A&A 464, 761 (2007)
DOI: 10.1051/0004-6361:20053201e

Erratum

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

I. G. Usoskin¹ - S. V. Berdyugina^2,3 - J. Poutanen⁴

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 $\Omega_j$ and $\Omega_{\rm C}$ interchanged. It should read

$$\Lambda_i=\Lambda_0 + T_{\rm C}\, \sum_{j=N_0}^i(\Omega_j - \Omega_{\rm C}). \nonumber$$

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

$$\epsilon_{ki}={\rm min}\left(\vert\tilde\lambda_{ki}\vert; \... ...t\,;\vert\tilde\lambda_{ki}-360^{\circ}\vert\right). \nonumber$$

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