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Solar Magnetoconvection and Small-Scale Dynamo

Recent Developments in Observation and Simulation

Abstract

A number of observational and theoretical aspects of solar magnetoconvection are considered in this review. We discuss recent developments in our understanding of the small-scale structure of the magnetic field on the solar surface and its interaction with convective flows, which is at the centre of current research. Topics range from plage areas in active regions over the magnetic network shaped by supergranulation to the ubiquituous ‘turbulent’ internetwork fields. On the theoretical side, we focus upon magnetic field generation by small-scale dynamo action.

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Notes

  1. 1.

    This number should be considered as a lower threshold as sometimes it is not easy to distinguish between strong isolated IN fields and the network.

  2. 2.

    The noise level \(\sigma\) is given in units of the continuum intensity spatially averaged over the quiet Sun.

  3. 3.

    The line-ratio technique measures the ratio s of the amplitudes in the circular polarization signals in two different spectral lines. Under the assumption that both lines possess the same opacity and provided that the magnetic field is weak, then s is equal to the quotient of their Landé factors.

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Acknowledgements

This work was partially supported by the BK21 plus program through the National Research Foundation (NRF) funded by the Ministry of Education of Korea.

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Borrero, J.M., Jafarzadeh, S., Schüssler, M. et al. Solar Magnetoconvection and Small-Scale Dynamo. Space Sci Rev 210, 275–316 (2017). https://doi.org/10.1007/s11214-015-0204-5

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Keywords

  • Sun
  • Convection
  • Magnetic field