Copyright © 2012 Pearson Education Inc. Orbital motion, final review Physics 7C lecture 18 Thursday...

Copyright © 2012 Pearson Education Inc.

Orbital motion, final review

Physics 7C lecture 18

Thursday December 5, 8:00 AM – 9:20 AMEngineering Hall 1200


Newton’s law of gravitation

• The gravitational force can be

expressed mathematically as

• Fg = Gm1m2/r2,

• where G is the gravitational

constant. Note G is different from

g.

• G = 6.67 E -11 N m2/kg2


Gravitation and spherically symmetric bodies

• The gravitational interaction of bodies having spherically symmetric mass distributions is the same as if all their mass were concentrated at their centers.

• This is exact, not approximation! Let’s prove it mathematically.


Gravitational potential energy

• The gravitational potential energy of a system consisting of a particle of mass m and the earth is U = –GmEm/r.

• This assumes zero energy at infinite distance.


The motion of satellites

• The trajectory of a projectile fired from A toward B depends on its initial speed. If it is fired fast enough, it goes into a closed elliptical orbit (trajectories 3, 4, and 5 in Figure 13.14 below).


Circular satellite orbits • For a circular orbit, the speed of a satellite is just right to keep its distance

from the center of the earth constant. (See Figure 13.15 below.)

• A satellite is constantly falling around the earth. Astronauts inside the satellite in orbit are in a state of apparent weightlessness because they are falling with the satellite. (See Figure 13.16 below.)

• Follow Example 13.6.


Kepler’s laws and planetary motion

• Each planet moves in an elliptical orbit with the sun at one focus.



• A line from the sun to a given planet sweeps out equal areas in equal times (see Figure at the right).



• The periods of the planets are proportional to the 3/2 powers of the major axis lengths of their orbits.


Some orbital examples• The orbit of Comet Halley. See Figure below.


A point mass inside a spherical shell

• If a point mass is inside a spherically symmetric shell, the potential energy of the system is constant. This means that the shell exerts no force on a point mass inside of it.

what is the motion of the small ball?


A point mass inside a spherical shell


Black holes • If a spherical nonrotating body has radius less than the Schwarzschild radius,

nothing can escape from it. Such a body is a black hole. (See Figure 13.26 below.)

• The Schwarzschild radius is RS = 2GM/c2.

• The event horizon is the surface of the sphere of radius RS surrounding a black hole.

• Follow Example 13.11.


Detecting black holes

• We can detect black holes by looking for x rays emitted from their accretion disks. (See Figure below.)


Review for final exam

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Copyright © 2012 Pearson Education Inc. Orbital motion, final review Physics 7C lecture 18 Thursday...

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