Relative Motion Parallax: Why the Formula Holds
Relative motion parallax is a powerful depth cue: nearby objects appear to move faster across your field of view than distant ones when you (or your viewpoint) move sideways. Let's build the formula from first principles.
1. The Physical Setup
Imagine you are moving with velocity v perpendicular to your line of sight. You fix your gaze on a distant reference point (say, a mountain far away). Now consider an object at distance d from you.
- Key idea: As you move, the direction to the object changes. This angular shift per unit time is the parallax rate.
2. Deriving the Angular Speed
Let the object be at perpendicular distance d from your path. When you move a small distance Δx sideways, the object's angular position θ (measured from your forward direction) changes.
From simple geometry:
tanθ=dx
where x is your lateral displacement from the point of closest approach.
Differentiate with respect to time:
sec2θ⋅dtdθ=d1⋅dtdx
Since dtdx=v (your speed) and sec2θ=1+tan2θ=1+(dx)2, we get:
dtdθ=dv⋅1+(x/d)21
3. The Key Formula (for small angles)
When the object is nearly straight ahead (x≈0), the formula simplifies dramatically:
dtdθ=dv
This is the core result: the angular speed of a stationary object due to your motion is inversely proportional to its distance.
4. Why This Makes Intuitive Sense
- Near objects (d small): dv is large → rapid angular motion.
- Far objects (d large): dv is small → almost no apparent motion.
This is exactly what you see from a moving car: telegraph poles whiz by, but mountains barely move.
5. The Parallax Shift Over a Finite Displacement
If you move a total distance L sideways, the total angular shift (parallax angle) is:
Δθ=dL(for small angles, in radians)
This is the parallax formula used in astronomy (where L is the Earth's orbital diameter and d is the star's distance).
6. Why the Formula Holds — The Core Reasoning
| Step | What happens | Why it matters |
|------|--------------|----------------| …