luminous blue variable

'luminous blue variable' can also refer to...

luminous blue variable

Modelling luminous-blue-variable isolation

Radio images of four luminous blue variable stars

New luminous blue variables in the Andromeda galaxy

Remarks on a model for outbursts in luminous blue variables

The ejecta from the luminous blue variable star P Cygni

The isolation of luminous blue variables: on subdividing the sample

WS1: one more new Galactic bona fide luminous blue variable

MN112: a new Galactic candidate luminous blue variable*

Infrared [Fe II] emission in the circumstellar nebulae of luminous blue variables

Discovery of a new Galactic bona fide luminous blue variable with Spitzer★

Luminous blue variable eruptions and related transients: diversity of progenitors and outburst properties

Discovery of two new Galactic candidate luminous blue variables with Wide‐field Infrared Survey Explorer*

On luminous blue variables as the progenitors of core-collapse supernovae, especially Type IIn supernovae

Radio detection of nebulae around four luminous blue variable stars in the Large Magellanic Cloud

The unprecedented 2012 outburst of SN 2009ip: a luminous blue variable star becomes a true supernova

Luminous blue variables are antisocial: their isolation implies that they are kicked mass gainers in binary evolution

The candidate luminous blue variable G79.29+0.46: a comprehensive study of its ejecta through a multiwavelength analysis

Identifying Type IIn supernova progenitors in our Galaxy: the circumstellar environment of the Galactic luminous blue variable candidate Gal 026.47+0.02


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An extremely hot, massive star at the very top of the Hertzsprung–Russell diagram, with a luminosity up to 10 million times or more that of the Sun; also known as an S Doradus star or a Hubble–Sandage variable. Such stars display variability in brightness and colour on various scales, ranging from rapid microvariations of 0.1–0.2 mag. to rare outbreaks of catastrophic mass loss on a timescale of centuries when the brightness can increase by 3 magnitudes or more. One famous example of the latter type is Eta Carinae. LBVs represent a very short-lived (perhaps as little as 40 000 years) phase in the evolution of young, massive stars, during which they undergo deep erosion of the outer layers before they enter the Wolf–Rayet phase. The spectra typically exhibit prominent emission lines of H, He, and iron, often with P-Cygni profiles. During quiescence the spectrum may be B-type, while at maximum brightness the star may appear as an A- or F-type supergiant. The luminosity and temperature are also highly variable, due to surrounding shells of ejected matter which absorb the star's visible and bluer radiation and re-radiate it at longer wavelengths.

Subjects: Astronomy and Astrophysics.

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