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Comparison of the mean photospheric magnetic field and the interplanetary magnetic field

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Abstract

The mean photospheric magnetic field of the sun seen as a star has been compared with the interplanetary magnetic field observed with spacecraft near the earth. Each change in polarity of the mean solar field is followed about 4 1/2 days later by a change in polarity of the interplanetary field (sector boundary). The scaling of the field magnitude from sun to near earth is within a factor of two of the theoretical value, indicating that large areas on the sun have the same predominant polarity as that of the interplanetary sector pattern. An independent determination of the zero level of the solar magnetograph has yielded a value of 0.1±0.05 G. An effect attributed to a delay of approximately one solar rotation between the appearance of a new photospheric magnetic feature and the resulting change in the interplanetary field is observed.

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Authors and Affiliations

  1. Crimean Astrophysical Observatory, Nauchny, Crimea, U.S.S.R.

    A. Severny

  2. Space Sciences Laboratory, University of California, Berkeley, Calif., U.S.A.

    J. M. Wilcox & P. H. Scherrer

  3. NASA Ames Research Center, Moffett Field, Calif., U.S.A.

    D. S. Colburn

Authors
  1. A. Severny
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  2. J. M. Wilcox
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  3. P. H. Scherrer
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  4. D. S. Colburn
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Severny, A., Wilcox, J.M., Scherrer, P.H. et al. Comparison of the mean photospheric magnetic field and the interplanetary magnetic field. Sol Phys 15, 3–14 (1970). https://doi.org/10.1007/BF00149468

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  • DOI: https://doi.org/10.1007/BF00149468

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