Solar Physics

, Volume 26, Issue 2, pp 283–289

Large-scale photospheric magnetic field: The diffusion of active region fields

  • Kenneth H. Schatten
  • Robert B. Leighton
  • Robert Howard
  • John M. Wilcox

DOI: 10.1007/BF00165269

Cite this article as:
Schatten, K.H., Leighton, R.B., Howard, R. et al. Sol Phys (1972) 26: 283. doi:10.1007/BF00165269


The large-scale photospheric magnetic field has been computed by allowing observed active region fields to diffuse and to be sheared by differential rotation in accordance with the Leighton (1969) magnetokinematic model of the solar cycle. The differential rotation of the computed field patterns as determined by autocorrelation curves is similar to that of the observed photospheric field, and poleward of 20° latitude both are significantly different from the differential rotation of the long-lived sunspots (Newton and Nunn, 1951) used as an input into the computations.

Copyright information

© D. Reidel Publishing Company 1972

Authors and Affiliations

  • Kenneth H. Schatten
    • 1
  • Robert B. Leighton
    • 2
  • Robert Howard
    • 3
  • John M. Wilcox
    • 4
  1. 1.Laboratory for Extraterrestrial Physics, NASA Goddard Space Flight CenterGreenbeltU.S.A.
  2. 2.Physics DepartmentCalifornia Institute of TechnologyPasadenaU.S.A.
  3. 3.Hale Observatories, Carnegie Institute of Washington, California Institute of TechnologyPasadenaU.S.A.
  4. 4.Institute for Plasma Research, Stanford UniversityStanfordU.S.A.