BETA LYRAE STAR Meaning and
Definition
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A Beta Lyrae star is a particular type of binary star system characterized by a periodical variation in its brightness due to the interaction and transfer of mass between its two component stars. This type of stellar system is named after Beta Lyrae, the prototype star of this class identified in the constellation Lyra.
A Beta Lyrae star consists of two main-sequence stars, typically massive and hot, orbiting each other in close proximity. The primary star, which is larger and more luminous, transfers mass to its less massive secondary companion. As a result, a disk or stream of material known as an accretion disk forms around the secondary star, causing an increase in brightness during one phase of the orbital cycle. The mass transfer process occurs through the star's inner Lagrangian point, where both gravitational and centrifugal forces balance out.
The period of mass transfer in a Beta Lyrae star is usually short, ranging from a few days to a few weeks, causing the system's observed brightness to fluctuate and exhibit variations in its spectrum. These systems are considered important in the study of stellar evolution, as their behavior provides valuable insights into the dynamics of binary systems and the mass loss processes in massive stars. Beta Lyrae stars serve as crucial astrophysical laboratories aiding astronomers in investigating the physical properties, evolution, and mass exchange mechanisms within these intriguing stellar configurations.
