by Galileo in 1610. The innermost Moon called Io is about half the size of the Earth. Io orbits an average distance of 422,000 km from the center of Jupiter and has an orbital period of 1.769 days. 3. The Keplerian Ratio is defined as K = r3 / T2 for any satellite orbiting a planet or moon. It depends only on the mass M of that planet. Calculate the Keplerian Ratio KJupiter for any satellite of Jupiter. 4. Use the above information to find an equation for the mass of Jupiter. Solve it. Your answer should be about 1027kg (Extra credit) What is the orbital radius of a Satellite in geosynchronous earth orbit? The Earth's mass is 5.98 x 1024 kg. Geosynch satellites remain apparently 'suspended' over the equator when viewed from the Earth's surface. ЮЯстцчdkАВЄ¤∙¤∙¤∙¤ї¤∙¤∙¤CJ(H*CJ(H*CJ FGNO╗╝╜╛╡╢КЛМ  ёЄчч╠ч╠ччччччччччччч▒ч & F ╞) ╨аp@ р░АP Ё└!Р$ & F ╞) ╨аp@ р░АP Ё└!Р$ ╞) ╨аp@ р░АP Ё└!Р$FGNO╗╝╜╛╡╢КЛМ  ёЄ№Ўє     & 00P░╨/ ░р=!░8"░8#Р8$Р8%░|HH╪( с т∙FG(№HH╪(d'`Р [:@ё :Normal 1$dЁCJPJmH nH <A@Є б<Default Paragraph FontJ■ё ЄJ Word4095Null 1$dЁOJPJQJmH nH Є(  ЄЄЄЄ'CE╛╟S\ckFTИРЇ╛їЇ  Daniel L. MacIsaac4Hummel 10GB: CrsesFall2000:PHY111:Kepler's Laws WBDaniel L. MacIsaac8Hummel 10GB: CrsesFall2000:PHY111:Kepler's Laws WB.BIGDaniel L. MacIsaac;Hummel 10GB:Temporary Items:AutoRecovery save of Kepler's LDaniel L. MacIsaac;Hummel 10GB: CrsesFall2000:PHY111:WBs:Kepler's Laws WB.BIGDaniel L. MacIsaac.Hummel 10GB:Temporary Items:Word Work File A 2Daniel L. MacIsaac;Hummel 10GB: CrsesFall2000:PHY111:WBs:Kepler's Laws WB.BIGDaniel L. MacIsaac;Hummel 10GB: CrsesFall2000:PHY111:WBs:Kepler's Laws WB.BIGDaniel L. MacIsaac;Hummel 10GB: CrsesSpr2001:PHY111:WBs:Kepler's Laws WB.BIG                            Д|ДД■╞|o(.Д|ДД■╞|o(.ДhДШ■╞ho(.               @(▓ ▌щ3┐Є0@GРTimes New Roman5РАSymbol3Р Arial3РTimes"AН╨hЮЫS&ЮЫS&ЗЪS&Ь|$>Gё├  EPHY111 Seat Activity: Johannes Kepler's Third Law of Planetary MotionDaniel L. MacIsaacDaniel L. MacIsaac■  рЕЯЄ∙OhлС+'│┘0└РШшЇ, HT p | И Фаи░╕'FPHY111 Seat Activity: Johannes Kepler's Third Law of Planetary Motion HY1Daniel L. MacIsaacyaniNormalLDaniel L. MacIsaacy2niMicrosoft Word 8.0y@F├#@R╬Ч░└@