A&A 394, 1117 (2002)

DOI: 10.1051/0004-6361:20021354

*Erratum*

##
Spatiotemporal fragmentation and the uncertainties

in the solar rotation law

**E. Covas**^{1} - R. Tavakol^{1} - S. Vorontsov^{1,2} - D. Moss^{3}

1 - Astronomy Unit, School of Mathematical Sciences,
Queen Mary, University of London, Mile End Road,

London E1 4NS, UK

2 - Institute of Physics of the Earth, B. Gruzinskaya 10, Moscow 123810, Russia

3 - Department of Mathematics, The University, Manchester M13 9PL, UK

A&A, 375, 260-263 (2001), DOI:10.1051/0004-6361:20010785

In this paper (and two others referenced) we stated that we fitted the dynamo
generated poloidal magnetic fields
to a vacuum exterior solution. We now realize that we instead inadvertently applied the
condition that the azimuthal component of vector potential *A*=0 at *r*=*R*,
with the consequence that the poloidal field lines do not penetrate the surface *r*=*R*.

We have since made extensive calculations with other boundary conditions on
both the poloidal and toroidal parts of the magnetic field, and
find that the results presented previously are *qualitatively
unaltered*. All the reported phenomena can be recovered, albeit at slightly different
parameter values, and the previously found robustness to changes in the
model persists.

Copyright ESO 2002