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Transcript of Walker3 Lecture Ch12
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2007 Pearson Prentice Hall
This work is protected by United States copyright laws and is provided solely for
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Lecture Outlines
Chapter 12
Phys ics, 3rdEdit ion
James S. Walker
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Chapter 12
Gravity
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Units of Chapter 12
Newtons Law of Universal Gravitation Gravitational Attraction of Spherical
Bodies
Keplers Laws of Orbital Motion
Gravitational Potential Energy
Energy Conservation
Tides
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12-1 Newtons Law of Universal Gravitation
Newtons insight:
The force accelerating an apple downward is
the same force that keeps the Moon in its orbit.
Hence, Universal Gravitation.
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12-1 Newtons Law of Universal Gravitation
The gravitational force is always attractive, and
points along the line connecting the two
masses:
The two forces shown are an action-reaction
pair.
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12-1 Newtons Law of Universal Gravitation
Gis a very small number; this means that theforce of gravity is negligible unless there is a
very large mass involved (such as the Earth).
If an object is being acted upon by several
different gravitational forces, the net force on it
is the vector sum of the individual forces.
This is called the principle of superposition.
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12-2 Gravitational Attraction of Spherical
Bodies
Gravitational force between a point mass and a
sphere: the force is the same as if all the mass
of the sphere were concentrated at its center.
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12-2 Gravitational Attraction of Spherical
Bodies
What about the gravitational force on objects atthe surface of the Earth? The center of the Earth is
one Earth radius away, so this is the distance we
use:
Therefore,
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12-2 Gravitational Attraction of Spherical
Bodies
The acceleration of gravity decreases slowly withaltitude:
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12-2 Gravitational Attraction of Spherical
Bodies
Once the altitude becomes comparable to the
radius of the Earth, the decrease in the
acceleration of gravity is much larger:
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12-2 Gravitational Attraction of Spherical
Bodies
The Cavendish experiment allows us to measurethe universal gravitation constant:
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12-2 Gravitational Attraction of Spherical
Bodies
Even though the gravitational force is very small,the mirror allows measurement of tiny deflections.
Measuring G also allowed the mass of the Earth tobe calculated, as the local acceleration of gravity
and the radius of the Earth were known.
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12-3 Keplers Laws of Orbital Motion
Johannes Kepler made detailed studies of the
apparent motions of the planets over many years,and was able to formulate three empirical laws:
1. Planets follow elliptical orbits, with the Sun at
one focus of the ellipse.
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12-3 Keplers Laws of Orbital Motion
2. As a planet moves in its orbit, it sweeps out an
equal amount of area in an equal amount of time.
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12-3 Keplers Laws of Orbital Motion
3. The period,T
, of a planet increases as itsmean distance from the Sun, r, raised to the 3/2
power.
This can be shown to be a consequence of the
inverse square form of the gravitational force.
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12-3 Keplers Laws of Orbital Motion
A geosynchronous satellite is one whose orbital
period is equal to one day. If such a satellite is
orbiting above the equator, it will be in a fixed
position with respect to the ground.
These satellites are used for communications and
and weather forecasting.
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12-3 Keplers Laws of Orbital Motion
GPS satellites are not in geosynchronous orbits;
their orbit period is 12 hours. Triangulation of
signals from several satellites allows preciselocation of objects on Earth.
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12-3 Keplers Laws of Orbital Motion
Keplers laws also give us an insight into
possible orbital maneuvers.
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12-4 Gravitational Potential Energy
Gravitational potential energy of an object of
mass m a distance rfrom the Earths center:
12 4 G
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12-4 Gravitational Potential Energy
Very close to the Earths surface, the
gravitational potential increases linearly withaltitude:
Gravitational potential energy, just like all
other forms of energy, is a scalar. Ittherefore has no components; just a sign.
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12-5 Energy Conservation
Total mechanical energy of an object of mass m
a distance r from the center of the Earth:
This confirms what we already know as an
object approaches the Earth, it moves fasterand faster.
12 5 E C ti
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12-5 Energy Conservation
12 5 E C ti
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12-5 Energy Conservation
Another way of visualizing the gravitational
potential well:
12 5 E C ti
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12-5 Energy Conservation
Escape speed: the initial upward speed a
projectile must have in order to escape
from the Earths gravity
12 5 E C ti
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12-5 Energy Conservation
Speed of a projectile as it leaves the Earth,
for various launch speeds
12 5 E C ti
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12-5 Energy Conservation
Black holes:
If an object is sufficiently massive and
sufficiently small, the escape speed will
equal or exceed the speed of light
light itself will not be able to escape the
surface.
This is a black hole.
12 5 E C ti
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12-5 Energy Conservation
Light will be bent by any
gravitational field; this canbe seen when we view a
distant galaxy beyond a
closer galaxy cluster. This is
called gravitational lensing,and many examples have
been found.
12 6 Tid
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12-6 Tides
Usually we can treat planets, moons, and stars
as though they were point objects, but in factthey are not.
When two large objects exert gravitational
forces on each other, the force on the near sideis larger than the force on the far side, because
the near side is closer to the other object.
This difference in gravitational force across an
object due to its size is called a tidal force.
12 6 Tides
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12-6 Tides
This figure illustrates a general tidal force on
the left, and the result of lunar tidal forces on
the Earth on the right.
12 6 Tides
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12-6 Tides
Tidal forces can result in orbital locking,
where the moon always has the same facetowards the planetas does Earths Moon.
If a moon gets too close to a large planet, the
tidal forces can be strong enough to tear the
moon apart. This occurs inside the Roche
limit; closer to the planet we have rings, notmoons.
Summary of Chapter 12
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Summary of Chapter 12
Force of gravity between two point masses:
G is the universal gravitational constant:
In calculating gravitational forces,spherically symmetric bodies can be replaced
by point masses.
Summary of Chapter 12
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Summary of Chapter 12
Acceleration of gravity:
Mass of the Earth:
Keplers laws:1. Planetary orbits are ellipses, Sun at one
focus
2. Planets sweep out equal area in equal time
3. Square of orbital period is proportional to
cube of distance from Sun
Summary of Chapter 12
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Summary of Chapter 12
Orbital period:
Gravitational potential energy:
U is a scalar, and goes to zero as the
masses become infinitely far apart
Summary of Chapter 12
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Summary of Chapter 12
Total mechanical energy:
Escape speed:
Tidal forces are due to the variations ingravitational force across an extended body