Trajectory

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For other uses, see Trajectory (disambiguation).

Mathematically the term trajectory refers to the ordered set of states which are assumed by a dynamical system over time (see e.g. Poincaré map).

Colloquially, a trajectory is the path in space followed by a body. Such a body can be a projectile, for example. Strictly speaking trajectory refers only to that portion of the path during which the body undergoes a transient movement between practically stationary or repetitive motions or until the body eventually stops moving. In a wider sense it also includes the meaning of orbit - the path of a planet, an asteroid or comet, for example. A trajectory can be described mathematically by the geometry of the path or as the position of the object over time.

A familiar example is the path of a thrown object such as a ball or a rock. In a greatly simplified model the object moves only under the influence of a uniform homogenous gravitational force field. This can be a good approximation for a rock that is thrown for short distances for example, at the surface of the moon. In this simple approximation the trajectory takes the shape of a parabola. Generally, when determining trajectories it may be necessary to account for nonuniform gravitational forces, air resistance (drag and aerodynamics). This is the focus of the discipline of ballistics.

In discrete mathematics, the term trajectory denotes the sequence (f^k(x))_{k \in \mathbb{N}} of values which one gets by iterated application of a mapping f to an element x of its source.

The word trajectory is also often used metaphorically, for instance, to describe an individual's career.

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[edit] Physics of trajectories

One of the remarkable achievements of Newtonian mechanics was the derivation of the laws of Kepler, in the case of the gravitational field of a single point mass (representing the Sun). The trajectory is a conic section, like an ellipse or a parabola. This agrees with the observed orbits of planets and comets, to a reasonably good approximation. Although if a comet passes close to the Sun, then it is also influenced by other forces, such as the solar wind and radiation pressure, which modify the orbit, and cause the comet to eject material into space.

Newton's theory later developed into the branch of theoretical physics known as classical mechanics. It employs the mathematics of differential calculus (which was, in fact, also initiated by Newton, in his youth). Over the centuries, countless scientists contributed to the development of these two disciplines. Classical mechanics became a most prominent demonstration of the power of rational thought, i.e. reason, in science as well as technology. It helps to understand and predict an enormous range of phenomena. Trajectories are but one example.

Consider a particle of mass m, moving in a potential field V. Physically speaking, mass represents inertia, and the field V represents external forces, of a particular kind known as "conservative". That is, given V at every relevant position, there is a way to infer the associated force that would act at that position, say from gravity. Not all forces can be expressed in this way, however.

The motion of the particle is described by the second-order differential equation

m \frac{d^2 \vec{x}(t)}{dt^2} = -\nabla V(\vec{x}(t)) with \vec{x} = (x, y, z)

On the right-hand side, the force is given in terms of \nabla V, the gradient of the potential, taken at positions along the trajectory. This is the mathematical form of Newton's second law of motion: mass times acceleration equals force, for such situations.

[edit] Examples

[edit] Uniform gravity, no drag or wind

The case of uniform gravity, disregarding drag and wind, yields a trajectory which is a parabola. To model this, one chooses V = mgz, where g is the acceleration of gravity. This gives the equations of motion

\frac{d^2 x}{dt^2} = \frac{d^2 y}{dt^2} = 0
\frac{d^2 z}{dt^2} = - g

Simplifications are made for the sake of studying the basics. The actual situation, at least on the surface of Earth, is considerably more complicated than this example would suggest, when it comes to computing actual trajectories. By deliberately introducing such simplifications, into the study of the given situation, one does, in fact, approach the problem in a way that has proved exceedingly useful in physics.

The present example is one of those originally investigated by Galileo Galilei. To neglect the action of the atmosphere, in shaping a trajectory, would (at best) have been considered a futile hypothesis by practical minded investigators, all through the Middle Ages in Europe. Nevertheless, by anticipating the existence of the vacuum, later to be demonstrated on Earth by his collaborator Evangelista Torricelli, Galileo was able to initiate the future science of mechanics. And in a near vacuum, as it turns out for instance on the Moon, his simplified parabolic trajectory proves essentially correct.

