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On the generation of the large-scale and turbulent magnetic fields in solar-type stars

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Abstract

It is thought that the large-scale solar-cycle magnetic field is generated in a thin region at the interface of the radiative core (RC) and solar convection zone (SCZ). We show that the bulk of the SCZ virogoursly generates a small-scale turbulent magnetic field. Rotation, while not essential, increases the generation rate of this field.

Thus, fully convective stars should have significant turbulent magnetic fields generated in their lower convection zones. In these stars the absence of a radiative core, i.e., the absence of a region of weak buoyancy, precludes the generation of a large-scale magnetic field, and as a consequence the angular momentum loss is reduced. This is, in our opinion, the explanation for the rapid rotation of the M-dwarfs in the Hyades cluster.

Adopting the Utrecht's group terminology, we argue that the residual chromospheric emission should have three distinctive components: the basal emission, the emission due to the large-scale field, and the emission due to the turbulent field, with the last component being particularly strong for low mass stars.

In the conventional dynamo equations, the dynamo frequencies and the propagation of the dynamo wave towards the equator are based on the highly questionable assumption of a constant α. Furthermore, meridional motions, a necessary consequence of the interaction of rotation with convection, are ignored. In this context we discuss Stenflo's results about the global wave pattern decomposition of the solar magnetic field and conclude that it cannot be interpreted in the framework of the conventional dynamo equations.

We discuss solar dynamo theories and argue that the surface layers could be essential for the generation of the poloidal field. If this is the case an α-effect would not be needed at the RC-SCZ interface (where the toroidal field is generated). The two central problems facing solar dynamo theories may the transport of the surface poloidal field to the RC-SCZ interface and the uncertainty about the contributions to the global magnetic field by the small-scale magnetic features.

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Authors and Affiliations

  1. Physics Department, University of Arizona, 85721, Tucson, AZ, USA

    Bernard R. Durney

  2. National Optical Astronomy Observatories, 85726, Tucson, AZ, USA

    David S. De Young

  3. Astronomy Unit, School of Mathematical Sciences, Queen Mary and Westfield College, University of London, London, U.K.

    Ian W. Roxburgh

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  1. Bernard R. Durney
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  3. Ian W. Roxburgh
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Visitor, National Solar Observatory, National Optical Astronomy Observatories.

The National Optical Astronomy Observatories are operated by the Association of Universities for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation.

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Durney, B.R., De Young, D.S. & Roxburgh, I.W. On the generation of the large-scale and turbulent magnetic fields in solar-type stars. Sol Phys 145, 207–225 (1993). https://doi.org/10.1007/BF00690652

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