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jw Fundamentals of Physics 2
Chapter 13: Newton, Einstein, and Gravity
Isaac Newton 1642 - 1727Albert Einstein 1872 - 1955
jw Fundamentals of Physics 3
Fundamentals of Physics
Chapter 13 Gravitation
1. Our Galaxy & the Gravitational Force
2. Newton’s Law of Gravitation
3. Gravitation & the Principle of Superposition
4. Gravitation Near Earth’s Surface
5. Gravitation Inside Earth
6. Gravitational Potential Energy
Path Independence
Potential Energy & Force
Escape Speed
7. Planets &Satellites: Kepler’s Laws
8. Satellites: Orbits & Energy
9. Einstein & Gravitation
Principle of Equivalence
Curvature of Space Review & SummaryExercises & Problems
jw Fundamentals of Physics 4
The World & the Gravitational Force
– Allowed matter to spread out after the Big Bang.
– Eventually pulled large amounts of mass together:
– Clouds of gas
– Brown dwarfs
– Stars
– Galaxies (The Milky Way, Andromeda)
– Clusters of Galaxies (“The Local Group”)
– Super Clusters
• “billions & billions” of galaxies and stars
– Big Bang - hydrogen, helium, lithium, & very little else
– Big Stars - burned out & exploded creating heavier elements - carbon, oxygen, iron, gold, . . .
– Gravity then pulled the sun & earth together
Gravity is a very weak force, but essential for us to exist!
jw Fundamentals of Physics 5
Physics ~1680
By now the world knew:
• Bodies of different weights fall at the same speed
• Bodies in motion did not necessarily come to rest
• Moons could orbit different planets
• Planets moved around the Sun in ellipses with the Sun at one focus
• The orbital speeds of the planets obeyed “Kepler’s Laws”
But why??? Isaac Newton put it all together.
jw Fundamentals of Physics 6
Newton’s Law of Gravitation
Every massive body in the universe attracts every other massive body through the gravitational force!
Newton (1665):
Gravity Force is weak!
G = 6.67 x 10-11 N m2 / kg2
Principle of superposition: net effect is the sum of the individual forces.(added vectorially).
221~
r
mmF
221
r
mmGF
jw Fundamentals of Physics 8
Measurement of the Gravitational Force
If two masses are brought very close together in the laboratory, the gravitational attraction between them can be detected.
G = 6.673 x 10-11 N m2 / kg2
(relatively poorly known: 1 part in 10,000)
Cavendish Experiment(~1760):
221
r
mmGF
jw Fundamentals of Physics 9
Gravitation Near Earth’s Surface
• The Earth is not uniform.
• The Earth is not a sphere.– An ellipsoid ~0.3%
• Earth is rotating.– Centripetal acceleration
FN-mag = m(-2R)
mg = mag-m(2R)
(measured wt.) = (mag. of gravitational force) – (mass x centripetal acceleration)
g = ag –2R
on equator difference ~ 0.034 m/s2
jw Fundamentals of Physics 10
Gravitation Near Earth’s Surface
r is the distance between the centers of the two bodies
Newton: The force exerted by any spherically symmetric object on a point
mass is the same as if all the mass were concentrated at its center.
221
r
mmGF
Newton had to invent calculus to prove it!
r
jw Fundamentals of Physics 11
Newton’s Law of Gravitation
Newton: The gravitational force provides the centripetal acceleration to hold the earth in its orbit around the sun:
2
2
r
mMG
r
vmF ES
jw Fundamentals of Physics 12
Newton: The gravitational attraction between the Earth and the Moon causes the Moon to orbit around the Earth rather than moving in a straight line.
Orbital Motion
jw Fundamentals of Physics 13
Gravitation Inside A Shell
Newton: gravitational force inside a uniform spherical shell of matter:
1 0 2 00 2 2
1 2
21 1
22 2
0
But:
0
m m m mF G G
r r
m r
m r
F
The forces on m0 due to m1 and m2 vary as ~1/r2, but the masses of m1 and m2 grow as r2, hence the two forces cancel out!
