A&A 464, 761 (2007)

DOI: 10.1051/0004-6361:20053201e

*Erratum*

(2) Preferred sunspot longitudes: non-axisymmetry and differential rotation

**I. G. Usoskin ^{1} - S. V. Berdyugina^{2,3} -
J. Poutanen^{4}**

1 - Sodankylä Geophysical Observatory (Oulu unit),
PO Box 3000, 90014 University of Oulu, Finland

2 -
Institut für Astronomie, ETH Zentrum, 8092 Zürich, Switzerland

3 -
Tuorla Observatory, University of Turku, 21500 Piikkiö, Finland

4 -
Astronomy Division, PO Box 3000,
90014 University of Oulu, Finland

(1) A&A, 405, 1121-1128 (2003), DOI:10.1051/0004-6361:20030748

(2) A&A, 441, 347-352 (2005), DOI:10.1051/0004-6361:20053201

**Key words: **Sun: activity - Sun: magnetic fields - errata, addenda

We correct three errors which appeared in these closely related papers.

- 1.
- In Paper (1), we were primarily interested in the effect
of the differential rotation rate
*B*and neglected the difference between the equatorial rotation rate*A*and the Carrington rotation rate in Eq. (5), which results in a slope in Figs. 3 and 4 that is too steep. This was corrected without comment in Paper (2) and subsequent papers. - 2.
- In Paper (2), Eq. (3) contains a typographical error, with
and
interchanged.
It should read

This correct form was used in all numerical work in that paper and all subsequent papers (e.g., Berdyugina et al. 2006, A&A, 445, 703). - 3.
- In Paper (2), the given form of Eq. (6) is incorrect.
It should read

This correct form was used in all numerical work in that and subsequent papers.

Copyright ESO 2007