Magnetic Flux Tubes and their Relation to Continuum and Photospheric Features

  1. C. T. Russell,
  2. E. R. Priest and
  3. L. C. Lee
  1. A. Title1,
  2. T. Tarbell1,
  3. K. Topka1,
  4. D. Cauffman1,
  5. C. Balke2 and
  6. G. Scharmer3

Published Online: 21 MAR 2013

DOI: 10.1029/GM058p0171

Physics of Magnetic Flux Ropes

Physics of Magnetic Flux Ropes

How to Cite

Title, A., Tarbell, T., Topka, K., Cauffman, D., Balke, C. and Scharmer, G. (1990) Magnetic Flux Tubes and their Relation to Continuum and Photospheric Features, 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/GM058p0171

Author Information

  1. 1

    Solar and Astrophysics Laboratory, Lockheed Palo Alto Research Laboratory , Palo Alto, CA 94304, USA

  2. 2

    Utrecht Astronomical Institute, Utrecht, the Netherlands

  3. 3

    Royal Swedish Academy of Sciences, Stockholm Observatorium, S-13300, Saltsjobaden, Sweden

Publication History

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

ISBN Information

Print ISBN: 9780875900261

Online ISBN: 9781118663868

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Keywords:

  • Solar photosphere;
  • Magnetic flux;
  • Astrophysics

Summary

On 29 September, 1988, time sequences of filtergrams of the solar photosphere with high resolution (0.3 to 0.5 arc second) were obtained at the Swedish Solar Observatory (SSO) on La Palma, Canary Islands in an active region near disk center. Every 50 seconds over a 2.5 hour interval, data for a Dopplergram, magnetogram, continuum, and line center image were obtained. We report here on the relationship between photospheric bright points (“filigree”), line center brightness, and magnetic field inferred from sets of individual images and movies. In these images there is a clear difference between two classes of magnetic regions. In the first, the granulation pattern is normal, the vertical velocity field is average, and the magnetic field is largely confined in narrow lanes. In the second, the granulation pattern scale is much smaller and “abnormal” in contrast, the vertical velocity is lower, and the magnetic field is relatively less compact. In the locales where the granulation is normal, there is excellent spatial correlation between bright continuum, line center, and the magnetic field fine structure. In the regions of abnormal granulation, the correspondence between bright structures and magnetic field is much more complex.