kääpiötähdet

Kääpiötähdet, often translated as dwarf stars, refer to stars that are in a stable, hydrogen-burning phase of their life cycle. This is the longest and most common stage for stars, including our own Sun. During this phase, stars generate energy through nuclear fusion in their core, converting hydrogen into helium. The size and luminosity of a dwarf star vary depending on its mass, with more massive stars being larger, hotter, and brighter. Our Sun, a G-type main-sequence star, is an example of a yellow dwarf. Stars in this category range from the smallest and coolest red dwarfs to the largest and hottest blue dwarfs. The term "dwarf star" is often used in contrast to giant or supergiant stars, which are in later, more evolved stages of stellar evolution. Once a dwarf star exhausts its core hydrogen supply, it will evolve off the main sequence, potentially becoming a red giant, white dwarf, or undergoing other dramatic transformations depending on its initial mass. The study of dwarf stars is fundamental to understanding stellar populations, galactic structure, and the evolution of stars throughout the universe.