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Stellar brightness is based on the apparent visual magnitude as perceived by the human eye, from the brightest stars of 1st magnitude to the faintest at 6th magnitude. Since the invention of the optical telescope and the documenting of binary stars and multiple star systems, stellar brightness could be expressed as either individual (separate ...
Consequently, a magnitude 1 star is about 2.5 times brighter than a magnitude 2 star, about 2.5 2 times brighter than a magnitude 3 star, about 2.5 3 times brighter than a magnitude 4 star, and so on. This is the modern magnitude system, which measures the brightness, not the apparent size, of stars.
A difference of 1.0 in magnitude corresponds to the brightness ratio of , or about 2.512. For example, a magnitude 2.0 star is 2.512 times as bright as a magnitude 3.0 star, 6.31 times as magnitude 4.0, and 100 times magnitude 7.0.
Star Normal maximum brightness is 2.29; magnitude 0.7 once observed 2.39 Epsilon Boötis: Binary star system 2.41 2.14 Mintaka: Triple star system 2.41 Kappa Scorpii: Binary star system Maximum brightness 2.42 2.31 Beta Pegasi: Star 2.42 Eta Ophiuchi: Binary star system 2.440 Phecda: Binary star system 2.45 2.38 Eta Canis Majoris: Star 2.46 ...
Galaxy color–magnitude diagram – Chart depicting the relationship between brightness and mass of large star systems; Hayashi track – Luminosity–temperature relationship in stars; Henyey track – path taken by pre-main-sequence stars in the Hertzsprung–Russell diagram
Factor ()Multiple Value Item 0 0 lux 0 lux Absolute darkness 10 −4: 100 microlux 100 microlux: Starlight overcast moonless night sky [1]: 140 microlux: Venus at brightest [1]: 200 microlux
It includes positions, parallaxes, and proper motions for about 1.3 billion stars and positions of an additional 300 million stars, red and blue photometric data for about 1.1 billion stars and single colour photometry for an additional 400 million stars, and median radial velocities for about 7 million stars between magnitude 4 and 13.
The Yale Bright Star Catalogue has been steadily enhanced since the Yale astronomer Frank Schlesinger published the first version in 1930; even though the YBS is limited to the 9110 objects already in the catalog, the data for the objects already listed is corrected and extended, and it is appended with a comments section about the objects. The ...