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A red supergiant star orbited by a smaller B-type main-sequence star with a radius estimated between 13 [54] and 25 R ☉. [55] Widely recognised as being among the largest known stars. [21] Another estimate give a radius of 660 R ☉ [25] based on the Gaia DR3 distance of 1 kpc. [35] U Lacertae A 1,013 [25] L/T eff: KW Sagittarii: 1,009 ± 142 ...
A giant star has a substantially larger radius and luminosity than a main-sequence (or dwarf) star of the same surface temperature. [1] They lie above the main sequence (luminosity class V in the Yerkes spectral classification) on the Hertzsprung–Russell diagram and correspond to luminosity classes II and III. [2]
The nearest white giant. Capella A 42.919 ± 0.049 [9] G8III [9] 11.98 ± 0.57 [9] 2.5687 [9] 0.03 [10] The nearest yellow giant, together with Capella A. With a magnitude of 0.08, [11] the Capella star system is the 6th-brightest star in the night sky. Capella B G0III [9] 8.83 ± 0.33 [9] 2.48 [9] 0.16 [10] The nearest yellow giant, together ...
This is a list of the nearest supergiant stars to Earth, located at a distance of up to 1,100 light-years (340 parsecs) from Earth. Some of the brightest stars in the night sky, such as Rigel and Antares, are in the list.
One region contained larger and more luminous stars of spectral types A to M and received the name giant. [1] Subsequently, as they lacked any measurable parallax, it became apparent that some of these stars were significantly larger and more luminous than the bulk, and the term super-giant arose, quickly adopted as supergiant. [2] [3] [4]
In the Hayashi limit, stars above this radius would be too unstable and simply do not form. Red supergiants have masses between about 10 M ☉ and 30 or 40 M ☉. [10] Main-sequence stars more massive than about 40 M ☉ do not expand and cool to become red supergiants. Red supergiants at the upper end of the possible mass and luminosity range ...
Rare ultramassive stars that exceed this limit – for example in the R136 star cluster – might be explained by the following proposal: Some of the pairs of massive stars in close orbit in young, unstable multiple-star systems must, on rare occasions, collide and merge when certain unusual circumstances hold that make a collision possible. [3]
VY Canis Majoris (abbreviated to VY CMa) is an extreme oxygen-rich red hypergiant or red supergiant (O-rich RHG or RSG) and pulsating variable star 1.2 kiloparsecs (3,900 light-years) from the Solar System in the slightly southern constellation of Canis Major.