The Waltz of the Planets and GravityGuiding QuestionsAncient astronomers invented geocentric models to explain planetary motionsSlide Number 4Slide Number 5Slide Number 6Slide Number 7Slide Number 8Slide Number 9Nicolaus Copernicus devised a comprehensive heliocentric modelA superior planet undergoes retrograde motion, as seen from Earth, when the Earth, moving faster, passes the planet in its orbitA planet’s synodic period is measured with respect to the Earth and the Sun (for example, from one opposition to the next)Slide Number 13Slide Number 14Tycho Brahe’s astronomical observations provided evidence for another model of the solar systemParallax – apparent difference in position of object viewed from two different locationsJohannes Kepler proposed elliptical paths for the planets about the SunKepler’s First LawSlide Number 19Kepler’s Second LawKepler’s Third LawGalileo’s discoveries with a telescope strongly supported a heliocentric modelSlide Number 23Slide Number 24Geocentric Model IssuesSlide Number 26Slide Number 27Isaac Newton formulated three laws that describe fundamental properties of physical realityNewton’s Laws IllustratedNewton’s Law of Universal GravitationNewton’s description of gravity accounts for Kepler’s laws and explains motion of all orbiting bodies Orbital MotionOrbits follow any one of the family of curves called conic sectionsSlide Number 34Gravitational forces between two objects produce tides in distant regions of the universeUnderstanding Tidal ForcesSlide Number 37Slide Number 38Slide Number 39Slide Number 40Slide Number 41Slide Number 42Jargon Du Jour1The Waltz of the Planets and Gravity2Guiding Questions1. How did ancient astronomers explain the motions of the planets?2. Why did Copernicus think that the Earth and the other planets go around the Sun?3. How did Tycho Brahe attempt to test the ideas of Copernicus?4. What paths do the planets follow as they move around the Sun?5. What did Galileo see in his telescope that confirmed that the planets orbit the Sun?6. What fundamental laws of nature explain the motions of objects on Earth as well as the motions of the planets?7. Why don’t the planets fall into the Sun?8. What keeps the same face of the Moon always pointed toward the Earth ?3Ancient astronomers invented geocentric models to explain planetary motions• Like the Sun and Moon, the planets were believed to move on the celestial sphere with respect to the background of stars• Most of the time a planet moves eastward in direct motion, in the same direction as the Sun and the Moon, but from time to time it moves westward in retrograde motion4• Ancient astronomers believed the Earth to be at the center of the universe• They invented a complex system of epicycles and deferents to explain the direct and retrograde motions of the planets on the celestial sphere56(Ptolemy)78910Nicolaus Copernicus devised a comprehensive heliocentric model• Copernicus’s heliocentric (Sun-centered) theory simplified the general explanation of planetary motions• In a heliocentric system, the Earth is one of the planets orbiting the Sun• The orbital sidereal period of a planet is measured with respect to the stars11A superior planet undergoes retrograde motion, as seen from Earth, when the Earth, moving faster, passes the planet in its orbit12A planet’s synodic period is measured with respect to the Earth and the Sun (for example, from one opposition to the next)131415Tycho Brahe’s astronomical observations provided evidence for another model of the solar system16Parallax – apparent difference in position of object viewed from two different locations17Johannes Kepler proposed elliptical paths for the planets about the Sun• Using data collected by Tycho Brahe, Kepler deduced three laws of planetary motion:– the orbits are ellipses– With Sun at one focus– Equal areas in equal times• a planet’s speed varies as it moves around its elliptical orbit – The period squared equals the semi-major axis cubed• the orbital period of a planet is related to the size of its orbit18Kepler’s First Law1920Kepler’s Second Law21Kepler’s Third LawP2 = a3P = planet’s sidereal period, in yearsa = planet’s semimajor axis, in AU22Galileo’s discoveries with a telescope strongly supported a heliocentric model• Galileo’s observations reported in 1610– the phases of Venus*– the motions of the moons of Jupiter*– “mountains” on the Moon– Sunspots on the Sun*observations supporting heliocentric model23• One of Galileo’s most important discoveries with the telescope was that Venus exhibits phases like those of the Moon• Galileo also noticed that the apparent size of Venus as seen through his telescope was related to the planet’s phase• Venus appears small at gibbous phase and largest at crescent phase24There is a correlation between the phases of Venus and the planet’s angular distance from the Sun58” 42”24”15” 10”25Geocentric Model Issues• To explain why Venus is never seen very far from the Sun, the Ptolemaic model had to assume that the deferents of Venus and of the Sun move together in lockstep, with the epicycle of Venus centered on a straight line between the Earth and the Sun• In this model, Venus was never on the opposite side of the Sun from the Earth, and so it could never have shown the gibbous phases that Galileo observed26• In 1610 Galileo discovered four moons of Jupiter, also called the Galilean moons or satellites• This is a page from his published work in 161027Telescope Photograph of Jupiter & the Galilean Moons28Isaac Newton formulated three laws that describe fundamental properties of physical reality• Called Newton’s Laws of Motion, they apply to the motions of objects on Earth as well as in space29Newton’s Laws Illustrated• A body remains at rest, or moves in a straight line at a constant speed, unless acted upon by an outside force– the law of inertia• The force on an object is directly proportional to its mass and acceleration– F = m x a• The principle of action and reaction– whenever one body exerts a force on a second body, the second body exerts an equal and opposite force on the first body30Newton’s Law of Universal GravitationF = gravitational force between two objectsm1 = mass of first objectm2 = mass of second objectr = distance between objectsG = universal constant of gravitation• If the masses