Hostname: page-component-cd9895bd7-jkksz Total loading time: 0 Render date: 2024-12-24T19:44:24.351Z Has data issue: false hasContentIssue false
  • English
  • Français

Transport coefficients for solar and stellar dynamos

Published online by Cambridge University Press:  01 November 2006

M. Ossendrijver  and
P.J. Käpylä
M. Ossendrijver
Affiliation:
Netherlands Institute for the Near East (NINO), Witte Singel 25, 2311 BG Leiden, NL Present address: Altorientalisches Seminar, Universität Tübingen, Burgsteige 11, Schloss Hohentübingen, 72070 Tübingen; email: [email protected]
P.J. Käpylä
Affiliation:
Kiepenheuer-Institut für Sonnenphysik (KIS), Schöneckstrasse 6, 79098 Freiburg, D
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The large-scale magnetic field of the Sun and solar-type stars is probably generated near the interface of the radiative core and the convection zone. One of the well-known difficulties of interface-type and other dynamo models is to explain the latitudinal distribution of magnetic fields as observed on the Sun. In this contribution new results of numerical MHD simulations of transport coefficients of magnetic fields in the rapid rotation regime, relevant for the base of the solar convection zone, are presented that may contribute to explaining the latitudinal distribution of magnetic fields observed on the Sun. A brief outlook on further numerical simulations of transport coefficients and their relevance for mean-field dynamo theory is given.

Keywords

Sun: activitymagnetic fieldsstars: activitymagnetic fieldsMHD
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S233: Solar Activity and its Magnetic Origin , March 2006 , pp. 3 - 8
Copyright
© 2006 International Astronomical Union