Astrophysics (Index)About

helium star

(O or B star with very strong helium lines)

The term helium star is naturally used for stars with some helium-related characteristics (in some cases due to a decided lack of hydrogen) but the term has been used for various such scenarios. Perhaps the common current usage is an O-type star or B-type star with stronger-than-usual helium spectral lines.

A different use of the term is for a white dwarf that has begun helium burning through merger with a binary companion. A third, older use, was as a synonym for B-type star.

The term extreme helium star (sometimes shortened to helium star) is used for stars with nearly no hydrogen, helium making up most of the star. Such a star burning helium in an analogous manner to hydrogen burning in a main sequence star is said to be on a helium main sequence (helium MS). The presumption is something removed the hydrogen, such as interaction with a binary companion, or an extreme stellar winds. They are PV Telescopii variables (PVTEL).


(star type)
Further reading:
https://en.wikipedia.org/wiki/Helium_star
https://en.wikipedia.org/wiki/Extreme_helium_star
https://www.oxfordreference.com/display/10.1093/oi/authority.20110803095929296
https://en.wiktionary.org/wiki/helium_star
https://vajiramias.com/current-affairs/extreme-helium-star-ehe/5ef02e651d5def608ab84a7a/
https://ui.adsabs.harvard.edu/abs/2019MNRAS.487.2538J/abstract
https://ui.adsabs.harvard.edu/abs/2022MNRAS.511L..66W/abstract
https://ui.adsabs.harvard.edu/abs/2006ApJ...648L.143P/abstract

Referenced by page:
supergiant

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