Bibcode
DOI
Sánchez Almeida, J.; Emonet, T.; Cattaneo, F.
Bibliographical reference
The Astrophysical Journal, Volume 585, Issue 1, pp. 536-552.
Advertised on:
3
2003
Journal
Citations
57
Refereed citations
44
Description
We employ the magnetic and velocity fields from turbulent dynamo
simulations to synthesize the polarization of a typical photospheric
line. The synthetic Stokes profiles have properties in common with those
observed in the quiet Sun. The simulated magnetograms present a level of
signal similar to that of the Inter-Network regions. Asymmetric Stokes V
profiles with two, three, and more lobes appear in a natural way. The
intensity profiles are broadened by the magnetic fields in fair
agreement with observational limits. Furthermore, the Hanle
depolarization signals of the Sr I λ4607 Å line turn out to
be within the solar values. Differences between synthetic and observed
polarized spectra can also be found. There is a shortage of Stokes V
asymmetries, which we attribute to a deficit of structuring in the
magnetic and velocity fields from the simulations as compared to the
Sun. This deficit may reflect the fact that the Reynolds numbers of the
numerical data are still far from solar values. We consider the
possibility that intense and tangled magnetic fields, like those in the
simulations, exist in the Sun. This scenario has several important
consequences. For example, less than 10% of the existing unsigned
magnetic flux would be detected in present magnetograms. The existing
flux would exceed by far that carried by active regions during the
maximum of the solar cycle. Detecting these magnetic fields would
involve improving the angular resolution, the techniques to interpret
the polarization signals, and to a lesser extent, the polarimetric
sensitivity.