1. Kinetics of Particles:
CHAPTER 12
Kinetics of Particles:
Newton’s Second Law

2. 12.1 INTRODUCTION
Reading Assignment

3. 12.2 NEWTON’S SECOND LAW OF MOTION
If the resultant force acting on a particle is not zero, the particle will have an acceleration proportional to the magnitude of the resultant and in the direction of this resultant force.
More accurately
Cause
= Effect

4. or Newtonian frame of reference –
Inertial frame
or Newtonian frame of reference –
one in which Newton’s second law equation holds. Wikipedia definition.

5. Free Body Diagrams (FBD)
This is a diagram showing some object and the forces applied to it.
It contains only forces and coordinate information, nothing else.
There are only two kinds of forces to be considered in mechanics:
Force of gravity
Contact forces

6. A car of mass m rests on a 300 incline.
Example FBD
A car of mass m rests on a 300 incline.
FBD N F x y
This completes the FBD. q q mg

7. A car of mass m rests on a 300 incline.
Example FBD
A car of mass m rests on a 300 incline.
FBD x y
Just for grins, let’s do
a vector addition. N F q q mg

8. Newton’s Second Law NSL
A car of mass m rests on a 300 incline.
FBD
NSL y N x F q q mg
What if friction is smaller?

9. Newton’s Second Law NSL
A car of mass m rests on a 300 incline.
NSL x y N F q q
oops mg

10. 12.3 LINEAR MOMENTUM OF A PARTICLE. RATE OF CHANGE OF LINEAR MOMENTUM

11. Linear Momentum Conservation Principle: If the resultant force on a particle is zero, the linear momentum of the particle remains constant in both magnitude and direction.

12. 12.4 SYSTEMS OF UNITS
Reading Assignment

13. 12.5 EQUATIONS OF MOTION
Rectangular Components or

14. x z y O
For Projectile Motion
In the x-y plane

15. Tangential and Normal Componentsx z y O m
And as a reminder

16. Take Newton’s second law,
12.6 DYNAMIC EQUILIBRIUM
Take Newton’s second law,
This has the appearance of being in static equilibrium and is actually referred to as dynamic equilibrium.
Don’t ever use this method in my course … H. Downing

17. 12. 7 ANGULAR MOMENTUM OF A PARTICLE
12.7 ANGULAR MOMENTUM OF A PARTICLE. RATE OF CHANGE OF ANGULAR MOMENTUM x z y O

18. Angular Momentum of a Particle
moment of momentum or the angular momentum of the particle about O. It is perpendicular to the plane containing the position vector and the velocity vector.

20. For motion in x-y plane y
In Polar Coordinates x O

21. Derivative of angular momentum with respect to time,

22. 12.8 EQUATIONS OF MOTION IN TERMS OF RADIAL AND TRANSVERSE COMPONENTS
Consider particle at r and q, in polar coordinates, y
This latter result may also be
derived from angular momentum. x O

23. This latter result may also be derived from angular momentum.x O

24. 12.9 MOTION UNDER A CENTRAL FORCE. CONSERVATION OF ANGULAR MOMENTUM
When the only force acting on particle is directed toward or away from a fixed point O, the particle is said to be moving under a central force.
Since the line of action of the central force passes through O, x O y m
Position vector and motion of particle are in a plane perpendicular to

25. Position vector and motion of particle are in a plane perpendicular to
Since the angular momentum is constant, its magnitude can be written as x y O m
Remember

26. Conservation of Angular Momentum
Radius vector OP sweeps infinitesimal area x y O
Areal velocity
Recall, for a body moving under a central force,
When a particle moves under a central force, its areal velocity is constant.

27. 12.10 NEWTON’S LAW OF GRAVITATION
Gravitational force exerted by the sun on a planet or by the earth on a satellite is an important example of gravitational force. m
Newton’s law of universal gravitation - two particles of mass M and m attract each other with equal and opposite forces directed along the line connecting the particles, M
For particle of mass m on the earth’s surface,

28. 12.11 TRAJECTORY OF A PARTICLE UNDER A CENTRAL FORCE
For particle moving under central force directed towards force center,
Second expression is equivalent to

29. Remember that
Let
Remember that

30. This can be solved, sometimes.
If F is a known function of r or u, then particle trajectory may be found by integrating for u = f(q ), with constants of integration determined from initial conditions.

31. 12.12 APPLICATION TO SPACE MECHANICS
Consider earth satellites subjected to only gravitational pull of the earth. r q O A

32. There are two solutions: General Solution Particular Solutionq O A
From the figure choose polar axis so that
The above equation for u is a conic section,
that is it is the equation for
ellipses (and circles), parabolas, and hyperbolas.

33. Conic Sections
Circle
Ellipse
Parabola
Hyperbola
Eccentricity

34. Origin, located at earth’s center, is a focus of the conic section.q O A
Trajectory may be ellipse, parabola, or hyperbola depending on value of eccentricity.

35. Hyperbola, e > 1 or C > GM/h2.
The radius vector becomes infinite for q1 r q O A q1

36. The radius vector becomes infinite for
Parabola, e = 1 or C = GM/h2.
The radius vector becomes infinite for q2 r q O A

37. Ellipse, e < 1 or C < GM/h2.
The radius vector is finite for all q, and is constant for a circle, for e = 0. r q O A

38. and
Integration constant C is determined by conditions at beginning of free flight, q =0, r = r0 . O
Burnout A
Powered Flight
Launching

39. Escape Velocity
Remember that
For O
Burnout A
Powered Flight
Launching

40. If the initial velocity is less than the escape velocity, the satellite will move in elliptical orbits.
If e = 0, then r q O A

41. Recall that for a particle moving under a central force, the areal velocity is constant, i.e.,B a
Periodic time or time required for a satellite to complete an orbit is equal to the area within the orbit divided by areal velocity, b A’ O’ C O A
Where r1 r0

42. 12.13 KEPLER’S LAWS OF PLANETARY MOTION
Results obtained for trajectories of satellites around earth may also be applied to trajectories of planets around the sun.
Properties of planetary orbits around the sun were determined by astronomical observations by Johann Kepler ( ) before Newton had developed his fundamental theory.
Each planet describes an ellipse, with the sun located at one of its foci.
The radius vector drawn from the sun to a planet sweeps equal areas in equal times.
The squares of the periodic times of the planets are proportional to the cubes of the semimajor axes of their orbits.