Subgiant

Eventually, perhaps 10 or 100 million years from now, subgiant stars like HD 200964 and 24 ❋ Unknown (2010)

Algol B (Beta Persei B) is a orange-red subgiant star of spectral class K0-2 IV. ❋ BMcP (2010)

As a subgiant, the star is also 3.4 times as luminous as our Sun. ❋ BMcP (2010)

The paradox is a result of Algol A being more massive star of the binary pair, yet still a main sequence star, while the less massive Algol B has already reached the subgiant stage in its evolution. ❋ BMcP (2010)

The close binary Algol system contains a radio-bright KIV subgiant star in a very close (0.062 astronomical units) and rapid (2.86 day) orbit with a main sequence B8 star. ❋ Unknown (2010)

Here we report multi-epoch radio imaging of the Algol system, in which we see a large, persistent coronal loop approximately one subgiant diameter in height, whose base is straddling the subgiant and whose apex is oriented towards the B8 star. ❋ Unknown (2010)

A large body of evidence points to the existence of an extended, complex coronal magnetosphere originating at the cooler K subgiant ❋ W. M. Peterson (2010)

These distances (with errors of 0.05 mag) will be used to determine the ages of globular clusters using the luminosity of the subgiant branch as an age indicator. ❋ Unknown (2009)

As Delta Pavonis is usually bright for its spectral type, it is suspected that the star is beginning to evolve off the main sequence on its way to becoming a subgiant star as it starts to fuse more and more helium at its core. ❋ Unknown (2009)

51 Pegasi is a yellow-orange main sequence star of spectral class of G4-5 Va, although it has been previously classified as G2IV-V (meaning either a dwarf or a subgiant). ❋ Unknown (2009)