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Studying the stars classes for my homework (school) i learned that stars are classified by the spectral types (Harvard) and luminosity class (MKK) ..

So the sun is a star class G2V

But can not understand that clasificacion (far in the future) changes to MIII when his main sequence ends and begins to burn helium

What is the relationship there? Would not it be more logical to classify stars according to their initial mass and any change that is made in the classification is related to the lifetime of the star? sub classify them according to: Fusion element: Deuterium, Hydrogen, Helium, etc. And Remaining time fusing current element?

We are glued to the story?

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  • $\begingroup$ Do you mean the luminosity class? $\endgroup$ – Py-ser Oct 17 '14 at 6:49
  • $\begingroup$ @Py-ser there are some translation issues, but yes $\endgroup$ – rnrneverdies Oct 17 '14 at 12:59
  • $\begingroup$ I am not sure to understand the question. Are you in doubt about WHY the star changes its spectral classification? $\endgroup$ – Py-ser Oct 18 '14 at 7:36
  • $\begingroup$ And how do you propose to measure the initial mass from a spectrum? $\endgroup$ – Rob Jeffries Dec 21 '14 at 22:43
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The classification of stars using spectral class is a very useful classification when considering the properties of (the atmosphere of) a star at that moment. If you consider the different stages in human development (embryo, fetus, infant, toddler, etc...), for instance, here one person also continuously changes its class. So it is not strange/uncommon/forbidden to change a classification of a thing whether it is a human or a star.

It also does not mean that other classifications are not useful. It depends on how you want to use the classification. In literature, concepts such as low-mass star, or Sun-like star are also used.

Classification according to the evolutionary stage (i.e. the type of fusion going on) of a star is also very common.

See the image below from ATNF in which you can see how stars of different zero-age main-sequence mass move along a colour-magnitude diagram. If we follow the track of a star of one solar mass then we get the following subsequent evolutionary stages:

  • MS - Main sequence stars (spectral type V) fuse hydrogen into helium in the core. When the hydrogen in the core is depleted, the star becomes an RGB star.
  • RGB - Red Giant Branch stars (V->II/III) fuse hydrogen into helium in a shell around the core while the core is inert helium. At some point (Helium flash) the core temperature becomes high enough to start fusing helium into carbon and oxygen, the star then becomes an HB star.
  • HB - Horizontal Branch stars (II/III) fuse helium into carbon/oxygen in the core. A shell with inert helium surrounds the core, which in turn is surrounded by a hydrogen burning shell.
  • AGB - Asymptotic Gian Branch stars (I) have a carbon/oxygen core with several inert or fusion shells around it.

These types (MS/RGB/HB/AGB) are classes in a very useful and common classification scheme.

In the end it just depends on what you want to do with your classification scheme.

NB. The classification of the Sun changes from G2 to M because the outer envelope and atmosphere expand enormously, causing the atmosphere to cool down. A cooler atmosphere means that the Sun changes from a yellow (6000K) to a red (4000K) star. The wavelength, and therefore colour, at which most energy is transmitted depends on the temperature of the star's atmosphere.

enter image description here

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  • $\begingroup$ Roman number is not related to the spectral type (G,M, etc), but to the luminosity class, see here: img.bhs4.com/89/9/… $\endgroup$ – Py-ser Oct 18 '14 at 7:35
  • $\begingroup$ @Py-ser Yes, I know. Though luminosity class is kind of a strange name if you consider Main Sequence stars (luminosity class V), which have absolute magnitudes from 14 to -9. ;-) $\endgroup$ – Dieudonné Oct 18 '14 at 17:36
  • $\begingroup$ Yes indeed, if only the OP would add more details to the question... $\endgroup$ – Py-ser Oct 22 '14 at 5:23

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