3.2.35 · D4Orbital Mechanics & Astrodynamics

Exercises — Solar radiation pressure

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Level 1 — Recognition

Goal: can you pick the right formula and plug in? No traps yet.

Problem 1.1

State, in words and symbols, what momentum a single photon of energy carries, and why a massless particle can carry any momentum at all.

Recall Solution 1.1

WHAT: A photon carries momentum . WHY: Relativity gives . A photon has mass , so the second term vanishes and , i.e. . The old rule is only the low-speed rule; it is not the definition of momentum. Massless light still carries momentum because momentum is fundamentally about energy and direction of flow, not about mass. See Photon momentum and relativity.

Problem 1.2

The Sun's luminosity is . Compute the intensity at 1 AU and confirm it matches the quoted solar constant.

Recall Solution 1.2

WHAT: Spread the power over a sphere of radius . WHY the sphere? Energy is conserved, so all the Sun's power passes through every sphere centred on the Sun (see Inverse-square law). Sphere area is . Denominator: .

Problem 1.3

Compute the base radiation pressure on a black (absorbing) surface at 1 AU.

Recall Solution 1.3

WHAT: Convert energy flux to momentum flux by dividing by . WHY: Each joule of light carries of momentum, so momentum-per-second-per-area (= pressure) is .


Level 2 — Application

Goal: chain two or three steps, handle reflection and geometry.

Problem 2.1

A perfectly reflecting solar sail of area faces the Sun head-on at 1 AU. Find the force.

Recall Solution 2.1

WHAT: Use with (mirror), so . WHY the : An absorber takes momentum ; a mirror sends the photon back with momentum , so its momentum change is . With that is the factor . Tiny, but never switches off — over months this builds huge (see Solar sails).

Problem 2.2

The same sail is now tilted so its normal makes angle with the Sun direction. Using the simple model , find the force.

Recall Solution 2.2 — study the tilt figure

Figure — Solar radiation pressure
WHAT: Only the projected area catches sunlight. Look at the figure: the incoming beam (yellow) sees the tilted plate edge-on-ish, so its effective width shrinks by . WHY and not : is measured from the normal (the arrow sticking straight out of the plate). When the plate faces the Sun fully → full area → . When the plate is edge-on → catches nothing → . Cosine is the function that is at and at , so it is the right tool. Exactly half the head-on value, since .

Problem 2.3

A dark asteroid chip of area and mass absorbs sunlight at 1 AU, face-on. Find its SRP acceleration.

Recall Solution 2.3

WHAT: with (absorber), so . WHY divide by : orbits respond to acceleration, and .


Level 3 — Analysis

Goal: reason about scaling, ratios, and competing effects.

Problem 3.1

Show that SRP acceleration at Mars (1.52 AU) is of its value at Earth, for the same spacecraft.

Recall Solution 3.1

WHAT: (the and factors are unchanged for the same craft). WHY the square: intensity spreads over , so it falls as (Inverse-square law).

Problem 3.2

Explain, then quantify, why the ratio (SRP acceleration)/(Sun's gravitational acceleration) does not change with distance, and find what it does depend on.

Recall Solution 3.2

WHAT: Write both accelerations. WHY the cancels: both carry a lone . Divide: Every symbol except (and the fixed reflectivity ) is a universal constant. So the ratio is distance-independent but proportional to — a feather-light solar sail feels SRP strongly, a dense probe barely. This is why SRP is not "just extra gravity"; see Orbital perturbations.

Problem 3.3

For the ratio in 3.2 to reach exactly (SRP balancing solar gravity), what area-to-mass ratio is required for a perfect absorber ()? Use .

Recall Solution 3.3

WHAT: Set the ratio and solve for . Numerator: . Denominator (): . A staggering square metres per kilogram — far beyond any real spacecraft, which is why SRP perturbs orbits but never fully cancels the Sun's pull for ordinary craft.


Level 4 — Synthesis

Goal: combine SRP with time, momentum budgets, and other perturbations.

Problem 4.1

The 9 mN sail from Problem 2.1 has total mass . Assuming the force stays constant and always along the velocity direction, estimate the gained in 1 year ().