Relative to a flat terrain, let the initial horizontal speed be vh, and the initial vertical speed be vv. It will be shown that, the range is 2vhvv / g, and the maximum altitude is {v_v^2}/2g. The maximum range, for a given total initial speed v, is obtained when vh = vv, i.e. the initial angle is 45 degrees. This range is 2v2 / g, and the maximum altitude at the maximum range is a quarter of that.

[edit] Derivation

The equations of motion may be used to calculate the characteristics of the trajectory.

Let

p(t)\; be the position of the projectile, expressed as a vector
t\; be the time into the flight of the projectile,
v_h \; be initial the horizontal velocity (which is constant)
v_v \; be the initial vertical velocity upwards.

The path of the projectile is known to be a parabola so

p(t) = ( A t, 0 , a t^2 + b t + c )\,

where A,\,a,\,b,\,c are parameters to be found. The first and second derivatives of p are:

p'(t) = ( A , 0 , 2 a t + b ),\quad p''(t) = ( 0 , 0 , 2 a ).

At t = 0

p(0)=0,\ p'(0)=(v_h,0,v_v),\ p''(0)=(0,0,-g)

so A = v_h,\ a = -g/2,\ b = v_v,\ c = 0. Giving eqn of parabola as

p(t) = (v_h t,0,v_v t - g t^2/2)\,\qquad(Equation I: trajectory of parabola).

[edit] Range and height

The range R of the projectile is found when the z-component of p is zero, that is when

0 = v_v t - g t^2/2 = t \left( v_v - g t/2\right)\,

which has solutions at t = 0 and t = 2vv / g (the hang-time of the projectile). The range is then R = 2 v_h v_v/g.\,

From the symmetry of the parabola the maximum height occurs at the halfway point t = vv / g at position

p(v_v/g)=(v_h v_v/g,0,v_v^2/(2g))\,

This can also be derived by finding when the z-component of p' is zero.

[edit] Angle of elevation

In terms of angle of elevation θ and initial speed v:

v_h=v \cos \theta,\quad v_v=v \sin \theta \;

giving the range as

R= 2 v^2 \cos(\theta) \sin(\theta) / g = v^2 \sin(2\theta) / g\,.

This equation can be rearranged to find the angle for a required range

{ \theta } = \frac 1 2 \sin^{-1} \left( { {g R} \over { v^2 } } \right) (Equation II: angle of projectile launch)

Note that the sine function is such that there are two solutions for θ for a given range dh. Physically, this corresponds to a direct shot versus a mortar shot up and over obstacles to the target.

The angle θ giving the maximum range can be found by considering the derivative or R with respect to θ and setting it to zero.

{dR\over d\theta}={2v^2\over g} cos(2\theta)=0

which has a non trivial solutions at \theta=\pi/2=45^\circ. The maximum range is then R_{max} = v^2/g\,. At this angle sin(\pi/2)=1/\sqrt{2} so the maximum height obtained is {v^2 \over 4g}.

To find the angle giving the maximum height for a given speed calculate the derivative of the maximum height H = vsin(θ) / (2g) with respect to θ, that is {dH\over d\theta}=v cos(\theta) /(2g) which is zero when \theta=\pi=90^\circ. So the maximum height H_{max}={v\over 2g} is obtain when the projectile is fired straight up.

[edit] Uphill/downhill in uniform gravity in a vacuum

The factual accuracy of this section is disputed.
Please see the relevant discussion on the talk page

Given a hill angle α and launch angle θ as before, it can be shown that the range along the hill Rs forms a ratio with the original range R along the imaginary horizontal, such that:

\frac{R_s} {R}=(1-\cot \theta \tan \alpha)\sec \alpha (Equation 11)

In this equation, downhill occurs when α is between 0 and -90 degrees. For this range of α we know: tan( − α) = − tanα and sec( − α) = secα. Thus for this range of α, Rs / R = (1 + tanθtanα)secα. Thus Rs / R is a positive value meaning the range downhill is always further than along level terrain. This makes perfect sense as it is expected that gravity will assist the projectile, giving it greater range.

