Dynamical Effects and Energy Transport in Intense Flux Tubes

  1. C. T. Russell,
  2. E. R. Priest and
  3. L. C. Lee
  1. S. S. Hasan

Published Online: 21 MAR 2013

DOI: 10.1029/GM058p0157

Physics of Magnetic Flux Ropes

Physics of Magnetic Flux Ropes

How to Cite

Hasan, S. S. (1990) Dynamical Effects and Energy Transport in Intense Flux Tubes, in Physics of Magnetic Flux Ropes (eds C. T. Russell, E. R. Priest and L. C. Lee), American Geophysical Union, Washington, D. C.. doi: 10.1029/GM058p0157

Author Information

  1. Indian Institute of Astrophysics, Bangalore 560034, India

Publication History

  1. Published Online: 21 MAR 2013
  2. Published Print: 1 JAN 1990

ISBN Information

Print ISBN: 9780875900261

Online ISBN: 9781118663868



  • Solar photosphere;
  • Magnetic flux;
  • Astrophysics


The aim of the present analysis is to provide a realistic model for conditions within intense flux tubes. In a previous examination, it was demonstrated that convective collapse is a feasible mechanism for generating kilogauss fields in the photosphere. An important finding to emerge was that the final state of convective collapse is not steady, but oscillatory. In the presence of horizontal heat exchange, overstable oscillations occur. The calculations have now been refined to treat radiative transport in the Eddington approximation and also to allow for convective energy transport within the flux tube. An equilibrium atmosphere in the tube, corresponding to a specified value of β00 = 8πp 00 2) at the top of the tube, is first constructed. This equilibrium is perturbed, by introducing a small downflow, and the subsequent time evolution of the tube is followed. Although oscillatory behaviour is again observed, the nature of the oscillations is different. The flow does not appear to have a simple sinusoidal behaviour, as found earlier, but a fairly complicated one. The uplow and downflow phases do not appear to be symmetric. An important finding is that vertical energy transport through radiation is very important, particularly close to continuum optical depth unity. The observational implications of the calculations are pointed out. A comparison with semi-empirical models shows reasonable agreement.