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Observations of moving magnetic features near sunspots

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Abstract

The properties of small (< 2″) moving magnetic features near certain sunspots are studied with several time series of longitudinal magnetograms and Hα filtergrams. We find that the moving magnetic features:

  1. (1)

    Are associated only with decaying sunspots surrounded entirely or in part by a zone without a permanent vertical magnetic field.

  2. (2)

    Appear first at or slightly beyond the outer edge of the parent sunspot regardless of the presence or absence of a penumbra.

  3. (3)

    Move approximately radially outward from sunspots at about 1 km s−1 until they vanish or reach the network.

  4. (4)

    Appear with both magnetic polarities from sunspots of single polarities but appear with a net flux of the same sign as the parent sunspot.

  5. (5)

    Transport net flux away from the parent sunspots at the same rates as the flux decay of the sunspots.

  6. (6)

    Tend to appear in opposite polarity pairs.

  7. (7)

    Appear to carry a total flux away from sunspots several times larger than the total flux of the sunspots.

  8. (8)

    Produce only a very faint emmission in the core of Hα.

A model to help understand the observations is proposed.

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Authors and Affiliations

  1. Lockheed Solar Observatory, Saugus, Calif., U.S.A.

    K. Harvey

  2. Kitt Peak National Observatory, Tucson, Ariz., U.S.A.

    J. Harvey

Authors
  1. K. Harvey
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  2. J. Harvey
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Visiting Astronomer, Solar Division, Kitt Peak National Observatory.

Operated by the Association of Universities for Research in Astronomy, Inc., under contract with the National Science Foundation.

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Harvey, K., Harvey, J. Observations of moving magnetic features near sunspots. Sol Phys 28, 61–71 (1973). https://doi.org/10.1007/BF00152912

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  • DOI: https://doi.org/10.1007/BF00152912

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