Hostname: page-component-78c5997874-94fs2 Total loading time: 0 Render date: 2024-11-13T09:54:44.819Z Has data issue: false hasContentIssue false
  • English
  • Français

Wave Propagation in the Magnetic Network on the Sun

Published online by Cambridge University Press:  01 November 2006

S. S. Hasan ,
G. Vigeesh  and
A. A. van Ballegooijen
S. S. Hasan
Affiliation:
Indian Institute of Astrophysics, Bangalore, India, email: hasan@iiap.res.in
G. Vigeesh
Affiliation:
Indian Institute of Astrophysics, Bangalore, India, email: hasan@iiap.res.in
A. A. van Ballegooijen
Affiliation:
Harvard-Smithsonian Centre for Astrophysics, Cambridge MA, U.S.A
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.

Hasan et al. (2005) have recently presented 2-D dynamical calculations on wave propagation in in the magnetic network of the Sun. The latter is idealized as consisting of non-potential flux tubes in the quiet solar chromosphere. It is of interest to understand how the nature of wave propagation is influenced by the choice of initial equilibrium configuration of the magnetic field. We examine this by comparing the earlier calculations with those when the network is modelled as a potential structure. Our calculations demonstrate that the nature of the wave propagation is significantly different, particularly the transport of energy which for the potential case, occurs more isotropically than for the non-potential configuration.

Keywords

Sun: magnetic fields - magnetohydrodynamics (MHD) - Sun: photosphere - oscillations
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S233: Solar Activity and its Magnetic Origin , March 2006 , pp. 116 - 117
Copyright
© 2006 International Astronomical Union