eclipsingbinäriks

An eclipsing binary is a type of binary star system where two stars orbit a common center of mass, and their orbital plane is oriented such that one star periodically passes in front of the other as seen from Earth. This phenomenon causes the total brightness of the system to fluctuate. When the dimmer star passes in front of the brighter star, the system appears dimmer, and when the brighter star passes in front of the dimmer star, the system also appears dimmer, although usually to a lesser extent. The period of these brightness variations is equal to the orbital period of the binary system.

The light curve, which is a graph of the system's brightness over time, is a key characteristic of an eclipsing binary. The shape of the light curve can reveal information about the relative sizes of the stars, their temperatures, and their orbital separation. There are several types of eclipsing binaries, including Algol-type, W Ursae Majoris-type, and beta Lyrae-type systems, each distinguished by the specific patterns in their light curves.

Eclipsing binaries are invaluable tools for astronomers. By studying the precise timing and depth of the eclipses, astronomers can accurately determine fundamental stellar parameters such as the masses, radii, luminosities, and temperatures of the individual stars. This makes them crucial for calibrating stellar models and understanding stellar evolution. They are also used to detect exoplanets; if a planet passes in front of one of the stars in an eclipsing binary, it can cause an additional dip in brightness that can be detected.