Article

# Magnetic flux in the internetwork quiet Sun

http://dx.doi.org/10.1051/0004-6361:200500114

ABSTRACT We report a direct comparison of the amplitudes of Stokes spectra of the Fe i 630 nm and 1.56 $\mu$m lines produced by realistic MHD simulations with simultaneous observations in the same spectral regions. The Stokes spectra were synthesized in snapshots with a mixed polarity magnetic field having a spatially averaged strength, $\langle B \rangle$, between 10 and 30 G. The distribution of Stokes $V$ amplitudes depends sensitively on $\langle B \rangle$. A quiet inter-network region was observed at the German VTT simultaneously with TIP (1.56 $\mu$m) and POLIS (630 nm). We find that the Stokes $V$ amplitudes of both infrared and visible observations are best reproduced by the simulation snapshot with $\langle B \rangle = 20$ G. In observations with 1 resolution, up to 2/3 of the magnetic flux can remain undetected.

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##### Article:The solar magnetic field
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ABSTRACT: The magnetic field of the Sun is the underlying cause of the many diverse phenomena combined under the heading of solar activity. Here we describe the magnetic field as it threads its way from the bottom of the convection zone, where it is built up by the solar dynamo, to the solar surface, where it manifests itself in the form of sunspots and faculae, and beyond into the outer solar atmosphere and, finally, into the heliosphere. On the way it, transports energy from the surface and the subsurface layers into the solar corona, where it heats the gas and accelerates the solar wind. Comment: 83 pages, 42 figures, about 2.5 MB in size
08/2010;

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### Keywords

$\langle B \rangle$\langle B \rangle$amplitudes direct comparison German VTT mixed polarity magnetic field POLIS quiet inter-network region realistic MHD simulations snapshots spatially spectral regions Stokes$V\$ amplitudes

Stokes spectra

undetected