This article has an erratum: [erratum]
Volume 441, Number 1, October I 2005
|Page(s)||347 - 352|
|Published online||13 September 2005|
Preferred sunspot longitudes: non-axisymmetry and differential rotation
Sodankylä Geophysical Observatory (Oulu unit), 90014 University of Oulu, Finland e-mail: firstname.lastname@example.org
2 Astronomy Division, PO Box 3000, 90014 University of Oulu, Finland e-mail: email@example.com
3 Institut für Astronomie, ETHZ, 8092 Zürich, Switzerland e-mail: firstname.lastname@example.org
Accepted: 15 June 2005
As recently found, the distribution of sunspots is non-axisymmetric and spot group formation implies the existence of two persistent active longitudes separated by 180°. Here we quantitatively study the non-axisymmetry of sunspot occurrence. In a dynamic reference frame inferred from the differential rotation law, the raw sunspot data show a clear clustering around the persistent active longitudes. The differential rotation describing the dynamic frame is quantified in terms of the equatorial angular velocity and the differential rotation rate, which appear to be significantly different from those for individual sunspots. This implies that the active longitudes are not linked to the depth of sunspot anchoring. In order to quantify the observed effect, we introduce a measure of the non-axisymmetry of the sunspot distribution. The non-axisymmetric component is found to be highly significant, and the ratio of its strength to that of the axisymmetric one is roughly 1:10. This provides additional constraints for solar dynamo models.
Key words: Sun: activity / Sun: magnetic fields / Sun: sunspots
© ESO, 2005
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