The solar photospheric abundance of phosphorus:: results from CO5BOLD 3D model atmospheres

Aims. We determine the solar abundance of phosphorus using (COBOLD)-B-5 3D hydrodynamic model atmospheres. Methods. High-resolution, high signal-to-noise solar spectra of the P I lines of Multiplet 1 at 1051-1068 nm are compared to line-formation computations performed on a (COBOLD)-B-5 solar model atmosphere. Results. We find A(P) = 5.46 +/- 0.04, in good agreement with previous analyses based on 1D model atmospheres, due to the P I lines of Mult. 1 not being affected much by 3D e. ects. We cannot confirm an earlier claim by other authors of a downward revision of the solar P abundance by 0.1 dex when employing a 3D model atmosphere. Concerning other stars, we find modest (< 0.1 dex) 3D abundance corrections for P among four F-dwarf model atmospheres of different metallicities, and these corrections are largest at lowest metallicity. Conclusions. We conclude that 3D abundance corrections are generally rather small for the P I lines studied in this work. They are marginally relevant for metal-poor stars, but may be neglected in the Sun.