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Supergiant star

They go on to successively ignite heavier elements, usually all the way to iron. They cannot lose enough mass to form a white dwarf, so they will leave behind a neutron star or black hole remnant, usually after a core collapse supernova explosion.

A much smaller grouping consists of very low-luminosity G-type supergiants, intermediate mass stars burning helium in their cores before reaching the The relative numbers of blue, yellow, and red supergiants is an indicator of the speed of stellar evolution and is used as a powerful test of models of the evolution of massive stars.The supergiants lie more or less on a horizontal band occupying the entire upper portion of the HR diagram, but there are some variations at different spectral types. Rogelio Bernal Andreo, CC By-SA.30 What Makes a Star a Red Supergiant? • MACS J1149 Lensed Star 1 (or Icarus) – most distant individual star detected Cool supergiants show enhanced helium and nitrogen at the surface due to convection of these fusion products to the surface during the main sequence of very massive stars, to dredge-ups during shell burning, and to the loss of the outer layers of the star.
The progenitor for the unusual type II Supergiants are rare and short-lived stars, but their high luminosity means that there are many naked-eye examples, including some of the brightest stars in the sky.

Also unlike lower-mass stars, red supergiants are massive enough to fuse elements heavier than helium, so they do not puff off their atmospheres as planetary nebulae after a period of hydrogen and helium shell burning; instead, they continue to burn heavier elements in their cores until they collapse. The constellation Orion holds the red supergiant star Betelgeuse (the red star in the upper left part of the constellation. If our Sun is an average sized star, there are some true monsters out there. A B0 main sequence star has an absolute magnitude of about −5, meaning that all B0 supergiants are significantly brighter than absolute magnitude −5. Stars with initial masses above 8-10 There are several categories of evolved stars which are not supergiants in evolutionary terms but may show supergiant spectral features or have luminosities comparable to supergiants.

Bolometric luminosities for even the faintest blue supergiants are tens of thousands of times the sun (The very hottest supergiants with early O spectral types occur in an extremely narrow range of luminosities above the highly luminous early O main sequence and giant stars. an exceptionally luminous star whose diameter is more than 100 times that of the sun, as Betelgeuse or Antares.

Get kids back-to-school ready with Expedition: Learn! They vary greatly in radius, usually from 30 to 500, or even in excess of 1,000 solar radii(R☉). Our editors will review what you’ve submitted and determine whether to revise the article. Overview of several types of stars, notably the red dwarf, red giant, supergiant, white dwarf, and brown dwarf.This article was most recently revised and updated by In 1956, the astronomers Feast and Thackeray used the term super-supergiant (later changed into hypergiant) for stars with an absolute magnitude brighter than M V = −7 (M Bol will be larger for very cool and very hot stars, for example at least −9.7 for a B0 hypergiant). The supergiants are …



History at your fingertips For very hot and very cool stars, the bolometric luminosity is dramatically higher than the visual luminosity, sometimes several magnitudes or a factor of five or more.

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