Display options
Cite
Howe R, Christensen-Dalsgaard J, Hill F, et al. Deeply Penetrating Banded Zonal Flows in the Solar Convection Zone. Astrophys J. 2000;533(2):L163-L166doi: 10.1086/312623.
Howe, R., Christensen-Dalsgaard, J., Hill, F., Komm, R. W., Larsen, R. M., Schou, J., Thompson, M. J., & Toomre, J. (2000). Deeply Penetrating Banded Zonal Flows in the Solar Convection Zone. The Astrophysical journal, 533(2), L163-L166. https://doi.org/10.1086/312623
Howe, et al. "Deeply Penetrating Banded Zonal Flows in the Solar Convection Zone." The Astrophysical journal vol. 533,2 (2000): L163-L166. doi: https://doi.org/10.1086/312623
Howe R, Christensen-Dalsgaard J, Hill F, Komm RW, Larsen RM, Schou J, Thompson MJ, Toomre J. Deeply Penetrating Banded Zonal Flows in the Solar Convection Zone. Astrophys J. 2000 Apr 20;533(2):L163-L166. doi: 10.1086/312623. PMID: 10770715.
Copy Download .nbib Format: NLM
Share it on

Astrophys J. 2000 Apr 20;533(2):L163-L166. doi: 10.1086/312623.

Deeply Penetrating Banded Zonal Flows in the Solar Convection Zone.

The Astrophysical journal

Howe, Christensen-Dalsgaard, Hill, Komm, Larsen, Schou, Thompson, Toomre

PMID: 10770715 DOI: 10.1086/312623

Abstract

Helioseismic observations have detected small temporal variations of the rotation rate below the solar surface that correspond to the so-called "torsional oscillations" known from Doppler measurements of the surface. These appear as bands of slower- and faster-than-average rotation moving equatorward. Here we establish, using complementary helioseismic observations over 4 yr from the GONG network and from the MDI instrument on board SOHO, that the banded flows are not merely a near-surface phenomenon: rather, they extend downward at least 60 Mm (some 8% of the total solar radius) and thus are evident over a significant fraction of the nearly 200 Mm depth of the solar convection zone.

Publication Types