how big is it?
The size of the two main stars in the Eta Carinae system is difficult to determine precisely because neither star can be seen directly
Eta Carinae
The size of the two main stars in the Eta Carinae system is difficult to determine precisely because neither star can be seen directly. Eta Carinae B is likely to have a well-defined photosphere and its radius can be estimated from the assumed type of star. An O supergiant of with a temperature of 37,200 K has an effective radius of .
where could be found hii emission nebula regions Sometimes several hundred light-years across, are often associated with giant molecular clouds what does this region mean? It is a region of interstellar atomic hydrogen that is ionized how did it get the name? The term H II is pronounced "H two" by astronomers. "H" is the chemical symbol for hydrogen, and "II" is the Roman numeral for 2. what are it's features? It vary greatly in their physical properties, their size is also known as the Stromgren radius and essentially depends on the intensity of the source of ionising photons and the density of the region, their densities range from over a million particles per cm³ in the ultra-compact H II regions to only a few particles per cm³ in the largest and most extended regions how is it distributed? The reason H II regions rarely appear in elliptical galaxies is that ellipticals are believed to form through galaxy mergers. In galaxy clusters, such mergers are frequent. does it face any problems? UNANSWERABLE which are the special regions it has? Orion Nebula, the Eta Carinae Nebula, and the Berkeley 59 / Cepheus OB4 Complex what is the second one about? It is also known as the Grand Nebula in Carina,  is a large complex area of bright and dark nebulosity in the constellation Carina who discovered it? Nicolas-Louis de Lacaille how is it classified? Eta Carinae A is classified as a luminous blue variable (LBV) due to the distinctive spectral and brightness variations.
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Eta Carinae [SEP] Size
The accretion radius of the secondary is around , suggesting strong accretion near periastron leading to a collapse of the secondary wind. It has been proposed that the initial brightening from 4th magnitude to 1st at relatively constant bolometric luminosity was a normal LBV outburst, albeit from an extreme example of the class. Then the companion star passing through the expanded photosphere of the primary at periastron triggered the further brightening, increase in luminosity, and extreme mass loss of the Great Eruption.