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Magnetic knots near a sunspot

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Abstract

Observations of longitudinal and transversal fields and of radial velocities in the magnetic ‘knots’ close to a sunspot were made with the help of Sayan Observatory magnetograph with spatial resolution 1″.2 x 1″.8.

The analysis led to following conclusions:

  1. (1)

    The magnetic field in the knots is mainly vertical. The mean inclination of the magnetic-field vector to the vertical direction is equal to 26°.

  2. (2)

    The phenomenon of darkening is connected with essentially vertical fields and brightening in the faculae with the horizontal fields on the sun.

  3. (3)

    An inverse relation between the value of darkening and the inclination of the field vector to the vertical direction and a direct relation on the longitudinal magnetic-field strength exist for the magnetic knots.

  4. (4)

    The magnetic knots in the active region are located in the Hα flocculi near the line where the radial velocity is changing sign in the photosphere.

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References

  • Beckers, J. M. and Schröter, E. H.: 1967, in Structure and Development of Solar Active Regions (IAU Symposium no. 35, Budapest, September 1967, ed. by K. O. Kiepenheuer), Reidel, Dordrecht, p. 178.

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Authors and Affiliations

  1. Siberian Institute of Terrestrial Magnetism, Ionosphere and Radio Propagation, the U.S.S.R. Academy of Sciences, Irkutsk

    V. M. Grigorjev

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  1. V. M. Grigorjev
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Grigorjev, V.M. Magnetic knots near a sunspot. Sol Phys 6, 67–71 (1969). https://doi.org/10.1007/BF00146796

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  • DOI: https://doi.org/10.1007/BF00146796

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