The Truth About Gravity u Gravity is a phenomenon and results in a force which can accelerate objects with mass. u g = acceleration due to the force of gravity
The Importance of Being Gravity u Gravity has basic properties: –(1) It is long-ranged and can act over cosmological distances –(2) It supplies an attractive force between any 2 pieces of matter in the Universe. u Although extremely weak, –It wins over cosmological distances –Most important force for the understanding of the large scale structure + evolution of the Universe.
So, let us deal with GRAVITY Well need a bit of a history lesson: Brahe Kepler Newton Einstein Pay close attention, gravity has many implications!
1) The planets move about the sun in elliptical orbits with the Sun at one focus. 2) The radius vector joining a planet to the sun sweeps over equal areas in equal intervals of time. 3) The square of the time of one compete revolution of a planet about its orbit is proportional to the cube of the orbit's semi-major axis Keplers Laws of Planetary Motion
Isaac Newton u Born 1642, the year Galileo died u Loner, tinkerer, paranoid u 1665-1666 Plague was very good for him u Suffered mental breakdown 1675 u Math, Chemistry, Theology, Parliament u Died 1727 u Has his picture on the British pound note He put the physics and mathematics to Keplers Laws!
Universal Law of Gravitation u All objects in the Universe attract each other with a force that varies directly as the product of their masses and inversely as the square of their separation from each other. F = G m m F = G m m r gravity 1 2 2
General Relativity u Einsteins Theory of Gravity, published 1915 u Principle of Equivalence: Accelerations are indistinguishable from gravitational fields. They are equivalent. u So, for example, when you are in freefall (like in an orbiting Shuttle), your downward acceleration is just enough to cancel the gravitational force.
Einsteins View of Gravity u Gravity is due to the curvature of space time. u Space time is curved by mass.
Predictions Light would be bent by gravity S Tested by Arthur Eddington during solar eclipse. S Confirmed! u Emission of gravitational radiation by accelerating objects S Tested by observations of binary pulsars. S Confirmed to 14 decimal places!
Applications of Newtons 2nd Law and Einsteins GR u Projectile Motion u Pendulums u Black Holes
Projectile Motion Projectile - any object given an initial velocity which subsequently follows a path determined by the gravitational force acting on it, and by the frictional resistance of the atmosphere bullet shot from a gun, rocket after the fuel is exhausted, thrown or batted baseball
Trajectory Trajectory - the path followed by a projectile
Our Assumptions We will consider only short length trajectories so that: u Gravitational force is considered constant in magnitude and direction u Earth is an inertial system u Air resistance is negligible In other words, we will examine motion in a vacuum on a flat, non-rotating Earth. In physics, we call this creating an
First, the Forces u Only force acting on the projectile is its weight…remember we are in the Ideal Case. u X-axis is horizontal; y-axis is vertical; origin is point where projectile starts its free flight u So x-component of the force on the projectile is zero and y-component of the force is the weight, mg.
Acceleration Netwons 2nd law then tells us that the x- component of the acceleration is zero and the y- component is -g. In other words, trajectory is a combination of a horizontal motion with constant velocity and a vertical component with constant acceleration.
Result u Under these conditions, projectiles travel in trajectories which are parabolas. u You can derive the equation for the parabolic motion from Newtons Laws!
Pendulums mg T mg sin For small angles, sin Simple Harmonic Motion L x Period = 2 L/g Measure period of oscillation and length of pendulum, determine g!
Black Holes A huge great enormous thing, like like nothing. A huge big well, like a I dont know like an enormous big nothing … Piglet describes the Heffalump, Piglet describes the Heffalump, in Winnie the Pooh by A.A. Milne in Winnie the Pooh by A.A. Milne
History u Based on Newtons theory of gravity u Proposed independently by: –1783 Rev. John Mitchell –1796 Pierre Simon Laplace
Bending of Light D D R photon d d is the approximate distance the photon falls over the diameter D of an object with mass M
From Newton, We Know... F = ma = GMm/R 2 Solving for a, a = GM/R 2 If you accelerate at rate a for time t, you move a distance d of d = 1/2 at 2 Recall that t = D/c. Putting everything together, we see: d = 1/2 GMD 2 /(c 2 R 2 )
Solving the Equations D D R d d = 1/2 GMD 2 /(c 2 R 2 ) but D=2R and = d/D RESULT: = GM/c 2 R Using GR, we would get 4 GM/c 2 R!
Making the Prediction When you plug in the values for G, c, and the mass and radius of the Sun, you predict that light should be bent by 8.5 x 10 -6 radians. u This corresponds to 1.75 seconds of arc. u Eddington measured 1.75…probably.
Mass and Weight u Weight is a force. It is the resultant gravitational force exerted on a body with mass m by all the other bodies on the Universe. u Near Earths surface, the gravitational force from our planet dominates all others, so according to Newtons Laws, we can write: Weight = F g = G m M e / R 2 = mg where M e is the mass of the Earth and R is the radius of the Earth.
But also... u Since weight is a force, it is measured in units of force, namely Newtons. Remember what mass is measured in units of?
Remember This! u Mass is a fundamental, universal property. You have the same amount of mass no matter where you are in the Universe. The only thing that can change your mass is velocity…according to General Relativity. As you approach the speed of light, you become infinitely heavy. u Weight is not fundamental; its value depends on what your circumstances are in the Universe.