Helioseismic constraints on the gradient of angular velocity at the base of the solar convection zone

Research output: Contribution to journalArticlepeer-review

133 Scopus citations

Abstract

The layer of transition from the nearly rigid rotation of the radiative interior to the latitudinal differential rotation of the convection zone plays a significant role in the internal dynamics of the Sun. Using rotational splitting coefficients of the p-mode frequencies, obtained during 1986-1990 at the Big Bear Solar Observatory, we have found that the thickness of the transitional layer is 0.09 ∓ 0.04 solar radii (63 ∓ 28 Mm), and that most of the transition occurs beneath the adiabatically stratified part of the convection zone, as suggested by the dynamo theories of the 22 yr solar activity cycle.

Original languageEnglish (US)
Pages (from-to)L61-L64
JournalAstrophysical Journal
Volume469
Issue number1 PART II
DOIs
StatePublished - 1996
Externally publishedYes

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Keywords

  • Convection
  • Methods: data analysis
  • Sun: activity
  • Sun: interior
  • Sun: oscillations
  • Sun: rotation

Fingerprint Dive into the research topics of 'Helioseismic constraints on the gradient of angular velocity at the base of the solar convection zone'. Together they form a unique fingerprint.

Cite this