The solar oxygen abundance from an empirical three-dimensional model^⋆

¹ Instituto de Astrofísica de Canarias, Avda vía Láctea S/N, 38200 La Laguna, Tenerife Spain
e-mail: hsocas@iac.es
² Departamento de Astrofísica, Universidad de La Laguna, 38205, La Laguna, Tenerife, Spain

Received: 24 September 2014
Accepted: 5 February 2015

Abstract

The oxygen abundance in the solar photosphere, and consequently the solar metallicity itself, is still a controversial question with far-reaching implications in many areas of astrophysics. This paper presents a new determination obtained by fitting the forbidden O i line at 6300 Å with an observational 3D model. The approach presented here is novel because previous determinations were based either on 1D empirical stratifications or on 3D theoretical models. The resulting best-fit abundances are log ϵ(O) = 8.90 and log ϵ(Ni) = 6.15. Nevertheless, by introducing minor tweaks in the model and the procedure, it is possible to retrieve very different values, even down to log ϵ(O) = 8.70. This extreme sensitivity of the abundance to possible systematic effects is not specific to this particular work, but probably reflects the real uncertainty inherent to all abundance determinations based on a prescribed model atmosphere.