Caption: A Hertzsprung-Russell (HR) diagram showing a representative sample post-main-sequence evolutionary tracks for single stars of various initial stellar masses, all with initial fiducial solar metallicity Z=0.02 and zero angular momentum.
Note the following HR diagram bands:
The evolutionary tracks leave the main sequence mostly moving toward the upper right half of the HR diagram.
So post-main-sequence stars are typically cooler and, except at the high-mass end, brighter than than main-sequence stars.
In understanding stellar evolution, you should always remember the main-sequence rule (local link / general link: star_main_sequence_rule.html).
EOF
php require("/home/jeffery/public_html/astro/star/star_main_sequence_rule.html");?>
For further understanding of
post-main-sequence evolution,
see
Post-main-sequence evolution keywords
below
(local link /
general link: post_main_sequence_keywords.html):
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