A new view of quiet-Sun topology from Hinode/SOT

Free access article

Issue		A&A Volume 484, Number 3, June IV 2008


Page(s)		L47 - L50
Section		Letters
DOI		http://dx.doi.org/10.1051/0004-6361:200809826
Published online		15 May 2008

A&A 484, L47-L50 (2008)
DOI: 10.1051/0004-6361:200809826

Letter

A new view of quiet-Sun topology from Hinode/SOT

S. Régnier, C. E. Parnell, and A. L. Haynes

School of Mathematics and Statistics, University of St Andrews, St Andrews, Fife KY16 9SS, Scotland, UK
e-mail: stephane@mcs.st-andrews.ac.uk

Received 21 March 2008 / Accepted 8 May 2008

Abstract
Context. With the recent launch of the Hinode satellite our view of the nature and evolution of quiet-Sun regions has been improved. In light of the new high resolution observations, we revisit the study of the quiet Sun's topological nature.
Aims. Topology is a tool to explain the complexity of the magnetic field, the occurrence of reconnection processes, and the heating of the corona. This Letter aims to give new insights to these different topics.
Methods. Using a high-resolution Hinode/SOT observation of the line-of-sight magnetic field on the photosphere, we calculate the three dimensional magnetic field in the region above assuming a potential field. From the 3D field, we determine the existence of null points in the magnetic configuration.
Results. From this model of a continuous field, we find that the distribution of null points with height is significantly different from that reported in previous studies. In particular, the null points are mainly located above the bottom boundary layer in the photosphere (54%) and in the chromosphere (44%) with only a few null points in the corona (2%). The density of null points (expressed as the ratio of the number of null points to the number of photospheric magnetic fragments) in the solar atmosphere is estimated to be between 3% and 8% depending on the method used to identify the number of magnetic fragments in the observed photosphere.
Conclusions. This study reveals that the heating of the corona by magnetic reconnection at coronal null points is unlikely. Our findings do not rule out the heating of the corona at other topological features. We also report the topological complexity of the chromosphere as strongly suggested by recent observations from Hinode/SOT.

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

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