Skip to main content Accessibility help
×
Home

Turbulent Transport of Magnetic Fields and the Solar Dynamo

  • L.L. Kichatinov (a1)

Abstract

The effect of anisotropic transport of the mean magnetic field by turbulence in a stratified rotating fluid is briefly discussed to find its qualitative correspondence to the observed field redistribution over a solar cycle. A kinematic model of a dynamo in a spherical shell is developed with the transport effect included to assess its importance in a more consistent way. The anisotropic transport brings the simulated field behavior closer to that observed on the Sun.

    • Send article to Kindle

      To send this article to your Kindle, first ensure no-reply@cambridge.org is added to your Approved Personal Document E-mail List under your Personal Document Settings on the Manage Your Content and Devices page of your Amazon account. Then enter the ‘name’ part of your Kindle email address below. Find out more about sending to your Kindle. Find out more about sending to your Kindle.

      Note you can select to send to either the @free.kindle.com or @kindle.com variations. ‘@free.kindle.com’ emails are free but can only be sent to your device when it is connected to wi-fi. ‘@kindle.com’ emails can be delivered even when you are not connected to wi-fi, but note that service fees apply.

      Find out more about the Kindle Personal Document Service.

      Turbulent Transport of Magnetic Fields and the Solar Dynamo
      Available formats
      ×

      Send article to Dropbox

      To send this article to your Dropbox account, please select one or more formats and confirm that you agree to abide by our usage policies. If this is the first time you use this feature, you will be asked to authorise Cambridge Core to connect with your <service> account. Find out more about sending content to Dropbox.

      Turbulent Transport of Magnetic Fields and the Solar Dynamo
      Available formats
      ×

      Send article to Google Drive

      To send this article to your Google Drive account, please select one or more formats and confirm that you agree to abide by our usage policies. If this is the first time you use this feature, you will be asked to authorise Cambridge Core to connect with your <service> account. Find out more about sending content to Google Drive.

      Turbulent Transport of Magnetic Fields and the Solar Dynamo
      Available formats
      ×

Copyright

References

Hide All
Durney, B.R. and Latour, J: 1978, Geophys. Astrophas. Fluid Dyn. 9, 241
Kichatinov, L.L.: 1988, Astron. Nachr. 309, 197
Kichatinov, L.L.: 1991, Astron. Astrophys. 243, 483
Libbrecht, K.G.: 1989, Astrophys. J. 336, 1092
Spitzer, L.: 1957, Astrophys. J. 125, 525
Stenflo, J.O.: 1988, Astrophys. Space Sci. 144, 321
Zeldovich, Ya.B.: 1957, Sov. Phys. JETP 4, 460

Turbulent Transport of Magnetic Fields and the Solar Dynamo

  • L.L. Kichatinov (a1)

Metrics

Full text views

Total number of HTML views: 0
Total number of PDF views: 0 *
Loading metrics...

Abstract views

Total abstract views: 0 *
Loading metrics...

* Views captured on Cambridge Core between <date>. This data will be updated every 24 hours.

Usage data cannot currently be displayed