The three spacecraft involved were NASA's Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI), which takes pictures of flaring regions using the Sun's high-energy X-rays and gamma rays; NASA's Transition Region and Coronal Explorer (TRACE), which makes images using ultraviolet light from the Sun; and the Solar and Heliospheric Observatory (SOHO) spacecraft, a collaboration between NASA and the European Space Agency.

"This was the first time that we have been able to identify and study in detail the region on the Sun where the initiation and acceleration of a coronal mass ejection occurs," said Dr. Peter Gallagher, research scientist for RHESSI and SOHO at NASA's Goddard Space Flight Center, Greenbelt, Md., and lead author of two papers on this research.

"We now have a better understanding of how the energy release above the surface of the Sun relates to the ejection of material, perhaps allowing some real-time forecasts." The results are being presented today during a meeting of the American Astronomical Society's Solar Physics Division in a press conference at the Johns Hopkins University Applied Physics Laboratory, Laurel, Md.

Coronal Mass Ejections (CME) are often associated with solar flares. A flare is a giant explosion in the solar atmosphere that spews radiation and results in the heating of solar gas and the acceleration of particles to nearly the speed of light. Both events can be initiated in a matter of seconds, making their joint observations difficult to coordinate.

The twisting and snapping of magnetic field lines on the Sun, called magnetic reconnection, seem to cause CMEs and solar flares. When these fields snap from the buildup of magnetic energy, plasma is heated and particles are accelerated, resulting in massive explosions and emitting radiation ranging from radio waves to X-rays.

Frequently, a CME and flare will burst from the same region of the Sun nearly simultaneously. Just like the debate over whether the chicken or the egg came first, solar researchers discuss whether flares cause CMEs or the reverse, or if they are more loosely associated.

The April 21, 2002 observation confirmed the predominant scenario for high-speed CMEs (those moving at one million to 5 million miles per hour or 1.6 million to 8 million km/hr.).

This is where solar magnetic fields act like a lid, holding down a blob of gas (CME) that is trying to rise. Somehow, the magnetic lid opens, possibly as a result of magnetic reconnection and the generation of a flare, and then the CME rises from the Sun, dragging the magnetic fields with it. Magnetic reconnection continues to energize the associated flare for over 12 hours.

All three spacecraft played vital roles in confirming that this was the process. First, RHESSI saw a gradually increasing burst of X-rays announcing the start of the flare.

TRACE observed the CME in the extreme ultraviolet as it began to rise from the Sun. Several minutes later, RHESSI saw a burst of high energy X-rays under the erupting CME, and TRACE saw a similar explosion of ultraviolet rays, both indicating a large flare. SOHO then captured the CME as it continued moving away from the Sun.

"Each of these spacecraft is quite complementary," said Gallagher. "It�s only through their coordination in this observation that we�re now able to understand the predominant scenario for these fast, large coronal mass ejections and the associated flares."

The current results feed into the decades-old controversy over whether solar flares cause coronal mass ejections, or vice versa. While the first signs of the flare occur before the CME liftoff, the bulk of the flare energy is released later, after the CME has already been accelerated. The two phenomena are revealed to be merely different aspects of the same event, according to the team. For images and more information, refer to:

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