Solar Cycle Update
Updated predictions from NASA scientists place the
solar maximum in mid-2000.
14, 1999: Beginning in late September, a continuing series
of minor to moderate geomagnetic storms have triggered aurorae
along the northern tier of U.S states and may have affected some
public power systems operating at high northern latitudes. These
events were caused by high-speed material streaming out from
areas on the sun known as coronal holes. This
week we can expect more of the same as another coronal hole
rotates into position to send high-speed solar wind particles
toward our planet. Space weather forecasters expect moderate
levels of aurorae, shortwave radio disruptions, and power grid
fluctuations at high latitudes for at least the next three days.
Right: On Sept. 14 1999, the space-based SOHO observatory photographed a huge eruptive prominence escaping the Sun, seen in the upper right corner of the image. Prominences are loops of magnetic fields with hot gas trapped inside. Sometimes, as the fields become unstable, the prominence will erupt as this one did and become part of a coronal mass ejection. Beautiful prominences like these become more common as we approach solar maximum.
The recent increase in geomagnetic activity offers a taste of things to come as the Sun approaches the maximum of its 11-year sunspot cycle. As sunspot numbers mount, coronal mass ejections and solar wind disturbances will trigger more and more geomagnetic storms. In extreme cases, these storms can induce electric currents in the earth and oceans that interfere with electric power transmission equipment.
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It's not all bad news, though. The increased levels of solar activity will likely trigger dazzling auroral displays at mid-latitudes. Sky watchers in the continental U.S. will be treated to sights normally reserved for residents of higher latitudes. Another piece of good news is that increased atmospheric drag at solar maximum acts as a scavenger and helps clean out space debris from low-Earth orbit.
|Parents and Educators: Please visit Thursday's Classroom for lesson plans and activities related to this story.|
When will the solar maximum actually take place? Recent work by David Hathaway, a solar physicist at the Marshall Space Flight Center, and his collaborators indicate that the solar activity will peak around the middle of the year 2000.
"Our predictions have consistently targeted 2000 as the
beginning of solar maximum," says Hathaway, "but the
latest numbers suggest that the peak sunspot count in 2000 will
be a bit lower than expected. The projected peak is comparable
to, but lower than the peaks of the last two maxima (in 1989
and 1978). That would put all three of the recent sunspot maxima
in the same class -- above average compared to all the sunspot
cycles since the mid 1700's."
Above: By combining data about geomagnetic
activity during the previous solar cycle with sunspot counts
for the current cycle, David Hathaway and collaborators are able
to predict when the next sunspot maximum will occur. [Click
here for details]. According to their results, the sunspot
number -- and other forms of solar activity -- will peak beginning
in mid-2000. The dotted lines above and below the solid curve
line indicate the prediction curve's range of error.
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"The sunspot maximum is usually a broad peak. There is a two or three year period when activity is quite high. I wouldn't say that we're really in the solar maximum yet. I expect solar activity to be highest in 2000 and 2001, and then in 2002 it may decline back to where we are now in October 1999."
"The effects we've been experiencing for the past few weeks are relatively minor geomagnetic disturbances caused by the solar wind flowing out of coronal holes. A coronal hole is something you see in x-ray pictures of the sun where the corona appears dark. In contrast, bright spots in the x-ray image tend to overlie sunspot groups where hot gas is bottled up in magnetic fields that rise up out of one sunspot and bend back to reconnect at another spot nearby."
"The magnetic fields around coronal holes are different," he continued. "Instead of looping back to reconnect on the sun's surface, these magnetic fields are essentially open. They go way out into the solar system and no one knows exactly where they reconnect. These open field lines allow high-speed solar wind particles to escape."
In fact, the solar wind streams off of the Sun in all directions, not just from coronal holes. But the wind speed is high (800 km/s) over coronal holes and much lower (300 to 400 km/s) elsewhere. The higher pressure streams from coronal holes buffet the Earth's magnetic field and can produce geomagnetic activity.
For more information about space weather and current solar activity, including official alerts, warnings, and forecasts, please see NOAA's Space Environment Center web site at http://www.sec.noaa.gov/.
UVI aurora home page for new pictures every 7 minutes.
Surfing Magnetic Waves in the Solar Atmosphere July 8, 1999. How the Solar Wind Gets Up to Speed
Solar Flares Show Their True Colors June 2, 1999. New research points to a common mechanism for spectral behavior in Solar Flares
"Cool" microflares could be solar hot spots May 31, 1999. Secret of coronal heating may be multitude of tiny blasts.
Finding the smoking gun before it fires March 9, 1999. Physicists discover a new tool for predicting solar eruptions.
Recent stories on the August '99 Eclipse
Decrypting the Eclipse - August 6, 1999, scientists around the world explore the possible and mysterious effect of eclipses on the motion of Foucault's pendulum.
There goes the Sun - August 5, 1999, features general information about the August 11, 1999 solar eclipse, including the effect of eclipses on the birds and the bees, and eclipses on other planets.
Audio eclipse may fill the sky - August 4, 1999 story on investigations of ionization and radio propagation in Earth's atmosphere during the eclipse
Peering through a Hole in the Sky - June 17, 1999 story on exotic gravity measurements to be carried out during the eclipse
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Dr. John M. Horack , Director of Science Communications
Curator: Bryan Walls
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