  Stellar structure and evolution theory is one of the basis in modern
astronomy. Stellar inner structures and their evolutionary states can be
precisely tested by asteroseismology, since the inner information is brought to
the stellar surface by the global oscillating waves and becomes observable. For
stellar evolutionary speed (i.e. how long time scale does a star stay at a
special evolution phase?), because of the insurmountable gap between the time
scales of the evolutionary history of human civilization and a star, it can
only be roughly tested by ensemble of stars in different evolutionary stages in
most cases, and all the snapshots of these stars make up our global view of
stellar evolution. The effect of stellar evolution on the structure and the
corresponding global size of a pulsating star will lead to tiny period
variations of its pulsation modes, which are the most valuable indicators of
its evolutionary state and can be used to test the stellar evolution theory by
a single star rather than ensemble of stars. Here, we report a High-Amplitude
$\delta$ Scuti star AE Ursae Majoris, who locates in the post main-sequence
(MS) evolutionary stage and its observed linear period variation rate can be
practically ascribed to its evolutionary effect. The result tests the stellar
evolution theory from the pre-MS to post-MS with an unprecedented precision by
a single star, and the framework can be extended to other type of pulsating
stars to perform precise evolutionary asteroseismology, which aims to test the
current stellar evolution theory in different evolutionary stages, discover the
discrepancies between the theory and observations, and ultimately build a
complete and precise stellar evolution theory to backtrack the history of each
of these stars.
