  Most of low- and intermediate-mass stars that populate the Universe will end
their lives as white dwarf stars. These ancient stellar remnants have encrypted
inside a precious record of the evolutionary history of the progenitor stars,
providing a wealth of information about the evolution of stars, star formation,
and the age of a variety of stellar populations, such as our Galaxy and open
and globular clusters. While some information like surface chemical
composition, temperature and gravity of white dwarfs can be inferred from
spectroscopy, the internal structure of these compact stars can be unveiled
only by means of asteroseismology, an approach based on the comparison between
the observed pulsation periods of variable stars and the periods of appropriate
theoretical models. In this communication, we first briefly describe the
physical properties of white dwarf stars and the various families of pulsating
white dwarfs known up to the present day, and then we present two recent
analysis carried out by the La Plata Stellar Evolution and Pulsation Group in
this active field of research.
