Many of them become luminous blue variables with episodes of extreme mass loss.

There are indications that they originate as stars similar to Luminous blue variables with large mass losses before exploding.

In some cases, after becoming supergiants, they can evolve into Wolf-Rayet stars or luminous blue variables.

Luminous blue variables are a class of highly luminous hot stars that display characteristic spectral variation.

Some luminous blue variables are classified as hypergiants, during at least part of their cycle of variation:

The hotter luminous blue variables may be related and show similar short- and long-term spectral and brightness variations with irregular eruptions.

HR Carinae undergoes spectral variations apparently correlated with the light variations similarly to other luminous blue variables.

One study has shown a possible route for low-luminosity post-red supergiant luminous blue variables to collapse, most likely as a type IIn supernova.

Luminous blue variables (LBVs) are massive evolved stars that show unpredictable and sometimes dramatic variations in both their spectra and their brightness.

HR Carinae is a lot like Eta Carinae, both luminous blue variables, and both surrounded by ejected material.

They are also known as Type V supernovae, Eta Carinae analogs, and giant eruptions of luminous blue variables LBV.

Luminous blue variables (LBVs) are a type of star that occur in the same region of the HR diagram as blue supergiants, but are generally classified separately.

Almost all hypergiants exhibit variations in luminosity over time due to instabilities within their interiors, but these are small except for two distinct instability regions where luminous blue variables (LBVs) and yellow hypergiants are found.

Most of them are thought to explode as supernovae without ever becoming blue supergiants again, but some may eventually pass right through the yellow void and become low mass low luminosity Luminous Blue Variables, and possibly Wolf-Rayet stars after that.

It shows pulsations with a period of 37 days and its spectrum is very similar to the ones of Luminous blue variables with moderate mass loss what suggests it's a Luminous blue variable caught pulsating and creating a circumstellar shell.

In 1978, Roberta Humphreys published a study of eight variables in M31 and M33 (excluding Var A) and referred to them as luminous blue variables, as well as making the link to the S Doradus class of variable stars.

Although it does not contain quite such luminous or massive stars as the nearby Arches cluster, it does have the distinction of hosting two of the extremely rare luminous blue variables, the Pistol star and the less well-known FMM 362, and a third just a few parsecs away.

In 1984 in a presentation at the IAU symposium, Peter Conti formally grouped the S Doradus variables, Hubble-Sandage variables, Eta Carinae, P Cygni, and other similar stars together under the term "luminous blue variables" and shortened it to LBV.

Many of them become luminous blue variables with episodes of extreme mass loss.

There are indications that they originate as stars similar to Luminous blue variables with large mass losses before exploding.

In some cases, after becoming supergiants, they can evolve into Wolf-Rayet stars or luminous blue variables.

Luminous blue variables are a class of highly luminous hot stars that display characteristic spectral variation.

Some luminous blue variables are classified as hypergiants, during at least part of their cycle of variation:

The hotter luminous blue variables may be related and show similar short- and long-term spectral and brightness variations with irregular eruptions.

HR Carinae undergoes spectral variations apparently correlated with the light variations similarly to other luminous blue variables.

One study has shown a possible route for low-luminosity post-red supergiant luminous blue variables to collapse, most likely as a type IIn supernova.

Luminous blue variables (LBVs) are massive evolved stars that show unpredictable and sometimes dramatic variations in both their spectra and their brightness.

HR Carinae is a lot like Eta Carinae, both luminous blue variables, and both surrounded by ejected material.

They are also known as Type V supernovae, Eta Carinae analogs, and giant eruptions of luminous blue variables LBV.

Luminous blue variables (LBVs) are a type of star that occur in the same region of the HR diagram as blue supergiants, but are generally classified separately.

Almost all hypergiants exhibit variations in luminosity over time due to instabilities within their interiors, but these are small except for two distinct instability regions where luminous blue variables (LBVs) and yellow hypergiants are found.

Most of them are thought to explode as supernovae without ever becoming blue supergiants again, but some may eventually pass right through the yellow void and become low mass low luminosity Luminous Blue Variables, and possibly Wolf-Rayet stars after that.

It shows pulsations with a period of 37 days and its spectrum is very similar to the ones of Luminous blue variables with moderate mass loss what suggests it's a Luminous blue variable caught pulsating and creating a circumstellar shell.

In 1978, Roberta Humphreys published a study of eight variables in M31 and M33 (excluding Var A) and referred to them as luminous blue variables, as well as making the link to the S Doradus class of variable stars.

Although it does not contain quite such luminous or massive stars as the nearby Arches cluster, it does have the distinction of hosting two of the extremely rare luminous blue variables, the Pistol star and the less well-known FMM 362, and a third just a few parsecs away.

In 1984 in a presentation at the IAU symposium, Peter Conti formally grouped the S Doradus variables, Hubble-Sandage variables, Eta Carinae, P Cygni, and other similar stars together under the term "luminous blue variables" and shortened it to LBV.