Concept information
Preferred term
R Coronae Borealis star
Definition
- An R Coronae Borealis star is a luminous, eruptive variable supergiant, rich in carbon and poor in hydrogen, of spectral type F or G, unusual in that it goes into outburst not by brightening, but by fading. Each minimum is thought to be caused by carbon-rich material puffed off the star during a pulsation cycle. As the cloud moves out, it cools and eventually condenses into carbon dust particles, which absorb much of the light coming from the star's photosphere. Only when the dust has been blown away by radiation pressure, does the star return to its normal brightness. While at maximum light, R Coronae Borealis stars are observed to undergo small-scale, Cepheid-like variations with fluctuations of several tenths of a magnitude and with periods of 20 to 100 days. (Encyclopedia of Science, by David Darling, https://www.daviddarling.info/encyclopedia/R/R_Coronae_Borealis_star.html)
Broader concept
Entry terms
- RCB star
- R CrB star
In other languages
URI
http://data.loterre.fr/ark:/67375/MDL-C64CSDMF-X
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