luminosity class

Luminosity class V is equivalent to saying on the main sequence.

Stars of luminosity class V belonged to the main sequence.

It has a spectral type of G5, while the luminosity class remains undetermined.

The luminosity class of this last component remains undetermined.

This is a white-hued, A-type star of unknown luminosity class.

They have luminosity class I and spectral class B9 or earlier.

O-type luminosity classes for subtypes earlier than O5 were not defined with standard stars until the 1970s.

Typically, a luminosity class of IV means that the star is in the subgiant stage.

A number of different luminosity classes are distinguished:

A luminosity class of III indicates that this is an evolved giant star.

It forms a pair with a star of type B9 with an unknown luminosity class separated by 0.28 arcseconds.

It is sensitive to the luminosity classes of G-K-M stars.

The luminosity class V is assigned to stars that are undergoing thermonuclear fusion of hydrogen at their core.

The luminosity class ranged from I to V, in order of decreasing luminosity.

The 'n' following the main sequence luminosity class of V indicates the absorption lines in the spectrum are broad and nebulous.

Dwarf star alone generally refers to any main-sequence star, a star of luminosity class V.

In Yerkes spectral classification their luminosity class is IV.

The luminosity class II in the Yerkes spectral classification is given to bright giants.

Subgiants are an entirely separate spectroscopic luminosity class (IV) from giants but share many features.

The luminosity class 'V' means this is a main sequence star that is generating energy through the thermonuclear fusion of hydrogen at its core.

This star has a stellar classification of G5, making it a G-type star with an undetermined luminosity class.

The luminosity class 'Iab' represents a supergiant star that has exhausted the supply of hydrogen at its core and evolved away from the main sequence.

This is surprising given the spectral luminosity classes and it could be that the interaction between the components of 24-1NE is confusing its classification.

For those stars found to have planets, high-resolution, high signal to noise ground-based spectroscopy is performed to clearly establish the spectral type and luminosity class.

This is the basis of the MK luminosity system which assigns stars to luminosity classes purely from observing their spectra.