Glossary term: Red Supergiant
Description: A red supergiant is a star that has a comparatively cool surface but a radius typically several hundred or even thousands of times that of a main sequence star like our Sun. The lower temperature gives the surface a reddish appearance, while the large diameter makes the star shine considerably brighter than our Sun.
Red supergiants are formed in the same way as red giants but from precursor stars that are considerably more massive. Both types were originally main sequence stars, that is, stars like our Sun that burn hydrogen to helium in their cores via nuclear fusion (although with masses much higher than the Sun's in the case of red supergiants). When such a star runs out of hydrogen fuel, it begins to burn helium into heavier elements. At that time, the star expands, its surface cooling down in the process, and with its increased size the star becomes more luminous. The remaining lifetimes of red supergiants amount to only a few tens of thousands of years.
Examples of red supergiants are Betelgeuse, in Orion, and Antares, in Scorpius. Like red giants, red supergiants are prone to pulsation and mass loss. Most, possibly all, red supergiants end in a supernova explosion, ejecting much of their gas, with their cores collapsing to form neutron stars or black holes.
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Term and definition status: This term and its definition have been approved by a research astronomer and a teacher
The OAE Multilingual Glossary is a project of the IAU Office of Astronomy for Education (OAE) in collaboration with the IAU Office of Astronomy Outreach (OAO). The terms and definitions were chosen, written and reviewed by a collective effort from the OAE, the OAE Centers and Nodes, the OAE National Astronomy Education Coordinators (NAECs) and other volunteers. You can find a full list of credits here. All glossary terms and their definitions are released under a Creative Commons CC BY-4.0 license and should be credited to "IAU OAE".
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