  As the most abundant element in the universe after hydrogen and helium,
oxygen plays a key role in planetary, stellar, and galactic astrophysics. Its
abundance is especially influential on stellar structure and evolution, and as
the dominant opacity contributor at the base of the Sun's convection zone it is
central to the discussion around the solar modelling problem. However,
abundance analyses require complete and reliable sets of atomic data. We
present extensive atomic data for O I, by using the multiconfiguration
Dirac-Hartree-Fock and relativistic configuration interaction methods.
Lifetimes and transition probabilities for radiative electric dipole
transitions are given and compared with results from previous calculations and
available measurements. The accuracy of the computed transition rates is
evaluated by the differences between the transition rates in Babushkin and
Coulomb gauges, as well as by a cancellation factor analysis. Out of the 989
computed transitions in this work, 205 are assigned to the accuracy classes
AA-B, that is, with uncertainties less than 10%, following the criteria defined
by the National Institute of Standards and Technology Atomic Spectra Database.
We discuss the influence of the new log(gf) values on the solar oxygen
abundance and ultimately advocate $\log\epsilon_{\mathrm{O}}=8.70\pm0.04$.
