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R71 has long been known as a blue supergiant and one of the brightest stars in the Magellanic Clouds.It was given a spectral type of B2.5 Iep. [7]By 1974, R71 had increased in brightness from about 11th magnitude to about magnitude 9.2, and examination of historical photographic plates showed that there had been similar changes in the past, with the brightness peaking around 1914 and 1939. [4]
Zeta Puppis (ζ Puppis, abbreviated Zeta Pup, ζ Pup), formally named Naos / n aʊ s /, [10] is the brightest star in the constellation of Puppis.. The spectral class of O4 means this is one of the hottest, and most luminous, stars visible to the naked eye.
Rho Cassiopeiae (/ ˌ r oʊ k æ s i ə ˈ p iː aɪ,-s i oʊ-,-iː /; ρ Cas, ρ Cassiopeiae) is a yellow hypergiant star in the constellation Cassiopeia.It is about 8,150 light-years (2,500 pc) from Earth, yet can still be seen by the naked eye as it is over 300,000 times brighter than the Sun.
The last stars in the list are familiar nearby stars put there for comparison, and not among the most luminous known. It may also interest the reader to know that the Sun is more luminous than approximately 95% of all known stars in the local neighbourhood (out to, say, a few hundred light years), due to enormous numbers of somewhat less ...
Prominent stars in the neighborhood of the Sun (center) This list of nearest bright stars is a table of stars found within 15 parsecs (48.9 light-years) of the nearest star, the Sun, that have an absolute magnitude of +8.5 or brighter, which is approximately comparable to a listing of stars more luminous than a red dwarf.
V838 Monocerotis (Nova Monocerotis 2002) is a cataclysmic binary star in the constellation Monoceros about 19,000 light years (6 kpc) from the Sun.The previously unremarked star was observed in early 2002 experiencing a major outburst, and was one of the largest known stars for a short period following the outburst. [10]
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In other words, stars 10 5 years old lie along the curve labeled 10 5, and similarly for the other 3 isochrones. The Hayashi track is a luminosity–temperature relationship obeyed by infant stars of less than 3 M ☉ in the pre-main-sequence phase (PMS phase) of stellar evolution.