New insights about the origin of solar wind

Images from telescopes aboard a Japanese satellite have shed new light about the Sun's magnetic field and the origins of solar wind.Provided by NASA Headquarters, Washington, D.C.
By | Published: December 10, 2007 | Last updated on May 18, 2023
This image, taken January 10, 2007 by Hinode’s X-ray telescope, shows an X-ray jet launching plasma out into the solar system from the Sun’s north polar coronal hole.
December 10, 2007
Data from the Japanese satellite, Hinode, shows that magnetic waves play a critical role in driving the solar wind into space. The solar wind is a stream of electrically charged gas that is propelled away from the Sun in all directions at speeds of almost 1 million miles per hour. Better understanding of the solar wind may lead to more accurate prediction of damaging radiation waves before they reach satellites.

How the solar wind is formed and powered has been the subject of debate for decades. Alfven waves in principle can transfer energy from the Sun’s surface up through its atmosphere, or corona, into the solar wind. Because of this, powerful magnetic Alfven waves in the electrically charged gas near the Sun have always been a leading candidate as a force in the formation of solar wind.

In the solar atmosphere, Alfven waves are created when convective motions and sound waves push magnetic fields around, or when dynamic processes create electrical currents that allow the magnetic fields to change shape or reconnect.

“Until now, Alfven waves have been impossible to observe because of limited resolution of available instruments,” says Alexei Pevtsov, Hinode program scientist from NASA Headquarters in Washington. “With the help of Hinode, we are now able to see direct evidence of Alfven waves, which will help us unravel the mystery of how the solar wind is powered.”

Using Hinode’s high resolution X-ray telescope, a team led by Jonathan Cirtain, a solar physicist at NASA’s Marshall Space Flight Center in Huntsville, Alabama, was able to peer low into the corona at the Sun’s poles and observe record numbers of X-ray jets. The jets are fountains of rapidly moving hot plasma. Previous research detected only a few jets daily.

With Hinode’s higher sensitivity, Cirtain’s team observed an average of 240 jets per day. They conclude that magnetic reconnection, a process where two oppositely charged magnetic fields collide and release energy, is frequently occurring in the low solar corona. This interaction forms both Alfven waves and the burst of energized plasma in X-ray jets.

“These observations show a clear relationship between magnetic reconnection and Alfven wave formation in the X-ray jets,” says Cirtain. “The large number of jets, coupled with the high speeds of the outflowing plasma, lends further credence to the idea that X-ray jets are a driving force in the creation of the fast solar wind.”

Another research team led by Bart De Pontieu, a solar physicist at Lockheed Martin’s Solar and Astrophysics Laboratory in Palo Alto, California, focused on the Sun’s chromosphere, the region sandwiched between the solar surface and its corona. Using extremely high-resolution images from Hinode’s Solar Optical Telescope, De Pontieu’s team found that the chromosphere is riddled with Alfven waves. When the waves leak into the corona, they are strong enough to power the solar wind.

“We find that most of these Alfven waves have periods of several minutes, much longer than many theoretical models have assumed in the past,” says De Pontieu. Comparisons with advanced computer simulations from the University of Oslo in Norway, indicate that reconnection is not the only source of the Alfven waves. De Pontieu continues, “The simulations imply that many of the waves occur when the sun’s magnetic field is jostled around by convective motions and sound waves in the low atmosphere.”