The internal dynamics and magnetism of the sun -- the perspective from global helioseismology (Invited)

Details The internal dynamics and magnetism of the sun -- the perspective from global helioseismology (Invited) The internal dynamics and magnetism of the sun -- the perspective from global helioseismology (Invited)

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsh11b..04h&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #SH11B-04

Astronomy and Astrophysics

Astrophysics

[7522] Solar Physics, Astrophysics, And Astronomy / Helioseismology, [7536] Solar Physics, Astrophysics, And Astronomy / Solar Activity Cycle

Scientific paper

Helioseismology allows us to probe the interior dynamics of the Sun. Observations over the past three decades reveal the interior rotation profile, with a near-surface shear layer, differential rotation throughout the convection zone, a strong shear layer -- the tachocline -- at the base of the convection zone, and approximately uniform rotation in the radiative interior. Since the mid 1990's, continuous observations from the Global Oscillations Network Group and the Michelson Doppler Imager have allowed the study of subtle temporal variations in the rotation within the convection zone. The so-called "torsional oscillation" pattern of migrating zonal flows accompanying the surface activity migration during the solar cycle has been shown to penetrate deep within the convection zone. During the current extended solar minimum, the flow bands can be seen to migrate more slowly towards the equator than was seen in the previous minimum. There have also been (still unconfirmed) findings of shorter-term variations in the rotation rate close to the tachocline during the early years of the previous solar cycle. This review will describe the important results and give an update on the most recent observations of the interior dynamics as we await the rise of solar cycle 24.

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