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The relations between chromospheric features and photospheric magnetic fields

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Abstract

High resolution photographic magnetograms are compared with Hα filtergrams (both on- and off - band) for a wide variety of solar features. It is verified that Hα filaments overlie neutral lines or bands and that Hα plages always occur at magnetic field clumps. However, the brightness of Hα plages bear no relation to magnetic field strength or polarity, and the direction of the magnetic field with respect to threads and filaments remains obscure. Counter-examples can be found for virtually every ‘rule’ that has been formulated so far.

Basic questions about the usefulness and final research goal of filtergrams and magnetograms are raised. It is shown that neither filtergram or magnetogram alone is capable of furnishing a unique solution. It is suggested that the proper direction for research is to use magnetograms, together with (as yet unspecified) additional sources of data, to understand Hα structures.

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Authors and Affiliations

  1. San Fernando Observatory, Space Physics Laboratory, Aerospace Corporation, El Segundo, Calif., U.S.A.

    Edward N. Frazier

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  1. Edward N. Frazier
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Frazier, E.N. The relations between chromospheric features and photospheric magnetic fields. Sol Phys 24, 98–112 (1972). https://doi.org/10.1007/BF00231086

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