A&A 468, 695-699 (2007)
DOI: 10.1051/0004-6361:20066854

Log-normal intensity distribution of the quiet-Sun FUV continuum observed by SUMER

J. M. Fontenla¹, W. Curdt², E. H. Avrett³, and J. Harder<sup>1

1</sup>  Laboratory for Atmospheric and Space Physics (LASP), University of Colorado, Boulder, CO 80309, USA
    e-mail: fontenla@lasp.colorado.edu
²  Max-Planck-Institut für Sonnensystemforschung (MPS), 37191 Katlenburg-Lindau, Germany
³  Harvard-Smithsonian Center for Astrophysics (CfA), 60 Garden Street, Cambridge, MA 02138, USA

(Received 1 December 2006 / Accepted 21 February 2007)

Abstract
We analyse observations of the quiet-Sun far ultraviolet (FUV) continuum at various wavelengths near 1430 Å obtained by the SUMER instrument on SOHO. According to semi-empirical atmospheric models this continuum originates from the layers in the chromosphere where the temperature rises from low values at near-radiative equilibrium to a plateau of about 6000 K. We study raster images and intensity distribution histograms and find that a single log-normal distribution matches these observations very well, and that the spatial structure observed corresponds to a mixture of features at supergranular and smaller scales that probably correspond to granular clusters. Also, a log-normal distribution was found in the literature to correspond to other chromospheric features and we compare here with histograms obtained from a H I Ly- quiet-Sun image. Because the continuum around 1430 Å is mainly produced by Si I recombination it is expected to respond well to deep chromospheric heating and not be directly affected by velocities. The data suggest that chromospheric heating originates through dissipation of magnetic free-energy fields of small size and magnitude in underlying photospheric intergranular lanes. It has been suggested that such fields can be produced by photospheric dynamos at the intergranular scale and/or by complex fields emerging in a "magnetic carpet". Such fields are expected to have sufficient free-energy to power the chromospheric heating. Plasma instabilities, such as the Farley-Buneman instability, would allow this free-energy to be dissipated in the chromosphere.

Key words: Sun: chromosphere -- Sun: magnetic fields

© ESO 2007

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