Powerful 'Conveyor Belts' Drive Sun's 11-year Cycle

Posted on: Jun 22, 2003

A cross-sectional view of the Sun's meridional circulation

The conveyor belt-like circulation extends through the Sun's convection zone — the outermost 30 percent of the solar interior. The flow is toward the poles at the surface and toward the equator at the base of the convection zone. The speed of the flow at the bottom sets the 11-year period of the sunspot cycle as well as the strength of future sunspot cycles. The colors in this image reveal the rotation rate of the different regions, red for rapid rotation with a 25-day period, orange for average rotation with a 27-day period, and blue for slow rotation with a 35-day rotation. (Dibyendu Nandy/Montana State University)

NASA and university astronomers have found evidence the 11-year sunspot cycle is driven in part by a giant conveyor belt-like, circulating current within the Sun.

The astronomers, Dr. David Hathaway, Robert Wilson and Ed Reichmann of NASA's Marshall Space Flight Center in Huntsville, Ala., and Dr. Dibyendu Nandy of Montana State University in Bozeman, reported their findings the week of June 16 at the annual meeting of the Solar Physics Division of the American Astronomical Society in Laurel, Md. The results were also published in the May 20 issue of the Astrophysical Journal.

The astronomers made their discovery by reviewing the positions and sizes of all sunspots seen on the Sun since 1874. "The sunspots appear in two bands on either side of the Sun's equator," said Hathaway. "Although the individual sunspots come and go from week-to-week, the central positions of the bands in which they appear drift slowly toward the solar equator over the course of each 11-year sunspot cycle."

Previously, scientists believed this equator-ward drift was a wave-like process involving magnetic forces. However, this new evidence suggests this drift is produced by a giant circulation system in which the compressed gases, 125,000 miles below the Sun's surface, move from the Sun's poles to its equator at about three mph — a leisurely walking pace. The gases then rise near the equator and turn back toward the poles, traveling in the surface layers where the gas is less compressed — moving at a faster rate of approximately 20 to 40 mph. Recent progress in theoretical modeling of the sunspot cycle has emphasized the important role of this circulation.

The speed of this circulation system, called a meridional circulation, changes slightly from one sunspot cycle to the next. The circulation is faster in cycles shorter than the average 11-year period and slower in cycles longer than the average period. This is a strong indication that this circulation acts like an internal clock that sets the period of the sunspot cycle.

The circulation also appears to influence the strength of future cycles, as seen in the number and sizes of the sunspots produced, not in the cycle immediately following, but rather in a two-cycle or 22-year time lag. When the flow is fast, it concentrates the magnetic field at the Sun's poles. These stronger fields are then transported downward into the solar interior where they are further compressed and amplified to become the intense magnetic fields that form sunspots years later.

The Sun is now in the declining phase of the current sunspot cycle that peaked in 2000 and 2001. Because the circulation flow was fast during the previous cycle, the astronomers believe the next cycle will be a strong one, peaking in the years 2010 and 2011.

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