Found 4 talks width keyword solar granulation

(1) In a recently published differential analysis (see Fabbian et al) we have derived abundance corrections for iron lines, using synthetic spectra from solar magneto-convection simulations that were performed via running the Copenhagen stagger-code on massively-parallel clusters. The series of 3D snapshots used for the spectral synthesis covers 2.5 solar hours in the statistically stationary regime of the convection. Crucially, we show that the effect of magnetic fields on solar abundance determinations cannot be neglected. This is equally valid for all three different Fe abundance indicators which we have studied, though the sign of the abundance correction changes depending on the interplay of the magnetic-sensitivity of the spectral line under consideration and of temperature structure variations.
Interestingly, for two of the abundance indicators (respectively, at 608.27nm and 624.07 nm) that were used in Asplund et al's analysis and that we also included in our investigation, the presence of a magnetic field has a predominantly indirect (i.e., due to temperature changes between MHD and HD models) effect, leading to positive abundance corrections (since the final equivalent width of those Fe I lines is found to decrease with increasing magnetic flux). The direct magnetic effect due to Zeeman broadening dominates instead for the 1564.85 nm absorption line, causing for it increasingly negative abundance corrections when making the initially implanted magnetic flux larger.

(2) A new three-dimensional model of the solar photosphere is presented in this paper and made publicly available to the community. This model has the peculiarity that it has been obtained by inverting spectro-polarimetric observations, rather than from numerical radiation hydrodynamical simulations. The data used here are from the spectro-polarimeter on-board the Hinode satellite, which routinely delivers Stokes I, Q, U and V profiles in the 6302 Å spectral region with excellent quality, stability and spatial resolution (approximately 0.3''). With such spatial resolution, the major granular components are well resolved, which implies that the derived model needs no micro- or macro-turbulence to properly fit the widths of the observed spectral lines. Not only this model fits the observed data used for its construction, but it can also fit previous solar atlas observations satisfactorily.

We have discovered small whirlpools in the Sun, with a size similar to the terrestrial hurricanes (<0.5 Mm). The theory of solar convection predicts them, but they had remained elusive so far. The vortex flows are created at the downdrafts where the plasma returns to the solar interior after cooling down, and we detect them because some magnetic bright points (BPs) follow a logarithmic spiral in their way to be engulfed by a downdraft. Our disk center observations show 0.009 vortexes per Mm², with a lifetime of the order of 5 min, and with no preferred sense of rotation. They are not evenly spread out over the surface, but they seem to trace the supergranulation and the mesogranulation. These observed properties are strongly biased by our type of measurement, unable to detect vortexes except when they are engulfing magnetic BPs.