Cluster Helps Disentangle Turbulence in the Solar Wind
From Earth, the Sun looks like a calm, placid body that does little
more than shine brightly while marching across the sky. Images from a
bit closer, of course, show it’s an unruly ball of hot gas that
can expel long plumes out into space – but even this isn’t
the whole story. Surrounding the Sun is a roiling wind of electrons and
protons that shows constant turbulence at every size scale: long
streaming jets, smaller whirling eddies, and even microscopic movements
as charged particles circle in miniature orbits. Through it all, great
magnetic waves and electric currents move through, stirring up the
particles even more.
This solar wind is some million degrees Celsius, can move as fast as
750 kilometers (466 statute miles) per second, and – so far
– defies a complete description by any one theory. It’s
hotter than expected, for one, and no one has yet agreed which of
several theories offers the best explanation.
Now, the ESA/NASA Cluster mission – four identical spacecraft
that fly in a tight formation to provide 3-dimensional snapshots of
structures around Earth – has provided new information about how
the protons in the solar wind are heated.
“We had a perfect window of 50 minutes,” says NASA
scientist Melvyn Goldstein, chief of the Geospace Physics Laboratory at
NASA’s Goddard Space Flight Center in Greenbelt, Md. and
co-author of the new paper that appeared in Physical Review Letters on
September 24. “It was a time when the four Cluster spacecraft
were so close together they could watch movements in the solar wind at
a scale small enough that it was possible to observe the heating of
protons through turbulence directly for the first time."
Scientists know that large turbulence tends to “cascade”
down into smaller turbulence -- imagine the sharply defined whitecaps
on top of long ocean waves. In ocean waves, the energy from such
cascades naturally adds a small amount of heat from friction as the
particles shift past each other, thus heating the water slightly. But
the fast, charged particles – known as “plasma” --
around the sun don’t experience that kind of friction, yet they
heat up in a similar way.
“Unlike the usual fluids of everyday life,” says Fouad
Sahraoui, lead author of a new paper on the solar wind and a scientist
at the CNRS-Ecole Polytechnique-UPMC in France, “plasmas possess
electric and magnetic fields generated by the motions of proton and
electrons. This changes much of the intuitive images that we get from
observing conventional fluids.”
Somehow the magnetic and electric fields in the plasma must contribute
to heating the particles. Decades of research on the solar wind have
been able to infer the length and effects of the magnetic waves, but
direct observation was not possible before the Cluster mission watched
large waves from afar. These start long as long wavelength
fluctuations, but lose energy – while getting shorter –
over time. Loss of energy in the waves transfer energy to the solar
wind particles, heating them up, but the exact method of energy
transfer, and the exact nature of the waves doing the heating, has not
been completely established.
In addition to trying to find the mechanism that heats the solar wind,
there’s another mystery: The magnetic waves transfer heat to the
particles at different rates depending on their wavelength. The largest
waves lose energy at a continuous rate until they make it down to about
100-kilometer wavelength. They then lose energy even more quickly
before they hit around 2-kilometer wavelength and return to more or
less the previous rate. To tackle these puzzles, scientists used data
from Cluster when it was in the solar wind in a position where it could
not be influenced by Earth’s magnetosphere.
For this latest paper, the four Cluster spacecraft provided 50 minutes
of data at a time when conditions were just right -- the spacecraft
were in a homogeneous area of the solar wind, they were close together,
and they formed a perfect tetrahedral shape -- such that the
instruments could measure electromagnetic waves in three dimensions at
the small scales that affect protons.
The measurements showed that the cascade of turbulence occurs through
the action of a special kind of traveling waves – named
Alfvén waves after Nobel laureate Hannes Alfvén, who
discovered them in 1941.
The surprising thing about the waves that Cluster observed is that they
pointed perpendicular to the magnetic field. This is in contrast to
previous work from the Helios spacecraft, which in the 1970’s
examined magnetic waves closer to the sun. That work found magnetic
waves running parallel to the magnetic field, which can send particles
moving in tight circular orbits – a process known as cyclotron
resonance -- thus giving them a kick in both energy and temperature.
The perpendicular waves found here, on the other hand, create electric
fields that efficiently transfer energy to particles by, essentially,
pushing them to move faster.
Indeed, earlier Cluster work suggested that this process – known
as Landau damping – helped heat electrons. But, since much of the
change in temperature with distance from the sun is due to changes in
the proton temperature, it was crucial to understand how they obtained
their energy. Since hot electrons do not heat protons very well at all,
this couldn’t be the mechanism.
That Landau damping is what adds energy to both protons and electrons
– at least near Earth – also helps explain the odd rate
change in wave fluctuations as well. When the wavelengths are about 100
kilometers or a bit shorter, the electric fields of these perpendicular
waves heat protons very efficiently. So, at these lengths, the waves
transfer energy quickly to the surrounding protons -- offering an
explanation why the magnetic waves suddenly begin to lose energy at a
faster rate. Waves that are about two kilometers, however, do not
interact efficiently with protons because the electric fields oscillate
too fast to push them. Instead these shorter waves begin to push and
heat electrons efficiently and quickly deplete all the energy in the
waves.
“We can see that not all the energy is dissipated by
protons,” Sahraoui said. “The remaining energy in the wave
continues its journey toward smaller scales, wavelengths of about two
kilometers long. At that point, electrons in turn get heated.”
Future NASA missions such as the Magnetospheric Multiscale mission,
scheduled for launch in 2014, will be able to probe the movements of
the solar wind at even smaller scales.
Cluster recently surpassed a decade of passing in and out of our
planet's magnetic field, returning invaluable data to scientists
worldwide. Besides studying the solar wind, Cluster’s other
observations include studying the composition of the earth’s
aurora and its magnetosphere.