Recall Solution 4.1

WHAT: , then (constant acceleration). WHY constant-a is fine here: over one year at 1 AU the intensity barely changes, so treating as constant is a good first estimate. A 9 mN whisper becomes nearly 3 km/s of velocity change in a year — that is the whole point of Solar sails: small force, no fuel, enormous integrated effect.

Problem 4.2

In low Earth orbit a balloon satellite feels both SRP and atmospheric drag. Its SRP acceleration is and its drag acceleration is . (a) Which dominates in LEO? (b) At what altitude would you expect SRP to overtake drag, qualitatively?

Recall Solution 4.2

(a) WHAT: Compare magnitudes. . Drag is about stronger, so drag dominates in LEO. (b) WHY altitude flips it: Drag depends on air density, which falls off exponentially with altitude, while SRP is essentially constant with altitude (the Sun's distance barely changes). So climb high enough and drag collapses while SRP holds steady — SRP overtakes drag somewhere in the upper thousands of km. See Atmospheric drag for the density model.

Problem 4.3

A photon of wavelength carries energy with . (a) Find its momentum . (b) How many such photons per second must strike a surface to produce a force of , if fully absorbed?

Recall Solution 4.3

(a) WHAT: . (b) WHY: Force = momentum delivered per second = (rate ) . Set : Nearly a trillion trillion photons per second for one newton — one photon really is nothing; the flood is everything.


Level 5 — Mastery

Goal: full mission-planner reasoning, correct physical model, all cases.

Problem 5.1

For a perfect mirror tilted at angle from the Sun direction, the rigorous force is directed along the plate normal with magnitude . (a) Explain physically where the two cosines come from. (b) Compare at against the simple-model value .

Recall Solution 5.1 — study the two-cosine figure

Figure — Solar radiation pressure
(a) WHY two cosines:

  • First — projected area. The tilted plate intercepts only of the beam (Problem 2.2 logic).
  • Second — direction of momentum change. For a mirror the reflected photons leave symmetrically about the normal, so the net momentum kick points along the normal. Only the component of the incoming momentum along the normal reverses, and that component is the full momentum times . Multiply the two effects → .

Look at the figure: the blue arrow (incoming momentum) splits into a normal part (length ) and a tangential part; only the normal part reverses on reflection, giving the green net force .

(b) Numbers (drop the common factor ; compare vs ):

simple rigorous

At they agree; as you tilt, the rigorous model gives a smaller normal force. A sail designer who used the simple model at would over-predict thrust by a factor of two.

Problem 5.2

A solar sail must "tack" to spiral inward toward the Sun. To lose orbital energy it should orient so SRP has a component opposing its velocity. If the useful along-velocity thrust component for a perfect mirror is (normal force projected onto the velocity direction), find the tilt angle that maximises .

Recall Solution 5.2 — the optimal tack angle

Figure — Solar radiation pressure
WHAT tool and WHY: We want the maximum of a smooth function of . The tool that finds a maximum is the derivative set to zero — at a peak the slope is flat. Define (drop the constant ; scaling a function does not move its peak). WHAT we do: differentiate and set to zero. Using the product rule with and : Set . The solution (i.e. ) is edge-on → zero thrust, a minimum, reject it. The useful root: Look at the figure: the curve rises, peaks near , then falls back to zero at . A real solar sail tacks at about , not head-on, to spiral its orbit most efficiently — a genuine mission-design result you just derived.


Wrap-up recall

Recall One-line takeaways (hide and test)

Photon momentum ::: Base pressure at 1 AU ::: Simple flat-plate force ::: Rigorous mirror normal force ::: Why SRP/gravity is distance-independent ::: both ; ratio Optimal solar-sail tack angle :::


Connections

  • Parent: Solar radiation pressure — the theory these exercises drill.
  • Solar sails — Problems 4.1 and 5.2 are sail-design calculations.
  • Orbital perturbations — SRP as a non-gravitational perturbing force (Problem 3.2).
  • Atmospheric drag — competing LEO force (Problem 4.2).
  • Photon momentum and relativity — origin of (Problems 1.1, 4.3).
  • Inverse-square law — the scaling (Problems 1.2, 3.1).
  • Yarkovsky effect — thermal-recoil cousin acting on spinning asteroids.