As an exoplanet transits, it blocks a small patch of the star's rotating disk. Because the star rotates, that blocked patch was contributing a slightly Doppler-shifted sliver of light to the star's integrated spectral lines. Removing it shifts the disk-averaged line centroid — the star briefly appears to have an anomalous radial velocity, even though it never actually moved. This is the Rossiter-McLaughlin (RM) effect.
Local line-of-sight velocity (rigid rotation,
spin axis in sky plane):
v(x) = v sin i* · (x / R_s)
Occulted flux fraction (limb-darkened):
f(x,y) = [A_overlap / (π R_s²)] · [1 − u(1 − μ)]
μ = sqrt(1 − (x² + y²)/R_s²)
Anomalous RV:
ΔRV(t) ≈ − v sin i* · (x(t)/R_s) · f(t)
The planet's true orbital path is a straight chord at fixed impact parameter b. The obliquity λ is the angle between that chord and the star's projected spin axis. Rotating the chord by λ mixes it into (x, y): a small λ (well-aligned system) blocks the approaching hemisphere first and the receding hemisphere second, giving the classic antisymmetric "S-curve" anomaly. Near λ = ±90° (a polar orbit) the planet stays on one Doppler hemisphere for the whole transit, so the anomaly no longer changes sign — this asymmetry is exactly how astronomers measure λ from real RM spectroscopy, most famously revealing that many hot Jupiters orbit misaligned with — or even opposite to — their star's spin.
- λ slider — spin-orbit angle; try 0° (aligned), 90° (polar), 180° (retrograde).
- b slider — how close the chord passes to disk centre; b → 0 gives the largest peak amplitude.
- Rp/Rs — bigger planets occult more flux, scaling the anomaly by (Rp/Rs)².
- v sin i* — faster stellar rotation directly scales the anomaly amplitude.