While the same equation applies to projectiles fired uphill, the interpretation is more complex as sometimes the uphill range may be shorter or longer than the equivalent range along level terrain. Equation 11 may be set to Rs / R = 1 (i.e. the slant range is equal to the level terrain range) and solving for the "critical angle" θcr:

1=(1-\tan \theta \tan \alpha)\sec \alpha \quad \;
\theta_{cr}=\arctan((1-\csc \alpha)\cot \alpha) \quad \;

Equation 11 may also be used to develop the "rifleman's rule" for small values of α and θ (i.e. close to horizontal firing, which is the case for many firearm situations). For small values, both tanα and tanθ have a small value and thus when multiplied together (as in equation 11), the result is almost zero. Thus equation 11 may be approximated as:

\frac{R_s} {R}=(1-0)\sec \alpha

And solving for level terrain range, R

R=R_s \cos \alpha \ "Rifleman's rule"

Thus if the shooter attempts to hit the level distance R, s/he will actually hit the slant target. "In other words, pretend that the inclined target is at a horizontal distance equal to the slant range distance multiplied by the cosine of the inclination angle, and aim as if the target were really at that horizontal position."[1]

[edit] Derivation based on equations of a parabola

The intersect of the projectile trajectory with a hill may most easily be derived using the trajectory in parabolic form in Cartesian coordinates (Equation 10) intersecting the hill of slope m in standard linear form at coordinates (x,y):

y=mx+b \; (Equation 12) where in this case, y = dv, x = dh and b = 0

Substituting the value of dv = mdh into Equation 10:

m x=-\frac{g}{2v^2{\cos}^2 \theta}x^2 + \frac{\sin \theta}{\cos \theta} x
x=\frac{2v^2\cos^2\theta}{g}\left(\frac{\sin \theta}{\cos \theta}-m\right) (Solving above x)

This value of x may be substituted back into the linear equation 12 to get the corresponding y coordinate at the intercept:

y=mx=m \frac{2v^2\cos^2\theta}{g} \left(\frac{\sin \theta}{\cos \theta}-m\right)

Now the slant range Rs is the distance of the intercept from the origin, which is just the hypotenuse of x and y:

R_s=\sqrt{x^2+y^2}=\sqrt{\left(\frac{2v^2\cos^2\theta}{g}\left(\frac{\sin \theta}{\cos \theta}-m\right)\right)^2+\left(m \frac{2v^2\cos^2\theta}{g} \left(\frac{\sin \theta}{\cos \theta}-m\right)\right)^2}
=\frac{2v^2\cos^2\theta}{g} \sqrt{\left(\frac{\sin \theta}{\cos \theta}-m\right)^2+m^2 \left(\frac{\sin \theta}{\cos \theta}-m\right)^2}
=\frac{2v^2\cos^2\theta}{g} \left(\frac{\sin \theta}{\cos \theta}-m\right) \sqrt{1+m^2}

Now α is defined as the angle of the hill, so by definition of tangent, m = tanα. This can be substituted into the equation for Rs:

R_s=\frac{2v^2\cos^2\theta}{g} \left(\frac{\sin \theta}{\cos \theta}-\tan \alpha\right) \sqrt{1+\tan^2 \alpha}

Now this can be refactored and the trigonometric identity for \sec \alpha = \sqrt {1 + \tan^2 \alpha} may be used:

R_s=\frac{2v^2\cos\theta\sin\theta}{g}\left(1-\frac{\sin\theta}{\cos\theta}\tan\alpha\right)\sec\alpha

Now the flat range R = v2sin2θ / g = 2v2sinθcosθ / g by the previously used trigonometric identity and sinθ / cosθ = tanθ so:

R_s=R(1-\tan\theta\tan\alpha)\sec\alpha \;
\frac{R_s}{R}=(1-\tan\theta\tan\alpha)\sec\alpha

[edit] Orbiting objects

If instead of a uniform downwards gravitational force we consider two bodies orbiting with the mutual gravitation between them, we obtain Kepler's laws of planetary motion. The derivation of these was one of the major works of Newton and provided much of the motivation for the development of differential calculus.

[edit] See also

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[edit] External Links

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