1. Chapter 13 Gravitation
PhysicsI 2048

2. Newton’s law of gravitation
Besides the three laws of motion, Newton also discovered the universal law of gravitation.
The force of gravity between two point object of mass m1 and m2 is attractive and of magnitude
where r is the distance between the masses and
G is a constant referred as the universal gravitation
constant.

3. Newton’s law of gravitation

4. Gravitation G is very small (=6.67x10-11 N·m2kg-2)
The law of gravity applies to all objects small or large.
G is very small (=6.67x10-11 N·m2kg-2)
The force is inverse proportional to distance.
Satisfies superposition.

5. Gravitation and the Principle of Superposition
Where F1,netis the net force on particle 1 due to n particles

6. Gravitation Near Earth's Surface
Newton was able to show that the net force exerted by the sphere on a point mass m is the same as if all the mass of the sphere were concentrated at its center.
For a mass is near the surface of earth:

7. Variation of ag with Altitude

8. Gravitation Near Earth's Surface
Earth's mass is not uniformly distributed.

9. Gravitation Near Earth's Surface
Earth is not a sphere. Earth is approximately an ellipsoid, flattened at the poles and bulging at the equator.
Earth is rotating. The rotation axis runs through the north and south poles of Earth.

10. Gravitation Near Earth's Surface

11. Gravitational Potential Energy

12. Proof of the gravitational potential energy equation
Let us shoot a baseball directly away from Earth along the path in Figure

13. Potential Energy and Force
This is Newton's law of gravitation. The minus sign indicates that the force on mass m points inward, toward mass M

14. Escape Speed
When the projectile reaches infinity, it stops and thus has no kinetic energy. It also has no potential energy because an infinite separation between two bodies is zero potential energy

15. Some Escape Speeds

16. Kepler’s law of orbital motion
Kepler’s three laws
(1) Planets follow elliptical orbits, with the Sun at one focus of the ellipse.

17. Kepler’s law 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.

18. Kepler’s law of orbital motion
(3) The period of a planet increases as its mean distance from the Sun, r raised to the 3/2 power

19. Kepler’s law of orbital motion
Here we will show that the Kepler’s third law can be derived from the definition of centripetal acceleration and the universal gravitation law.

20. Satellites: Orbits and Energy
The potential energy of the system is given by Equation
we write Newton's second law (F = ma) as
Where a is the ellipsis semimajor axis

21. The mean diameters of planets M and E are 6. 9 × 103 km and 1
The mean diameters of planets M and E are 6.9 × 103 km and 1.3 × 104 km, respectively. The ratio of the mass of planet M to that of planet E is (a) What is the ratio of the mean density of M to that of E? (b) What is the ratio of the gravitational acceleration on M to that on E? (c) What is the ratio of escape speed on M to that on E?

22. a- b- C-

23. Two neutron stars are separated by a distance of 1. 0 x 1010 m
Two neutron stars are separated by a distance of 1.0 x 1010 m. They each have a mass of 1.0 x 1030 kg and a radius of 1.0 x 105 m. They are initially at rest with respect to each other. As measured from that rest frame, how fast are they moving when (a) their separation has decreased to one-half its initial value and (b) they are about to collide?

24. (a) Use the principle of conservation of energy
(a) Use the principle of conservation of energy. The initial potential energy is.
The initial kinetic energy is zero since the stars are at rest.
The final potential energy is.

25. (b) Now the final separation of the centers is