Generally only the more evolved supergiants show hypergiant properties, since their instability increases after high mass-loss and some increase in luminosity. blue hypergiant star and an LBV
Part of the theorized population III of stars, their existence is necessary to explain observations of elements other than hydrogen and helium in quasars. Known as the Garnet Star on account of its deep red colour, it is large enough to engulf over a billion Suns within it. is red hypergiant (or perhaps a red supergiant or the supergiant
Above:
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.
magnitude -0.8), emitting almost as much light as a supernova
Wolf-Rayet stars are very hot and luminous stars with a surface
these starts accumulated so much. And as the name indicates, these stars are huge…super huge. Perhaps surprisingly, this increases the hypergiant's luminosity still further, and the additional pressure of escaping radiation causes the star's outer surface to swell and cool, transforming it into a yellow, orange or red hypergiant depending on exactly where the balance is reached. This means that they do not increase their luminosity as dramatically as lower-mass stars, and they progress nearly horizontally across the HR diagram to become red supergiants. Due to their strong emission lines, they can be identified in nearby galaxies. Though they are not the largest known stars, these are the brightest and most energetic. magnitude -0.8), emitting almost as much light as a supernova
)and a solitary star. A very small number of Mira variables and other late AGB stars have supergiant luminosity classes, for example α Herculis. Supergiant spectra are frequently annotated to indicate spectral peculiarities, for example B2 Iae or F5 Ipec. Supergiants are also evolved stars with higher levels of heavy elements than main-sequence stars. Blue supergiants are supergiant stars (class I) of spectral type O. Above: imaged in the ultra-violet, showing warm magnesium-rich gas
It is a variable (and probable) binary star and it is
Rare red hypergiants, however, are the biggest stars in the universe. finished accreting mass when they begin to, . For example, luminous blue variables are extremely bright stars that show long, slow changes in brightness with occasional outbursts, and include both supergiant and hypergiant stars. storage unit for, The
[16], 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.[17].
Above: a
Stars with initial masses above 8-10 M☉ quickly and smoothly initiate helium core fusion after they have exhausted their hydrogen, and continue fusing heavier elements after helium exhaustion until they develop an iron core, at which point the core collapses to produce a Type 2 supernova. Rare red hypergiants, however, are the biggest stars … Very rare stars, as well as hypergiants, they can include blue supergiants. Stars that evolve into this area also become very unstable, shedding vast quantities of their masses. Asymptotic-giant-branch (AGB) and post-AGB stars are highly evolved lower-mass red giants with luminosities that can be comparable to more massive red supergiants, but because of their low mass, being in a different stage of development (helium shell burning), and their lives ending in a different way (planetary nebula and white dwarf rather than supernova), astrophysicists prefer to keep them separate. The absolute magnitude of this star approaches that of some of the … what is it? blue variable)
Supergiants are evolved stars and may have undergone convection of fusion products to the surface. The majority of them are intermediate mass stars fusing helium in their cores and will eventually transition to the asymptotic giant branch. Eta Carinae (Tseen She, lit. Eta Carinae is the bright dot at the centre and the two large spherical objects either side of it are the remains of a huge outburst some 160 years earlier. thought to have been an O star of about 30 - 40 solar masses
Size comparison between sun and the blue giant star Rigel (beta Ori), which is approx. The progenitor for the unusual type II Supernova 1987A was a blue supergiant,[26] thought to have already passed through the red supergiant phase of its life, and this is now known to be far from an exceptional situation. supernova, but the star survives, it simply blasts off a vast
They feature strong, broad emission lines of helium and nitrogen, carbon, and oxygen. They are usually supergiants or hypergiants, occasionally with Wolf-Rayet spectra—extremely luminous, massive, evolved stars with expanded outer layers, but they are so distinctive and unusual that they are often treated as a separate category without being referred to as supergiants or given a supergiant spectral type.
The dividing line becomes blurred at around 7–10 M☉ (or as high as 12 M☉ in some models[11]) where stars start to undergo limited fusion of elements heavier than helium. There are only about a dozen
Above their area is another quaintly named zone - the "Yellow Evolutionary Void". These "luminous blue variables" do pretty much what it says on the tin: they're luminous, blue and variable.
[15], There are supergiant stars at all of the main spectral classes and across the whole range of temperatures from mid-M class stars at around 3,400 K to the hottest O class stars over 40,000 K. Supergiants are generally not found cooler than mid-M class. [12] Many post-AGB stars receive spectral types with supergiant luminosity classes. Their blue colour shows that their temperature is around 10,000 to 15,000 above. They are essentially supergiants (either red, yellow or blue) … [7] In 1943 Morgan and Keenan formalised the definition of spectral luminosity classes, with class I referring to supergiant stars. [8] The same system of MK luminosity classes is still used today, with refinements based on the increased resolution of modern spectra. Above:
They can have luminosities anywhere from about 10,000 to a million times that of the Sun. [9] Supergiants occur in every spectral class from young blue class O supergiants to highly evolved red class M supergiants. Similarly, the Great Red Spot (Jupiter’s largest storm) could swallow Earth twice over, while over 1,300 Earths could easily fit inside the planet itself. The "blue" description comes from their high temperatures, they are extremely luminous and this may vary considerably over their brief existence. In some cases, the shockwave from the explosion can ignite clouds of material ejected from the star thousands of years before, creating an exceptionally bright supernova explosion known as a hypernova. The term hypergiant stars describe a star's luminosity rather than its physical size, so blue hypergiants can actually be smaller than the standard red giants formed by normal Sun-like stars towards the end of their lives, despite being many times brighter.
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