The elementary theory of twisted flux tubes. I - Equilibrium configurations

Wilson, P.R.

doi:10.1086/155286

Cited by 14 publications

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“…Higher orders in the radial expansion procedure which to zeroth order gives the slender fluxtube approximation (cf. Roberts and Webb, 1978;Ferriz-Mas and Schüssler, 1989) and allow to include twisted fields have been considered by Wilson (1977), Browning and Priest (1983) and Pneuman et al (1986). The similarity approach was used by Osherovich et al (1983) and Solov'ev (1984).…”

Section: Magnetic Fieldmentioning

confidence: 99%

Theoretical Aspects of Small-Scale Photospheric Magnetic Fields

Schüßler

1990

Symp. - Int. Astron. Union

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The state of theoretical description of small-scale concentrated magnetic fields in the solar photosphere (excluding oscillations and wave propagation) is reviewed with emphasis on work done since 1982. The processes which probably lead to the formation of strong fields (flux expulsion, convective collapse) are discussed in some detail and the present understanding of the subsequent (quasi-)equilibrium state is summarized. We consider in particular the magnetic and thermal structure of the basic magnetic flux concentrations (magnetic elements) and stress the importance of radiative transfer effects, e.g. the horizontal heat exchange with the surroundings and the effect of radiation from the hot bottom and walls on the upper layers. Velocity fields within and around magnetic flux concentrations are discussed with emphasis on shift and asymmetry of the observed Stokes V-profiles which have recently been understood in terms of a downflow in the immediate vicinity outside magnetic structures. Reconnection and instabilities are considered as possible destruction processes for magnetic elements.

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Section: Magnetic Fieldmentioning

confidence: 99%

Theoretical Aspects of Small-Scale Photospheric Magnetic Fields

Schüßler

1990

Symp. - Int. Astron. Union

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“…Observations also indicate that emerging flux loops exhibit some degree of twisting and, although the effect may not be quite so dominant as Piddington suggests, it is important to take it into account. The following parametric model permits the study of the effect of twist and of tapering on the configuration of the flux tube (Wilson 1977…”

Section: Standard Modelsmentioning

confidence: 99%

Structure within a Magnetic Flux Tube

Wilson

1978

Publ. Astron. Soc. Aust.

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Since their initial discovery by Hale, the nature of solar magnetic fields has presented us with a number of problems. At one time it was thought that the field consisted of a weak background dipole field of order 1-2 G on which was superimposed the considerably more intense fields associated with active regions and sunspots. However, more recent observational studies by Harvey, Frasier, Stenflo and others have suggested that 90% of the background field appears in the form of intense small-scale fields with intensities of order 103 gauss or greater and which have remarkably similar properties whether they occur in active or quiet regions. In particular, the field intensity appears independent of the total amount of flux present but the appearance of the structure depends critically on the total flux.

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Theoretical Aspects Of Small-Scale Photospheric Magnetic Fields

Schüßler

1990

Solar Photosphere: Structure, Convection, and Magnetic Fields

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The elementary theory of twisted flux tubes. I - Equilibrium configurations

Cited by 14 publications

References 0 publications

Theoretical Aspects of Small-Scale Photospheric Magnetic Fields

Theoretical Aspects of Small-Scale Photospheric Magnetic Fields

Structure within a Magnetic Flux Tube

Theoretical Aspects Of Small-Scale Photospheric Magnetic Fields

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