sekundääripeiliksi

Sekundääripeiliksi, often translated as secondary mirror, is a crucial component in reflecting telescopes. Its primary function is to redirect the light collected by the main mirror (primary mirror) towards the eyepiece or imaging sensor. Without a secondary mirror, the light would simply continue in a straight line and would not be focused in a usable location.

There are several types of secondary mirrors, with the most common being flat or convex. In a Newtonian telescope, a flat secondary mirror is typically positioned at a 45-degree angle to the optical path. This angle reflects the focused light out of the side of the telescope tube, where the eyepiece is mounted. In Cassegrain and similar telescope designs, a convex secondary mirror is used. This mirror reflects the light back down through a hole in the center of the primary mirror, effectively shortening the physical length of the telescope while increasing its focal length.

The size, shape, and precise positioning of the secondary mirror are critical for the performance of a reflecting telescope. Aberrations introduced by an improperly designed or positioned secondary mirror can degrade image quality. The secondary mirror also obstructs a small portion of the incoming light, which is a trade-off for achieving a more compact and user-friendly optical design. The design and manufacturing of secondary mirrors require high precision to ensure they are perfectly shaped and aligned for optimal light reflection and image formation.