Physic Labs

Optics

Convex and concave mirrors

Trace the principal rays to locate the image formed by a spherical mirror; check f=R/2f = R/2 and the mirror formula 1f=1d+1d′\tfrac{1}{f} = \tfrac{1}{d} + \tfrac{1}{d'} against the positions read on the figure, distinguishing converging and diverging beams.

Middle school

Equipment

  • Spherical mirror (concave/convex) with focal point and center shown in 3D
  • “Incident angle” slider for the probe ray
  • “Focal length” slider changing the mirror curvature
  • Second ray figure highlighting the image position and special rays

Procedure

  1. Identify the focal point and center of curvature

    Drag the canvas to rotate the mirror; locate the vertex, the center of curvature C and the focal point F on the principal axis. Verify on the figure that F lies halfway between the vertex and C, i.e. f=R/2f = R/2 — a property of paraxial beams.

  2. Draw the special rays and locate the image

    Adjust “Incident angle” to watch the axis-parallel ray reflect through F and the ray through F reflect parallel to the axis. Read the intersection point of the rays — the image — and check 1f=1d+1d′\tfrac{1}{f} = \tfrac{1}{d} + \tfrac{1}{d'} with the simulated distances.

  3. Vary the focal length and compare concave–convex

    Drag “Focal length” to change the curvature and see the reflected beam converge sooner or later. Infer the convex case: reflected rays diverge and only their virtual extensions meet at F behind the mirror, so the image is always virtual, upright and reduced.

Simulation

Experiment history

The Book of Optics by Ibn al-Haytham (Alhazen, about 1020) contains the first systematic analysis of concave and convex spherical mirrors, including the famous problem of finding the reflection point on a sphere — later called “Alhazen's problem”. He also described parabolic concave mirrors focusing light to a point. In 1668 Isaac Newton built the first reflecting telescope with a concave spherical mirror, avoiding the chromatic aberration of glass lenses; he presented it to the Royal Society in 1672. Today's large telescopes use parabolic mirrors — the generalized form of the spherical mirror explored in this simulation.

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