Transcript Newton`s Law of Universal Gravitation

Newton’s Law of Universal Gravitation
Kepler’s Three Laws of
Planetary Motion
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Tycho Brahe (1546-1601) – Danish
astronomer who dedicated much of his life
to accurately collecting astronomical data
Built the finest observatory at the time on
the island of Hven and charted the
movements of the planets and stars for 20
years
Kepler’s Three Laws of
Planetary Motion
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In 1597 Johannes Kepler(1571-1630)
became an assistant of Brahe in Prague
Kepler attempted to use Geometry and
Mathematics to describe a heliocentric
(sun-centered) system that would agree
with Brahe’s Data
Result: Kepler’s Three Laws of
Planetary Motion
Kepler’s Three Laws of
Planetary Motion
1.
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The path of the planets around the sun
are ellipses with the sun at one of the
focus points
Consequence: The planets traveling in
their orbits are sometimes closer to the
sun and other times further away
Note: The orbits are only slightly
elliptical. They are close to circular.
Kepler’s Three Laws of
Planetary Motion
2.
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The planets sweep out equal areas in
equal time intervals no matter how close
or far away a planet is from the sun
Consequence: Planets speed up as they
move closer to the sun and slow down as
they move further away
Kepler’s Three Laws of
Planetary Motion
3. The ratio of the squares of the Periods of
any two planets going around the sun is
equal to the ratio of the cubes of their
Average Distances away from the sun.
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Consequence: Planets that are farther
away from the sun have a longer Period
of Revolution
Equation for Kepler’s Third Law
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Kepler’s 3rd Law can be written in an
equation form.
(Ta)2
(Tb)2
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=
(Ra)3
(Rb)3
Kepler’s 3rd law applies to any two
objects going around a third central
object!
(2 planets around the
sun or 2 moons around a planet)
Astronomical Units (A.U.)
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The average distance between the Earth
and the Sun is dE-S = 1.5 x 1011 m
To avoid using large numbers and
exponents in calculations scientists have
developed the Astronomical Unit (A.U.)
1 A.U. = 1.5 x 1011 m
 dE-S = 1A.U.
History of Universal Gravitation
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Greeks (Aristotle and Ptolemy) –
Geocentric Model
Copernicus – Heliocentric Model
Galileo – Discoveries with his telescope
Kepler – Three Laws of Planetary Motion
History of Universal Gravitation
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After Galileo and Kepler, the
heliocentric model gained acceptance
but scientists still did not know what
causes the motion of the planets!
The stage was set in 1666 for Issac
Newton to use his concept of a force
and his Three Laws of Motion to
explain the force behind planetary
motion
Universal Gravitation
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Newton named this force Gravity
He suggested Gravity is a force of
attraction between any two masses and
that each mass pulls on the other with an
equal and opposite force
Universal Gravitation
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The Force of Gravity is directly
proportional to the mass of each object
Fam
The Force of Gravity is inversely
proportional to the square of the
distance between the center of the
masses
F a 1/d2 (Inverse Square Law)
Gravitation
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Every object with mass attracts every
other object with mass.
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Newton realized that the force of attraction
between two massive objects:
Increases as the mass of the objects increases.
 Decreases as the distance between the objects
increases.
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Law of Universal Gravitation
M1M2
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FG = G
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G = Gravitational Constant
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r2
G = 6.67x10-11 N*m2/kg2
M1 and M2 = the mass of two bodies
r = the distance between them
Law of Universal Gravitation
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The LoUG is an inverse-square law:
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If the distance doubles, the force drops to 1/4.
If the distance triples, the force drops to 1/9.
Distance x 10 = FG / 100.
Law of Universal Gravitation
Gravitational Force (N)
M1 and M2 = 10 kg
8E-11
7E-11
6E-11
5E-11
4E-11
3E-11
2E-11
1E-11
0
0
20
40
60
Distance (m)
80
100
Law of Universal Gravitation
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Jimmy is attracted to Betty. Jimmy’s mass is 90.0 kg and
Betty’s mass is 57.0 kg. If Jim is standing 10.0 meters away
from Betty, what is the gravitational force between them?
 FG = GM1M2 / r2
 FG = (6.67x10-11 Nm2/kg2)(90.0 kg)(57.0 kg) / (10.0 m)2
 FG = (3.42x10-7 Nm2) / (100. m2)
 FG = 3.42x10-9 N = 3.42 nN
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In standard terms, that’s 7.6 ten-billionths of a pound of force.