A uniform spherical shell of matter exerts no net gravitational force on a particle located anywhere inside it.
jw Fundamentals of Physics 14
Gravitation Outside A Shell
Newton invents calculus!!!
g dg
dgG dM
s
dM MdAA
MR R d
R
s r R r R
sds r R d
R s r sr
r r
r
2
2
2 2 2
2 2 2
2
4
2
2 2
2
cos
sin
cos
sin
cos
Gravitational acceleration at a distance r from a point particle!
Integrating from s = r - R to s = r + R:
g r G M
r 2
Newton: A uniform spherical shell of matter attracts a particle that is outside the shell as if all the shell’s matter were concentrated at its center.
jw Fundamentals of Physics 15
Gravitation Inside & Outside a Uniform Sphere
Newton: Consider the sphere as a set of concentric shells:
The gravitational force inside a uniform spherical shell of matter is zero.
Only the matter inside radius r attracts an object at that radius.
jw Fundamentals of Physics 16
Gravitation Inside Earth
Newton: A uniform spherical shell of matter attracts a particle that is outside the shell as if all the shell’s matter were concentrated at its center.
Hooke’s Law
F r~
m oscillates back & forth!
Newton: The gravitational force inside a uniform spherical shell of matter is zero.
rR
MGgr 3
rR
mMGFr 3
jw Fundamentals of Physics 17
Gravitational Potential Energy of a 2-Particle System
Gravity is a conservative force.
The work done by the gravitational force on a particle moving from an initial point A to a final point G is independent of the path taken between the points.
Gravity is a conservative force.
Potential Energy:
(attractive force) 2
M mF r G
r
r rU U W F r dr
r
mMGrU
Only U is important; the location of U = 0 is arbitrary.
Choose U = 0 to be the point at which the masses are far apart.
0U
M
m
r
G M mU U
r
jw Fundamentals of Physics 18
Escape Velocity
Consider a projectile of mass m, leaving the surface of a planet. The loses kinetic energy and gains gravitational potential energy.
Does not depend on the mass of the projectile nor on its initial direction (i.e. escape speed not escape velocity).
12
2 0
2
mv GM m
R
vG M
R
U GM m
R 0
E K U constant
K U 0
K mv 12
2 0
Escape Speed: When the projectile reaches infinity, it has no potential energy (U = 0) and no kinetic energy (stopped: v = 0): the total mechanical energy is zero.
jw Fundamentals of Physics 19
Escape Velocity
~ 25,000 mi/hr
E K U constant
rU
E
Escapes
Bound Orbit
No hydrogen & helium in the earth’s atmosphere: escvv
skmmsmgrve /2.11)1038.6)(/81.9(22 62
U rG M m
rE Choosing U 0
Escape Speed
jw Fundamentals of Physics 20
http://ww2.unime.it/dipart/i_fismed/wbt/mirror/ntnujava/projectileOrbit/projectileOrbit.html
jw Fundamentals of Physics 21
Tycho Brahe (1546-1601)
Johannes Kepler (1571-1630)
Planets & Satellites: Kepler’s Laws
Sun
Path of Mars across the sky.
jw Fundamentals of Physics 22
Planets & Satellites: Kepler’s Laws
– Equal Areas in Equal Times by sun-planet line.
Sun
Kepler’s Laws:
– Elliptical orbits with the Sun at one focus.
– T2 ~ r3 (Period & Mean Distance from sun)
jw Fundamentals of Physics 23
Kepler’s 1st Law
The Law of Orbits: All planets move in elliptical orbits, with the Sun at one focus.
ellipse - sum of distances from 2 foci is constant (2a).
eccentricity of earth = 0.0167 e = 0 circle (1 focus)
M m
Sun is very near one focus.
perihelion - closest point to Sum
aphelion - farthest point
jw Fundamentals of Physics 24
Kepler’s 2nd Law
The Law of Areas: A line that connects a planet to the Sun sweeps out equal areas in the plane of the plane’s orbit in equal times; that is, the rate dA/dt at which it sweeps out area A is constant.
slower faster
http://ww2.unime.it/dipart/i_fismed/wbt/mirror/ntnujava/Kepler/Kepler.html
jw Fundamentals of Physics 25
Kepler’s 2nd Law
The Law of Areas: A line that connects a planet to the Sun sweeps out equal areas in the plane of the plane’s orbit in equal times; that is, the rate dA/dt at which it sweeps out area A is constant.
