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Topic: Blue supergiant

Related Topics

Blue giant

Supergiant

Red giant

Spectral type

Red dwarf star

Supernova

White dwarf

Brown dwarf

Solar mass

Black hole

Solar radius

Supernova 1987a

Sun

Triangulum Galaxy

Ozone layer

	Blue supergiant - Wikipedia, the free encyclopedia
		Blue supergiants are supergiant stars (class I) of spectral type O. They are extremely hot and bright, with surface temperatures of between 20,000 - 50,000°C. They typically have 10 to 50 solar masses on the Hertzsprung-Russell diagram, and can have radii up to about 25 solar radii.
		Blue supergiants represent a slower burning phase in the death of a massive star.
		It was assumed all supernovae were from red supergiants until Supernova 1987A forced revision as the progenitor was a B3 blue supergiant.
	en.wikipedia.org /wiki/Blue_supergiant (577 words)

	Supergiant - Wikipedia, the free encyclopedia
		The Stefan-Boltzmann law dictates that the relatively cool surfaces of red supergiants radiate much less energy per unit area than those of blue supergiants; thus, for a given luminosity red supergiants are larger than their blue counterparts.
		Supergiants occur in every spectral class from young blue class O supergiants stars to highly evolved red class M supergiants.
		However, the progenitor for Supernova 1987A was a blue supergiant.
	en.wikipedia.org /wiki/Supergiant (435 words)

	Supergiant (Site not responding. Last check: 2007-10-23)
		A supergiant is a very large type of star which is ~10 to 50 solar masses on the Hertzsprung-Russell diagram.
		Most supergiants are either blue supergiants existing on the main sequence as type O or B and red supergiants existing off the main sequence.
		For some time, it was believed that large stars would become red supergiants near the end of their lives before going supernova.
	bopedia.com /en/wikipedia/s/su/supergiant.html (280 words)

	Apparent magnitude - Wikipedia, the free encyclopedia
		For this purpose the UBV system is widely used, in which the magnitude is measured in three different wavelength bands: U (centred at about 350 nm, in the near ultraviolet), B (about 435 nm, in the blue region) and V (about 555 nm, in the middle of the human visual range in daylight).
		Since cooler stars, such as red giants and red dwarfs, emit little energy in the blue and UV regions of the spectrum their power is often under-represented by the UBV scale.
		On early 20th-century and older orthochromatic (blue-sensitive) photographic film, the relative brightnesses of the blue supergiant Rigel and the red supergiant Betelgeuse irregular variable star (at maximum) are reversed compared to what our eyes see since this archaic film is more sensitive to blue light than it is to red light.
	en.wikipedia.org /wiki/Apparent_magnitude (1435 words)

	supergiant
		Supergiants have luminosities of 10,000 to 100,000 solar luminosities and radii of 20 to several hundred solar radii (about the size of Jupiter's orbit).
		The two commonest types are red supergiants, exemplified by Betelgeuse and Antares, and blue supergiants, exemplified by Rigel.
		Through a vigorous stellar wind, red supergiants steadily lose their extended atmospheres and turn into smaller but much hotter blue supergiants.
	www.daviddarling.info /encyclopedia/S/supergiant.html (264 words)

	eSky: Rigel
		The pulsating blue supergiant Rigel has a diameter of about 100 million kilometres, some seventy times that of the Sun.
		A blue supergiant star that remains very bright despite lying almost 800 light years away.
		The famous blue star Rigel forms the western foot of the Hunter Orion, and indeed its Arabic name means 'Leg of the Giant'.
	www.glyphweb.com /esky/stars/rigel.html (140 words)

	Astronomy
		They then expand to a supergiant star and go on to fuse elements such as carbon, oxygen and silicon in their cores, providing that they can reach sufficiently high temperatures to ignite such reactions.
		Blue supergiants produce intense UV radiation which ionises gas in nebulae such as the Orion nebula (see left), giving rise to spectacular displays of colour.
		The surprise discovery that the progenitor star of supernova 1987A was a blue supergiant is yet another reason to study these stars.
	www.star.ucl.ac.uk /~scs/astronomy.html (470 words)

	t3_s1'99
		The Sun is a (a) giant (b) supergiant (c) white dwarf (d) main sequence star.
		A star the same color as the Sun, but the size of the Earth would be a (a) white dwarf (b) pygmy star (c) neutron star (d) planetary nebula.
		Blue skies and red sunsets are due to (a) interstellar dust (b) interference (c) diffraction (d) Rayleigh scattering.
	www.uark.edu /misc/clacy/ASTR2003/tests/t3_s1'99.htm (998 words)

	[No title]
		The difference between red and blue supergiants is that the blue variety are believed to have evolved from red supergiants after shedding much of their extended atmosphere.
		The presence of this glowing gas in the first observations of the supernova means that it must be close to the explosion and that the star must have been in a red supergiant phase shortly before its demise.
		Prior to the 1987 blue supergiant explosion, the most recent nearby supernova that could be seen without a telescope took place in 1604 and was observed by Johannes Kepler, one of the great German astronomers.
	science.ksc.nasa.gov /shuttle/missions/status/r93-63 (801 words)

