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Yellow supergiants generally have spectral types of F and G, although sometimes late A or early K stars are included. [1] [2] [3] These spectral types are characterised by hydrogen lines that are very strong in class A, weakening through F and G until they are very weak or absent in class K. Calcium H and K lines are present in late A spectra, but stronger in class F, and strongest in class G ...
R Coronae Borealis is a low-mass yellow supergiant star in the constellation of Corona Borealis.It is the prototype of the R Coronae Borealis variable of variable stars, which fade by several magnitudes at irregular intervals.
The primary component of the φ Cassiopeiae system is a very luminous yellow supergiant. Its absolute magnitude is comparable to some yellow hypergiants but it does not show the level of mass loss and instability that would qualify it as a hypergiant itself.
RW Cephei has been classified as a semi-regular variable star of type SRd, meaning that it is a slowly varying yellow giant or supergiant. The General Catalogue of Variable Stars cites a 1952 study giving a period of approximately 346 days, [ 35 ] [ 5 ] while other studies suggest different periods and certainly no strong periodicity.
Intrinsic variable types in the Hertzsprung–Russell diagram showing the Yellow Hypergiants above (i.e. more luminous than) the Cepheid instability strip. A yellow hypergiant (YHG) is a massive star with an extended atmosphere, a spectral class from A to K, and, starting with an initial mass of about 20–60 solar masses, has lost as much as half that mass.
V1027 Cygni is a luminous yellow supergiant star located in the constellation of Cygnus, about 14,000 light years away. For a time, it was thought that it could be a low-mass post-AGB star, however recent parallax measurements published in Gaia DR3 have shown this to likely not be the case, and instead it is likely a massive yellow supergiant star.
V810 Centauri is a double star consisting of a yellow hypergiant [3] primary (V810 Cen A) and blue giant secondary (V810 Cen B). It is a small amplitude variable star , entirely due to the supergiant primary which is visually over three magnitudes (about 12x) brighter than the secondary. [ 6 ]
S Muscae is a classical (δ) Cepheid variable star in the constellation Musca about 2,600 light years away.. A light curve for S Muscae, plotted from TESS data [11]. S Muscae is a yellow supergiant ranging between spectral types F6Ib and G0Ib and magnitudes 5.89 to 6.49 over a period of 9.66 days. [3]