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1. Homework/Quiz etc Problematic email addresses: fkim1@umbc.eduevak1@umbc.edunbecke1@umbc.edu (this one ok, I have an alternative) -Mailbox full errors for these A class email noted L1 + L2 and answer to homework on the webpage http://www.jca.umbc.edu/~turner/2003_phys316.html Homework will not be graded, but same and similar questions will appear in exams and quizzes. QUIZ next Tuesday -at start of lecture, 45 minutes. Bring a calculator. Will cover last weeks, todays and some of Thursdays material. Closed book! Lecture 3

2. Review of Kepler Kepler’s First Law:  The orbit of each planet about the Sun is an ellipse withthe Sun at one focus Lecture 3

3. Orbits Lecture 3

4. Review of Kepler Kepler’s Second Law:  As a planet moves in its orbit around the Sun, itsweeps out equal areas in equal times Lecture 3

5. Review of Kepler Kepler’s Third Law: P2=R3 where P is the period in years & R is the semi-major axis in AU (1 AU is Earth-Sun dist) Lecture 3

6. Review of Kepler So, Kepler parameterized the planetary orbits, without understanding why things were as they are… and P2=R3 only true using certain units (years and AU, all Earth-related measures) -in general P2= k R3 and the physics hidden in the constant, k, was not understood. Lecture 3

7. Galileo Galilei - The Telescope At the same time as Kepler proposed his laws of planetary motion, Galileowas proving planets really didmove around the Sun, supporting Copernicus model Circa 1600, - still 3 objections to a heliocentric solar system withnoncircular orbits.  All were rooted in the beliefs of Aristotle. -The Earth could not be moving because if it were, all the objects on it would be left behind as it moved. -The heavens were thought to be perfect and unchanging -If the Earth orbits the sun, we ought to be able to see stellar parallax. Lecture 3

8. Galileo Galilei - The Telescope In 1609 Galileo Galilei starts using the telescope for astronomy-took the basic telescope used for terrestrial viewing and turned it into a scientific instrument Lecture 3

9. Galileo Galilei - The Telescope Letter from Galileo reporting the discovery of Jupiter’s moons… The fact they orbit Jupiter and not Earth challenged the idea of a favored position for the Earth Lecture 3

10. Galileo Galilei - The Telescope Observations showed phases for Venus, proving it must orbit the Sun and not the Earth Lecture 3

11. Galileo Galilei - The Telescope Showed the Sun had changing sunspots-adding weight against the view of a perfect and unchanging heavens Lecture 3

12. Galileo Galilei - The Telescope Summary, 1609: Galileo starts using the telescope for astronomy Discovers: -phases of Venus (it orbits the Sun) -satellites of Jupiter (they orbit Jupiter) -mountains on the moon -sunspots Celestial bodies clearly seen to be complex, imperfect and changing-supporting Copernican/heliocentric models in 1632 Galileo published “Dialogue on Two World Systems” strongly supporting the Copernican system Lecture 3

13. Galileo Galilei - Relativity Galileo also added to scientific understanding with some new ideas, realized force is not responsible for motion, but for changes in motion:- He also postulated - velocity is not absolute, - speed of a falling body is independent of weight, i.e “Galileo's Principle of Equivalence” (later) - a theory of relativity all (mechanical) experiments performed in inertial frames will give the same results These are cornerstones of Einstein's theories of relativity. Lecture 3

14. A Few Reminders/ Simple Concepts Speed conveys how fast one is going Velocity conveys speed and direction -can change velocity without changing speed Acceleration/deceleration describes the change in velocity (g=9.8m/s/s) Momentum describes the product mass x velocity (note mass is amount of matter comprising a body, weight is the sum of accelerating forces on a body) Force describes a change in momentum Lecture 3

15. Simple Concepts of Motion Angular Momentum the product mass x velocity x radius for an object moving in a circle (or orbit) Lecture 3

16. Inertial Frames - Reminder An inertial frame is one in which under the influence of no forces, an object will remain at rest or in uniform motion (elevator scenario 1) Accelerating (or rotating) frames not inertial frames. Given the universal force of gravity, no body can actually be under the influence of no forces. However the concept of inertial frames is still useful since: - effect of gravity can be very small. Thus physical insight can be obtained (e.g. Einstein's Special Theory of Relativity). -valid under Einstein's General Theory of Relativity: a frame in free-fall under the influence of gravity is an inertial frame. Lecture 3

17. Galileo’s Principle of Equivalence Inertial and gravitational mass are equivalent Gravitational Mass measure of how strongly a body is affected by the force of Gravity It is the mg in Newton's universal law of gravitation when the body is a distance R from another body of mass M: Force = G mg M R-2 Inertial Mass is measure of how strongly the body is accelerated (by A) by a given force. It is the mi in Newton's 2nd-law: Force = mi A Lecture 3

