Astronomy

Reading the light of two stars

Tilt a binary orbit until eclipses appear. Unequal eclipse depths reveal different surface brightnesses; their widths constrain stellar radii.

By Mykhailo Makarov

Actual application image

The model and its limits

Circular binary of adjustable separation and total mass, spherical stars with linear limb darkening and bolometric brightness proportional to T⁴. No tidal distortion or reflection. Photometry is measured along the fixed +Z observer axis.

Equations used in the module

Equations
F = 1 − blocked flux/total flux; surface brightness ∝ T⁴; P² = 4π²a³/(GM).

Related experiments

Back to catalogue

Astronomy

A star's bow wave

Balance an outward stellar wind against an incoming interstellar flow. Change density or speed and watch the stand-off distance respond.

Astronomy

The radioactive light of a supernova

Follow an expanding Type Ia remnant through its first hundred days. Compare nickel mass, diffusion time and apparent brightness at different distances.

Astronomy

Between a planet and a star

Increase the mass while keeping a Jupiter-sized object in view. Compare cooling brown dwarfs with objects capable of sustained hydrogen fusion.