Rossby waves on the Sun as revealed by solar ‘hills’

J. R. Kuhn (), J. D. Armstrong, R. I. Bush and P. Scherrer
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J. R. Kuhn: Institute for Astronomy, University of Hawaii
J. D. Armstrong: Institute for Astronomy, University of Hawaii
R. I. Bush: Stanford University, HEPL 4085
P. Scherrer: Stanford University, HEPL 4085

Nature, 2000, vol. 405, issue 6786, 544-546

Abstract: Abstract It is a long-standing puzzle that the Sun's photosphere—its visible surface—rotates differentially, with the equatorial regions rotating faster than the poles. It has been suggested1 that waves analogous to terrestrial Rossby waves, and known as r-mode oscillations, could explain the Sun's differential rotation: Rossby waves are seen2 in the oceans as large-scale (hundreds of kilometres) variations of sea-surface height (5-cm-high waves), which propagate slowly either east or west (they could take tens of years to cross the Pacific Ocean). Calculations show that the solar r-mode oscillations have properties that should be strongly constrained by differential rotation3. Here we report the detection of 100-m-high ‘hills’ in the photosphere, spaced uniformly over the Sun's surface with a spacing of (8.7 ± 0.6) × 104 km. If convection under the photosphere is organized by the r-modes, the observed corrugated photosphere is a probable surface manifestation of these solar oscillations.

Date: 2000
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DOI: 10.1038/35014530

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