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so the sun starts helium burning as it starts the helium burning process it settles down becomes a horizontal branch star its not really stable at this point its still evolving its still moving across the hr diagram back towards the main sequence and so its still heading back towards the main sequence but the thing is we also know the lifetime of a star on the main sequence depends on the mass of the star so wed already given this equation earlier saying that the main sequence lifetime can be approximated by that equation at least for stars that are within a reasonable range for super high mass stars this equation doesnt work and for really low mass stars this equation doesnt work but for in between this equation works pretty good and so its a pretty good approximation lets so we can look at a star cluster and this is the hr diagram of a very old star cluster and remember the main sequence would look something kind of like that okay so whats happened is that the stars that w