18. Galileo’s Principle of Equivalence The inertial massmidetermines how the body accelerates as a results of the application of any force. The gravitational massmg determines how the body "feels" a gravitational force (and how much of a gravitational force it generates). The fact that one can equate the above two forces: mi A = G mg M R-2 Then if mi equals mg then one sees that the acceleration (due to the force of gravity) is independent of mass. Galileo:If all forces apart from gravity can be ignored, all objects fall at the same rate Lecture 3

19. Galileo’s Principle of Equivalence This equivalence is a mathematical confirmation of Galileo's experiments (cannonball & feather etc) and can be used to derive Kepler's 3rd law of planetary motion The fact that mi and mg are equal is often referred to as Galileo's Principle of Equivalence - used and extended by Albert Einstein (1915) as he formulated General Relativity. Indeed the whole of General Relativity rests on Einstein's Principle of Equivalence Lecture 3

20. Physical Cosmology Arrives Isaac Newton's discovery that it is gravity which plays the vital role of determining the motion of the planets "signifies the the arrival of the first physical cosmology" Newton's universal theory of gravity contains the concept of action at a distance Many scientists did not accept this concept. Newton's law of gravity was not immediately accepted universally. Instead many scientists preferred to stick with the prevailing idea of the time (e.g. Rene Descartes) that forces work through contact. Lecture 3

21. Isaac Newton (1643-1727) Formulated a theory of mechanics & gravity that explained the solar system with remarkable accuracy! Realized that gravity responsible for the motion of the Moon and planets. Newton’s law of universal gravitation Every mass attracts every other mass Force drops off with square of distance Kepler’s laws are a direct consequence of Newton’s law of gravity Lecture 3

22. Orbits under gravity Gravity also allows us open hyperbolic or parabolic orbits (like those of comets) Lecture 3

23. Newton Universal Law of Gravitation Every mass attracts every other mass through the force called gravity The force of attraction between 2 objects is directly proportional to the product of their masses. Doubling the mass of one body doubles the force of gravity between the two Fg=GM1M2/r2 r -dist between centers G grav const Fg force of grav. attraction Lecture 3

24. Isaac Newton In 1687, Isaac Newton publishes Philosophiae Naturalis Principia Mathematica Stephen Hawking, in A Brief History of Time notes "probably the most important single work ever published in the physical sciences.” Newtons 3 laws of motion: 1:Every body continues in its state of rest or (straight-line) motion until compelled to do otherwise by an external force (ie. intertial frames) So, if a body is not acted on by any forces, its vel remains const- conservation of momentum 2:Force equals Mass times Acceleration -defines inertial mass as the degree by which a body resists being accelerated by a force 3:To every Force there is an equal (& opposite) Reaction Remember these! Lecture 3

25. Isaac Newton N1:Every body continues in its state of rest or (straight-line) motion until compelled to do otherwise by an external force (inertial frames) Comes from Galilean Relativity- Galileo was the first to state this in his ‘’law of inertia’’ Concept: Frames of references at rest or moving with constant velocity are called inertial frames. Newtons laws hold within these frames of reference In non-inertial frames you may be fooled into thinking there are forces acting on freely moving bodies Lecture 3

26. Isaac Newton N2:Net force is proportional to mass x acceleration An object subject to n forces experiences a net force Fnet =  Fi = ma (summed over i=1…n) However, a=dv/dt - giving us Fnet = m dv/dt = d (mv)/dt = dp/dt Vectors, quantities having magnitude and direction, are in boldface Lecture 3

27. Isaac Newton N2:Net force is proportional to mass x acceleration Thus N2 may be expressed as - the net force on an object equals its rate of change of momentum Fnet= dp/dt Lecture 3

28. Isaac Newton N3:For every action there is an equal and opposite reaction action and reaction are forces F12= -F21 Lecture 3

29. Law of Universal Gravitation Using his 3 laws of motion+ Keplers 3rd law - Newton was able to find an expression describing the force which holds the planets in their orbits. Consider a circular orbit of mass m about much larger mass M (M >> m) . Recall K3:- P2= kr3Remember this one! r is dist. between the objects and k is a constant, in circular orbit P is P = 2r/v (v is velocity of the mass m) substitute 2nd eqn into first to get 4 2r2/v2 = kr3 Lecture 3

30. Law of Universal Gravitation 4 2r2/v2 = kr3 -rearrange terms and mult. through by m mv2/r= 42m/ kr2 left hand side is recognizable as the centripetal force for circular motion; thus F = 42m/ kr2 must be the grav force keeping m in orbit around M Now, the force exerted by m on M equal the mag of that exerted by M on m Lecture 3

