  We provide a status report on the determination of stellar ages from
asteroseismology for stars of various masses and evolutionary stages. The
ability to deduce the ages of stars with a relative precision of typically 10
to 20% is a unique opportunity for stellar evolution and also of great value
for both galactic and exoplanet studies. Further, a major uncalibrated
ingredient that makes stellar evolution models uncertain, is the stellar
interior rotation frequency $\Omega(r)$ and its evolution during stellar life.
We summarize the recent achievements in the derivation of $\Omega(r)$ for
different types stars, offering stringent observational constraints on
theoretical models. Core-to-envelope rotation rates during the red giant stage
are far lower than theoretical predictions, pointing towards the need to
include new physical ingredients that allow strong and efficient coupling
between the core and the envelope in the models of low-mass stars in the
evolutionary phase prior to the core helium burning. Stars are subject to
efficient mixing phenomena, even at low rotation rates. Young massive stars
with seismically determined interior rotation frequency reveal low
core-to-envelope rotation values.
