English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We have developed a high-precision code which solves the kinematic dynamoproblem both for given rotation law and meridional flow in the case of a loweddy diffusivity of the order of $10^{11}$ cm$^2$/s known from the sunspotdecay. All our models work with an \alf-effect which is positive (negative) inthe northern (southern) hemisphere. It is concentrated in radial layers locatedeither at the top or at the bottom of the convection zone. We have alsoconsidered an \alf-effect uniformly distributed in all the convection zone. Inthe present paper the main attention is focused on i) the parity of thesolution, ii) the form of the butterfly diagram and iii) the phase relation ofthe resulting field components. If the helioseismologically derived internalsolar rotation law is considered, a model without meridional flow of highmagnetic Reynolds number (corresponding to low eddy diffusivity) fails in allthe three issues in comparison with the observations. However, a meridionalflow with equatorial drift at the bottom of the convection zone of few metersby second can indeed enforce the equatorward migration of the toroidal magneticfield belts similar to the observed butterfly diagram but, the solution hasonly a dipolar parity if the (positive) \alf-effect is located at the base ofthe convection zone rather than at the top. We can, therefore, confirm the mainresults of a similar study by Dikpati & Gilman (2001).Comment: 9 pages, 16 figures, to appear on Astronomy and Astrophysic

Parity properties of an advection-dominated solar $\mathsf{\alpha^2 \Omega}$-dy na mo