	AstronomyNZ - Star Data North
		A spectroscopic binary system in which the primary star is a blue supergiant (B0 Ia) 30,200 times brighter than the Sun.
		A binary system in which the primary star is a blue supergiant (O9.5 Ib) 10,760 times brighter than the Sun.
		The cluster, which is 368 light years away, is immersed in a cloud of dust and ice crystals that reflects the blue light of the brightest stars.
	www.astronomynz.org.nz /nightsky/star_charts/bright_stars_north.htm (1107 words)

	Hubble Space Telescope, Thumbnail Views page 7
		NGC 3603 (cont.): The color difference between the supergiant's bipolar outflow and the diffuse interstellar medium in the giant nebula dramatically visualizes the enrichment in heavy elements due to synthesis of heavier elements within stars.
		NGC 3603 (cont.): This is a close-up of the blue supergiant called Sher 25.
		The beefy star [lower center] is embedded in the bright blue bubble.
	www.laughtergenealogy.com /bin/hubble/thumbs07.html (1871 words)

	Learn more about Apparent magnitude in the online encyclopedia. (Site not responding. Last check: 2007-10-23)
		For this purpose the UBV system is widely used, in which the magnitude is measured in three different wavelength bands: U (centred at about 350 nm, in the near ultraviolet), B (about 435 nm, in the blue region) and V (about 555 nm, in the middle of the human visual range).
		Since cooler stars, such as red giants and red dwarfs, emit little energy in the blue and UV reaches of the spectrum their power is often under-represented by the UBV scale.
		On photographic film, the relative brightnesses of the blue supergiant Rigel and the red supergiant Betelgeuse are reversed compared to what our eyes see since film is more sensitive to blue light than it is to red light.
	www.onlineencyclopedia.org /a/ap/apparent_magnitude.html (860 words)

	Frontiers - Feature
		Their study is important because it provides the opportunity to investigate the evolutionary processes of supergiant stars which are massive nuclear furnaces and the source of most of the heavy chemical elements in all galaxies (the heaviest elements form when these massive stars explode as supernovae).
		Studies of the elemental composition in similar supergiants and their nebulae are also inconsistent with a previous RSG phase, implying that the nebulae must be ejected during their blue period.
		In fact, in the Milky Way, there is not one single blue supergiant, or nebula surrounding a blue supergiant, that shows element abundances indicating that the star evolved through a previous red supergiant phase.
	www.pparc.ac.uk /frontiers/latest/feature.asp?article=12F5&style=feature (1319 words)

	Multiwavelength 30 Doradus - Tarantula Nebula
		The primary sources of illumination are hot and young blue supergiant stars buried within the central core of the nebula.
		Emission at 3.6 microns is depicted in blue, 4.5 microns in green, 5.8 microns in orange, and 8.0 microns in red.
		The fainter (green) emission in the center of the image, and to the immediate south, is the faint glow from a population of other older and weaker SNR distributed throughout the cluster.
	coolcosmos.ipac.caltech.edu /cosmic_classroom/multiwavelength_astronomy/multiwavelength_museum/30dor.html (902 words)

	[No title] (Site not responding. Last check: 2007-10-23)
		SK -69 202 is a blue supergiant whereas the typical TYPE II supernova is thought to be produced by a red supergiant.
		The inference that TYPE II supernovae are produced by red supergiants is based on theoretical modeling of the light curves of supernovae and numerical simulations of massive stars.
		So, although the observation that a blue supergiant exploded was initially puzzling, it turned out that such an observation was easily accomodated by theory and it in fact explained some of the odd behavior of the light curve of SN1987A.
	zebu.uoregon.edu /~imamura/122/mar4/sk.html (480 words)

	Bresolin et al., Spectroscopy of Blue Supergiants in the Spiral Galaxy NGC 300 (Site not responding. Last check: 2007-10-23)
		Spectroscopy of Blue Supergiants in the Spiral Galaxy NGC 300
		Of the 62 spectroscopically confirmed blue supergiants, with spectral types ranging from late-O to F, 57 have types between early-B and mid-A. We present a detailed spectral catalog containing identification, magnitudes, colors and spectral types.
		We employ synthetic spectra calculated from blue supergiant model atmospheres for different metallicities to determine metal abundances for two A0 supergiants of the sample.
	www.ifa.hawaii.edu /publications/preprints/01preprints/Bresolin_01-29.html (334 words)

	Wikinfo \| Blue giant
		In astronomy, a blue giant or blue supergiant is a very hot, very
		massive (at least 18 times the mass of the sun) blue star of spectral type O or B. In the standard Hertzsprung-Russell diagram, blue giants are found on the upper left corner, thanks to their high luminosity and early spectral type.
		Images, some of which are used under the doctrine of Fair use or used with permission, may not be available.
	www.wikinfo.org /wiki.php?title=Blue_giant (247 words)