31. Law of Universal Gravitation F = 42m/ kr2 Now, the force exerted by m on M equal the mag of that exerted by M on m -thus the form of the eqn should be symmetric w.r.t. exchange of m and M Expressing the symmetry explicitly and grouping the constants into a new one, G we arrive at the law of universal gravitation found by Newton F = GMm/r2 G=6.67 x 10-11 m3 kg-1 s-2 SI units Lecture 3

32. Law of Universal Gravitation Law of universal gravitation F = GMm/r2 Remember this one! Gravitational force follows an inverse square law- doubling separation between two objects, grav attraction drops x 4 Lecture 3

33. Gravity due to Earth Law of universal gravitation F = GMm/r2 Remember this one! Consider mass m falling from height h above Earths surface, earths radius denoted R and mass M F = G M m/(R + h)2 h << R so F = G M m/R2 However, F =ma = mg thus g = G M /R2 Lecture 3

34. Gravity due to Earth g = G M /R2 M = 5.974 x 1024 kg & R = 6.378x 106 m gives acceleration due to Earths gravity g= 9.8 m s-2 Lecture 3

35. Gravitational Potential Energy Consider now the energy (work) req. to raise mass m to height h against grav. force, ie the change in potential energy of the system Uf - Ui = U = - F. dr(between ri & rf) where F is the force vector and ri & rf are initial and final position vectors dris the infinitesimal change in posn vector If gravitational force on m is due to mass M then U=  GMm/r2dr Lecture 3

36. Gravitational Potential Energy If gravitational force on m is due to mass M then U= GMm/r2dr evaluate the integral to give Uf - Ui = - GMm(1/rf - 1/ri)dr since we are interested in relative change in potential we can choose to define p.e going to zero at infinity , let rf approach infinity so Uf = 0 then (dropping subscripts) U= - GMm/r - gravitational p.e. Now, total mechanical energy of a particle is E= 1/2 mv2 - GMm/r Lecture 3

37. Escape velocity E= 1/2 mv2 - GMm/r can be used to calculate the escape velocity around mass M (>>m) by equating kinetic energy and grav. force 1/2 mv2 = GMm/r which may be solved for the velocity vesc = √(2GM/r) Remember this one! mass of escaping object does not appear! For earth vesc = 11.2km/s Lecture 3

38. Generalization of Keplers work Newton explained Keplers laws by solving the law of universal gravitation together w/ the laws of motion. Solved a pair of algebraic equations w/ use of calculus Newtons work showed Keplers first two laws apply to any object orbiting another under the force of gravity, or objects orbiting each other with their center of mass at one focus. Lecture 3

39. Newtons form of Keplers Third Law Newton also generalized Kepler’s third law as P2=42 R3 /G(M1+M2) Allowed Kepler’s Laws to be applied to moons and (much later) binary stars and extrasolar planets. Remember this one! Lecture 3

40. Very good, but not perfect.. Isaac Newton also contributed to science with - invention of the telescopes using mirrors - theories of light (colors & corpuscles) - development of calculus But Isaac Newton did not get it all right.. e.g. He incorrectly believed space & time were absolute and unaffected by the presence of objects His character was not perfect either -he had huge academic (& personal) rows with Robert Hooke (re: who 1st discovered the 1/r2 law) Gottfried Wilhelm von Leibnitz (re: who 1st discovered calculus) (e.g. see Steve Hawking“A Brief History of Time”) Lecture 3

41. Einstein's Principle of Equivalence Albert Einstein extended Galileo's Principle of Equivalence (inertial & gravitational masses are equal) i.e. acceleration and gravity cannot be distinguished. This led to Einstein's Principle of Equivalence The Laws of Physics are the same in a uniformly accelerated reference frame as in a uniform gravitational field Albert Einstein “The happiest thought of my life” The whole of General Relativity rests on this (testable) principle Lecture 3

42. Einstein's Principle of Equivalence The consequences of the Principle of Equivalence include - the effects of a gravitational force are indistinguishable from those present in an accelerated reference frame - there is an (accelerating) reference frame in which the effects of gravity are not experienced (falling elevator) - the path of light is "bent" by gravity - clocks run "slow" under the influence of gravity gravitational "redshift" of light waves - gravity affects anything carrying energy (E=mc2) ...more later on GR Lecture 3

43. Overview Background reading -Chapter 3 … things to know (for a quiz next week) -Contributions to astronomy from the ancient Greeks -Ptolemy and his model -Copernicus, how did he change our view and what was his first model -What is meant by the Copernican & Perfect Cosmological Principles -Kepler, how did he progress from the heliocentric model using circular orbits Lecture 3

44. Overview -What are Keplers 3 laws, what factors does the orbital period depend on? -What were the major achievements of Galileo? -What was Newtons contribution to astronomy? -Should be able to remember & use Newtons Law of Universal Gravitation and Keplers Laws (esp. newtons general version of K3) -& calc escape velocities Lecture 3