Volume 577, May 2015
|Number of page(s)||8|
|Published online||24 April 2015|
The solar oxygen abundance from an empirical three-dimensional model⋆
Instituto de Astrofísica de Canarias,
Avda vía Láctea S/N, 38200
2 Departamento de Astrofísica, Universidad de La Laguna, 38205, La Laguna, Tenerife, Spain
Received: 24 September 2014
Accepted: 5 February 2015
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.
Key words: Sun: abundances / Sun: atmosphere / Sun: granulation / Sun: photosphere / stars: abundances / stars: atmospheres
As with the earlier version, the new 3D model is publicly available and may be downloaded from the CDS via anonymous ftp to cdsarc.u-strasbg.fr (18.104.22.168) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/577/A25
© ESO, 2015
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