	Stars (Site not responding. Last check: 2007-10-23)
		A collection of blue- and white-colored stars near the left of the image are among the most massive stars known anywhere in the universe.
		In the blue region on the right edge, low and medium energy X rays have been filtered out by a cloud of dust and gas in the remnant.
		The blue color indicates that the object is hot, as expected from the bright X-ray emission.
	www.cosmiclight.com /imagegalleries/stars.htm (6321 words)

	AstronomyNZ - Star Data South
		It is a white supergiant (A9 Ib) 13,800 times brighter than the Sun.
		It is a blue supergiant (O5 Ia) 20,330 times brighter than the Sun.
		A spectroscopic binary consisting of the brightest known Wolf-Rayet star and a blue supergiant (WC8, O9 I).
	www.astronomynz.org.nz /nightsky/star_charts/bright_stars_south.htm (726 words)

	Luminous Blue Variables
		The defining characteristics of luminous blue variables are presented and interpreted in an evolutionary context.
		This scenario may lead an LBV to a Wolf-Rayet phase or even a supernova, which perhaps could occur either during the outburst phase as a red supergiant or the quiescent phase as a blue supergiant such as the progenitor of SN 1987A.
		These temperature variations should not be confused with the ‘blue loops’ that are thought to occur in the post-main-sequence evolution of massive stars due to nuclear evolution; in LBVs the variability is due to photospheric instabilities and changes" (Parker et al.
	www.peripatus.gen.nz /Astronomy/LumBluVar.html (2774 words)

	eNature: Articles: Detail
		Rigel is also a supergiant, though it's in a highly active stage of its life, whereas Betelgeuse is nearing the end of its life and has cooled considerably (thus the red color).
		Rigel will be a blue supergiant for only about 1.5 million years, not long at all considering typical life spans of stars and durations of individual phases.
		When Rigel burns through its current phase it will become a red supergiant, like its neighbor Betelgeuse, which by that time will no longer be visible, having either exploded as a supernova or simply expended its energy and faded from view.
	www.enature.com /articles/detail.asp?storyID=246 (768 words)

	Colors of the cosmos: red, green, and blue may mean one thing to a scientist and something different to everybody else ...
		Professional photographers, however, would swear the Sun is blue; daylight film is color balanced on the expectation that the light source (presumably the Sun) is strong in the blue part of the spectrum.
		And it's not uncommon to see an image of a spiral galaxy that has been color coded for its rotation: the parts coming toward you are shades of blue, while the parts moving away are shades of red.
		What we do is assign the three colors to which the human retina is sensitive (red, green, and blue, or RGB for short) to three different parts of the spectrum.
	www.findarticles.com /p/articles/mi_m1134/is_2_111/ai_83553537 (926 words)

	[68.02] Extragalctic Stellar Astronomy (Site not responding. Last check: 2007-10-23)
		Two groups of objects, blue supergiant stars and Planetary Nebulae are discussed.
		It is shown how the parameters of the most luminous blue supergiants (temperature, gravity, radii, luminosities, masses, mass-loss rates, wind velocities, abundances) in different galaxies are determined using spectral information from the UV to the IR and hydrodynamic NLTE model atmospheres including the effects of stellar winds and spherical extension.
		Recent results for O, B, A-supergiants in galaxies of the Local Group and in spirals out to 7 Mpc distance are presented.
	www.aas.org /publications/baas/v32n4/aas197/890.htm (220 words)

	Rho Cassiopeiae
		In theory, hydrogen-fusing dwarf stars of 10 to around 60 Solar-masses first evolve as spectral type O to become blue supergiants and then progress to become red supergiants (type M).
		Stars with 30 to 60 Solar-masses then "loop back" from swollen and cooler, red supergiant phase back into much hotter but smaller blue supergiants (Stothers and Chin, 2001); in contrast, those starting with more 60 Solar-masses remain as blue supergiants.
		Rho Cas appears to be changing back from being a red supergiant, when it may have been five times larger (James Kaler, 2002; Israelian et al, 1999; and Cornelius de Jager, 1997).
	www.solstation.com /x-objects/rho-cas.htm (1127 words)

	Orion the Hunter
		Gamma Orionis, Bellatrix (05h25m +06° 21') means "female warrior." Bellatrix is a class B2 blue supergiant with a magnitude of 1.6.
		The spectroscopic companion is a blue star, the visual companion is 52 arcseconds from Mintaka.
		Kappa Orionis, Saiph (05h48m -09° 40') is a 2.1 magnitude class B0.5 blue supergiant.
	starryskies.com /The_sky/constellations/orion.html (639 words)

	SN1987A
		Once the star has become a blue supergiant, it develops a powerful stellar wind that sweeps the disc outwards.
		The outer rings may be 'swept-up' parts of a shock region in the shape of a double cone, produced by the interaction of stellar winds from each of the two stars before they merged.
		Material that flowed out during the red supergiant phase was subsequently compressed by the blue supergiant wind to form the ring.
	www.xs4all.nl /~carlkop/blast.html (2321 words)

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