Law of Universal Gravitation
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The Moon is attracted to the Earth. The
mass of the Earth is 6.0x1024 kg and the
mass of the Moon is 7.4x1022 kg. If the
Earth and Moon are 345,000 km apart,
what is the gravitational force between
them?
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FG = GM1M2 / r2
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FG = (6.67x10-11 Nm2/kg2)
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FG = 2.49x1020 N
(6.0x1024 kg)(7.4x1022 kg)
(3.45x108 m)2
Gravitational Field
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Gravitational field – an area of influence
surrounding a massive body.
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g = GM / r2
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Field strength = acceleration due to gravity (g).
Notice that field strength does not depend on
the mass of a second object.
GM1M2/r2 = M2g = FG = Fw
So gravity causes mass to have weight.
Gravitational Field Strength
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The mass of the Earth is 6.0x1024 kg and its radius is 6378
km. What is the gravitational field strength at Earth’s
surface?
 g = GM/r2
 g = (6.67x10-11 Nm2/kg2)(6.0x1024 kg) / (6.378x106 m)2
 g = 9.8 m/s2
A planet has a radius of 3500 km and a surface gravity of
3.8 m/s2. What is the mass of the planet?
 (3.8 m/s2) = (6.67x10-11 Nm2/kg2)(M) / (3.5x106 m)2
 (3.8 m/s2) = (6.67x10-11 Nm2/kg2)(M) / (1.2x1013 m2)
 (4.6x1013 m3/s2) = (6.67x10-11 Nm2/kg2)(M)
 M = 6.9x1023 kg
Variations in Gravitational Field Strength
Things Newton Didn’t Know
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Newton didn’t know what caused gravity,
although he knew that all objects with
mass have gravity and respond to gravity.
To Newton, gravity was simply a property
of objects with mass.
Newton also couldn’t explain how gravity
was able to span between objects that
weren’t touching.
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He didn’t like the idea of “action-at-adistance”.
Discovery of Neptune
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Newton’s Law of Universal Gravitation did a very
good job of predicting the orbits of planets.
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In fact, the LoUG was used to predict the existence of
Neptune.
The planet Uranus was not moving as expected.
The gravity of the known planets wasn’t sufficient to
explain the disturbance.
Urbain LeVerrier (and others) predicted the existence
of an eighth planet and worked out the details of its
orbit.
Neptune was discovered on September 23, 1846 by
Johann Gottfried Galle, only 1º away from where
LeVerrier predicted it would be.
Precession of Perihelion
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Newton’s Law has some flaws, however:
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It does not predict the precession of Mercury’s
perihelion, nor does it explain it.
All planets orbit the Sun in slightly elliptical orbits.
 Mercury has the most elliptical orbit of any planet
in the solar system (if you don’t count Pluto).
 The closest point in Mercury’s orbit to the Sun is
called the perihelion.
 Over long periods of time, Mercury’s perihelion
precedes around the Sun.
 This effect is not explainable using only Newtonian
mechanics.
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Precession of Mercury’s Perihelion
The eccentricity of
Mercury’s orbit has been
exaggerated for effect
in this diagram.
Other Things Newton Didn’t Know
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Newton didn’t know that gravity bends
light.
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This was verified by the solar eclipse
experiment you read about earlier this year.
He also didn’t know that gravity slows
down time.
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Clocks near the surface of Earth run slightly
slower than clocks higher up.
This effect must be accounted for by GPS
satellites, which rely on accurate time
measurements to calculate your position.
Einstein and Relativity
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Einstein’s theory of relativity explains
many of the things that Newtonian
mechanics cannot explain.
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According to Einstein, massive bodies cause a
curvature in space-time.
Objects moving through this curvature
move in locally straight paths through
curved space-time.
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To any observer inside this curved space-time,
the object’s motion would appear to be
curved by gravity.
Curvature of Space-Time
Curvature of Space-Time
Gravity: Not So Simple Anymore
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According to Einstein, gravity isn’t technically a
force.
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It’s an effect caused by the curvature of space-time
by massive bodies.
Why treat it as a force if it isn’t one?
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Because in normal situations, Newton’s LoUG provides
an excellent approximation of the behavior of massive
bodies.
And besides, using the LoUG is a lot simpler than
using the theory of relativity, and provides results that
are almost as good in most cases.
So there.