Star
A star is a massive, self-luminous sphere of plasma held together by its own gravity. It shines by converting hydrogen into helium through nuclear fusion in its core, releasing energy across the electromagnetic spectrum.
Stars form in large clouds of gas and dust—called nebulae—where regions collapse under gravity, creating protostars. When core temperatures reach millions of degrees, fusion ignites, marking the birth of a star. Observatories like Hubble and missions such as NASA’s Infrared telescopes have imaged this process in action.
The majority (~90%) of stars are main-sequence stars, fusing hydrogen into helium. These include a broad range of masses—from red dwarfs (small, long-lived, faint) to blue giants and supergiants (massive, hot, and short-lived). Our Sun is a middle-aged G-type main sequence star.
As stars exhaust their hydrogen fuel, their evolution depends on mass. Lower-mass stars become red giants then white dwarfs. More massive stars undergo successive fusion stages, end in supernova explosions, and leave behind neutron stars or black holes.
Stars vary in brightness, size, and color. They are classified using spectral types (O, B, A, F, G, K, M) based on surface temperature and absorption lines. For example, O- and B-type stars are hot and blue; M-type are cool and red.
Stellar remnants include white dwarfs (Earth-sized cores of former stars), neutron stars (city-sized remnants of supernovae), and black holes (extreme-density objects from the most massive stars).
Stars are not static—many rotate, exhibit magnetic activity (like sunspots and flares), and broadcast stellar winds. Their lifecycle enriches the interstellar medium with heavier elements, seeding future generations of stars and planets.
Stars often exist in groups—binary or systems within star clusters and galaxies. Their properties are studied via brightness, spectra, parallax, variability, and statistical surveys by missions like Gaia and Kepler.
Sources
APODs including "Star"
EUVE Sky Map
31 January 2002
The stars beyond the Sun and the distant galaxies should be undetectable at extreme ultraviolet wavelengths. At least that was the conventional wisdom when it was first realized that the space between the stars is filled with hydrogen, a strong absorber of extreme ultraviolet light. But this idea was seriously questioned as it became apparent that interstellar hydrogen was patchy in its distribution and the quest to explore the extreme ultraviolet sky culminated in 1992 with the launch of the EUVE (Extreme UltraViolet Explorer) spacecraft. An all-sky map, based on the satellite's first six months of operation, appears above showing brightness variations in the EUV sky in false color (north is up). EUVE's scanning by orbit gives the picture a striped look while other instrument artifacts are seen as crosses and data gaps are dark. Multiple images of the Moon combine to form the short, bright dashed lines wandering along the middle of the picture. The belt stars of the familiar constellation Orion are fairly easy to make out left of picture center. EUVE's science operations ceased in 2001 but it ultimately detected nearly 1,000 celestial objects, including over three dozen outside our own galaxy. EUVE's voyage of discovery is now complete, and the spacecraft re-entered the Earth's atmosphere yesterday at approximately 11:15 p.m. EST.