A NOTE ON THE TORSIONAL OSCILLATION AT SOLAR MINIMUM

Journal Article · Thu Aug 20 00:00:00 EDT 2009 · Astrophysical Journal (Online)

DOI:https://doi.org/10.1088/0004-637X/701/2/L87; COUNTRY OF INPUT: INTERNATIONAL ATOMIC ENERGY AGENCY (IAEA)· OSTI ID:21319541

Howe, R; Hill, F; Komm, R ^[1]; Christensen-Dalsgaard, J ^[2]; Schou, J ^[3]

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1. National Solar Observatory, P.O. Box 26732, Tucson, AZ 85726-6732 (United States)
2. Department of Physics and Astronomy, Aarhus University, DK-8000 Aarhus C (Denmark)
3. HEPL Solar Physics, 452 Lomita Mall, Stanford University, Stanford, CA 94305-4085 (United States)

We examine the evolution of the zonal flow pattern in the upper solar convection zone during the current extended solar minimum, and compare it with that during the previous minimum. The results suggest that a configuration matching that at the previous minimum was reached during 2008, but that the flow band corresponding to the new cycle has been moving more slowly toward the equator than was observed in the previous cycle, resulting in a gradual increase in the apparent length of the cycle during the 2007-2008 period. The current position of the lower-latitude fast-rotating belt corresponds to that seen around the onset of activity in the previous cycle.

• OSTI ID: 21319541
• Journal Information: Astrophysical Journal (Online), Vol. 701, Issue 2; Other Information: DOI: 10.1088/0004-637X/701/2/L87; Country of input: International Atomic Energy Agency (IAEA); ISSN 1538-4357
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
CONVECTION
EQUATOR
OSCILLATIONS
ROTATION
SUN