Conservation of Angular Momentum:
dA r v dt
dAm
r mv dt
dAm
L dt
12
12
12
dAdt m
L
L
12
constant
constant
Any Central Force
jw Fundamentals of Physics 26
Kepler’s 3rd Law
The Law of Periods: The square of the period of any planet is proportional to the cube of the semimajor axis of its orbit.
Consider the special case of a circular orbit:
See Table 13-3.
r
MGv
r
mMG
r
vmF
2
2
2
v
rT
2 :Period 3
22 4
rMG
T
32 ~ rT
Determine the mass of a planet by measuring period and mean orbital distance of a moon orbiting it.
jw Fundamentals of Physics 27
What did Newton know?
Kepler’s 3rd Law:32 ~ rT
acceleration of the moon: r
va
2
velocity of the moon:T
rv
2
His own law! amF
A little algebra by Newton:2
1~
rF
The force holding the moon in orbit depends on the square of its distance from earth.
jw Fundamentals of Physics 28
Einstein & Gravitation
“Science is a perfectionist” - Narlikar
– Newton’s Law of Gravity works great!
– But, how & why does it work?
– A small problem with the planet Mercury.
jw Fundamentals of Physics 29
Einstein & Gravitation
A “Small” problem with the planet Mercury:
• Mercury takes 88 Earth days to orbit the sun.
• But, measurements show the perihelion “advancing”:
– 0.159o per 100 years! (Newton’s Law says zero!)
• Attractions by the other planets almost explain it.
– 0.147o per 100 years!
• 43 arc-seconds per 100 years unexplained.
Einstein explains it!
jw Fundamentals of Physics 30
Einstein & Gravitation
• Special Theory of Relativity
– Space & Time are intimately connected.
c = constant everywhere
– Mass & Energy are equivalent.
E = m c2
• General Theory of Relativity
– A theory of gravitation
space–time geometry mass (material bodies)
jw Fundamentals of Physics 31
Einstein & Gravitation
• Galileo / Newton Universe
– No interdependence of time, space & mass.
• Time flows uniformly.
• Space is immutable.
– Euclidean geometry - “straight lines”
• Mass of a body is constant.
(shape & dimension of rigid bodies is also constant)
• Einstein Universe
• Gravitational forces reach out to infinity.
– All bodies are moving in the gravitational field of other bodies.
Not moving in a straight line.
• Space is curved!
jw Fundamentals of Physics 32
Einstein & Gravitation
The General Theory of Relativity:
The Equivalence Principle:
Is it gravity or rockets that causes a?
No experiment can tell the difference!
Einstein’s Strong Equivalence Principle:
jw Fundamentals of Physics 33
If light appears to follow a curved path in the elevator, gravity must also cause it to curve.
Gravity & Light:
Einstein’s Strong Equivalence Principle:
Observe light in an accelerating elevator:
Einstein: Light does not travel in a straight line!
jw Fundamentals of Physics 34
In his General Theory of Relativity, Einstein explained the force of attraction between massive objects in this way:
“Mass tells space-time how to curve, and the curvature of space-time tells masses how to accelerate.”
Einstein’s View of Gravitation
“space-time” refers to 4-dimensional space: x, y, z, ct
Einstein: Space-Time is curved by the presence of mass!
jw Fundamentals of Physics 35
Bending of Space Time
• Newton said the forces due to the mass of the Earth and the mass of the Moon kept the Moon in orbit.
• Einstein said the Moon was trapped in the funnel of the Earths gravity well.
– A gravity well is formed when a mass bends the fabric of space-time.
• General Theory of Relativity
– Orbit is not caused by forces but by the curvature of space-time (funnel curve)
jw Fundamentals of Physics 36
Einstein & Gravitation
Einstein: Space-Time is curved by the presence of mass!
jw Fundamentals of Physics 37
Einstein proposed a radical experiment to test his theory:
1919: Einstein’s prediction verified by Eddington during a solar eclipse by the moon.
1915
Einstein becomes the most famous scientist of the 20th century!
jw Fundamentals of Physics 39
Gravitational Lensing
These usually involve light paths from quasars & galaxies being bent by intervening galaxies & clusters.
a galaxy behind a galaxy
“Einstein Ring” “Einstein Cross”
multiple images