Hostname: page-component-78c5997874-s2hrs Total loading time: 0 Render date: 2024-11-11T04:02:28.636Z Has data issue: false hasContentIssue false
  • English
  • Français

Magnetic flux emergence into the atmosphere

Published online by Cambridge University Press:  01 November 2006

F. Moreno-Insertis
F. Moreno-Insertis
Affiliation:
Instituto de Astrofisica de Canarias, 38200 La Laguna (Tenerife), Spain email: fmi@ll.iac.es Dept of Astrophysics, Univ of La Laguna, Tenerife, Spain
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.

Understanding the mechanism that causes the emergence of magnetic flux from the solar interior to the atmosphere, the drastic changes in the properties of the matter and magnetic fields along the rise and the interplay of dynamic and resistive phenomena that shape the emerged regions is one of the major open tasks in solar physics. Important advances are being made both in the theoretical modelling and in the observation of the emergence events. This review concentrates on recent advances through 3D numerical experiments carried out with massively parallel MHD and radiative transfer codes.

Keywords

Sun:activitySun: magnetic fieldsSun:coronaSun:photospheremethods: numericalplasmasMHDradiative transfer
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S233: Solar Activity and its Magnetic Origin , March 2006 , pp. 33 - 40
Copyright
© 2006 International Astronomical Union