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The white dwarf luminosity function is an important tool to understand theproperties of the Solar neighborhood, like its star formation history, and itsage. Here we present a population synthesis study of the white dwarf populationwithin 40~pc from the Sun, and compare the results of this study with theproperties of the observed sample. We use a state-of-the-art populationsynthesis code based on Monte Carlo techniques, that incorporates the mostrecent and reliable white dwarf cooling sequences, an accurate description ofthe Galactic neighborhood, and a realistic treatment of all the knownobservational biases and selection procedures. We find a good agreement betweenour theoretical models and the observed data. In particular, our simulationsreproduce a previously unexplained feature of the bright branch of the whitedwarf luminosity function, which we argue is due to a recent episode of starformation. We also derive the age of the Solar neighborhood employing theposition of the observed cut-off of the white dwarf luminosity function,obtaining ~8.9+-0.2 Gyr. We conclude that a detailed description of theensemble properties of the population of white dwarfs within 40pc of the Sunallows us to obtain interesting constraints on the history of the Solarneighborhood.

The white dwarf population within 40 pc of the Sun