Cambridge, MA — Astronomers at the Harvard-Smithsonian Center for
Astrophysics (CfA) may have good news for the Earth: calmer weather
in space is ahead. When the Sun is more active and space weather gets
“stormy,” it has bad effects on our planet. Energy from solar
eruptions changes the orbits of satellites, causing them to spiral
back to the Earth. The intensified solar radiation and streams of
electrically charged particles can directly damage satellites and
increase radiation doses to astronauts. Solar eruptions perturb the
Earth’s magnetic field, causing communications disruptions especially
to cell phone and other wireless devices. Magnetic storms also cause
current surges in power lines that destroy equipment and knock out
power over large areas.

The predictions of calmer weather are the result of analyzing
observations from a CfA instrument called the Ultraviolet Coronagraph
Spectrometer, or UVCS. These first-of-a-kind observations by UVCS and
other instruments aboard the international Solar and Heliospheric
Observatory (SOHO) are providing the best descriptions yet of the
workings of the Sun from its core to its surface. The observations
also are leading the way to better long-term predictions of how and
when the Sun’s gusty particle emissions are released to affect
spacecraft and life on Earth. Improved predictions are expected after
next-generation instruments come on line later in the decade. “We
need these better predictions as we become more dependent upon
satellites and reliable long-distance communications,” says CfA’s Dr.
Mari Paz Miralles.

Solar activity varies over an 11-year cycle. Every eleven years the
Sun undergoes a period of low activity called solar minimum that
ascends to a period of high activity called solar maximum and then
back to solar minimum. One way of tracking the solar activity is by
observing sunspots. Sunspots are regions of intense magnetic field
that are cooler and darker than the surrounding areas of the Sun’s
surface. These active regions can erupt and cause solar flares and
coronal mass ejections, which hurl energetic, electrically charged
particles toward the Earth. During solar minimum there are only a few
sunspots on the Sun’s surface, while during solar maximum there are
about 20 times more spots.

Space weather is influenced not only by the presence of active
regions, but also by coronal holes – open magnetic field regions of
the corona that have low density and brightness. At solar minimum,
the Sun generally has a coronal hole at each of its poles and none
near its equator. As solar activity increases, the coronal hole at
the Sun’s north pole shrinks, other smaller coronal holes emerge near
it, and they appear to migrate toward the solar equator and
eventually to the south pole. The same happens in reverse at the
Sun’s south pole. At solar maximum, the coronal holes are found near
the equator along with active regions. As the Sun spins, coronal mass
ejections and high-energy atomic particles from solar flares are
sprayed at the Earth like water from a twirling garden sprinkler. As
the solar cycle continues, the coronal holes complete their migration
to the opposite pole, causing the Sun’s magnetic poles to reverse.
The changes in the magnetic field that lead to the flipping of the
Sun’s magnetic poles is the major reason for long-term variations in
space weather.

These observations above the solar surface reveal the workings of the
solar “dynamo” that operates in the Sun’s interior and generates the
solar magnetic field. Unlike the Earth, which has a molten iron core,
the Sun is gaseous throughout its interior. The Sun’s magnetic field
is created solely by electrical currents similar to the way an
electromagnet operates. In the Sun, these currents are produced by
the circulation of extremely hot, electrically charged gas or plasma.
A combination of the interior circulation of the plasma and the Sun’s
rotation creates the magnetic field. The dynamo action takes this
initially weak field and builds it up to a much stronger magnetic
field.

The main driver of this dynamo is the solar differential rotation:
the Sun is not a rigid body, but rotates faster at the equator than
at the poles. This differential rotation causes any north-south
magnetic field inside the Sun to be stretched out in the east-west
direction. This stretching contributes to the birth of new active
regions, which then drive the movement of magnetic flux to the poles,
eventually leading to a reversal of the Sun’s entire magnetic field.

The UVCS is valuable for studying the Sun because it is the only
instrument able to measure atomic particle speeds and temperatures in
the region of the solar corona where the primary accelerations of the
solar wind and coronal mass ejections occur. The UVCS has observed
the solar corona – the faint outer atmosphere of the Sun visible from
the Earth during a total solar eclipse – for six years and has
recorded drastic changes in this hot, tenuous layer. During this
period, the Sun’s activity increased from its lowest level in 1996 to
its maximum in 2000, then decreased again only to rebound in 2001.
This second increase in the Sun’s activity level created a
double-peaked activity maximum.

Another instrument called LASCO from the Navel Research Laboratory
makes images of the solar corona and determines particle densities.
Together, these two instruments have seen, for the first time, how
the densities, temperatures, and speeds of charged particles in the
expanding solar wind vary as solar activity changes. In 1996-1997 at
solar minimum, UVCS observed a simpler solar wind structure, with
fast, hot flows from polar coronal holes that remained open over long
periods of time. Around solar maximum, UVCS also observed coronal
holes at other places as well, like at the Sun’s equator and middle
latitudes. When comparing UVCS measurements of coronal holes at solar
minimum and maximum, scientists discovered intriguing differences.
The wind at solar minimum accelerates faster from coronal holes that
are both hotter and less dense than those at solar maximum. These
results were reported by Mari Paz Miralles and Steven Cranmer at an
international meeting on “SOHO Observations Over Half a Solar Cycle”
held in Davos, Switzerland earlier this month. The results are also
reported in two articles published in the March 10 and October 20,
2001 issues of Astrophysical Journal Letters.

Understanding the variation of the solar corona and its wind over the
solar cycle is vital for our comprehension of the Sun’s role in our
daily lives. As we approach solar minimum, only five years away, the
Sun will produce fewer solar flares and fewer coronal mass ejections.
But the coronal holes at the solar poles will fan out and their
magnetic fields will reach downward toward the solar equator,
allowing high-speed wind from the solar poles to reach the Earth.
During this relatively peaceful time ahead, we will still need to be
mindful of the approach of these high-speed wind streams and their
associated high-energy electrons and magnetic disturbances that will
still pose a threat to all of our satellite based essentials and
conveniences.

Headquartered in Cambridge, Massachusetts, the Harvard-Smithsonian
Center for Astrophysics (CfA) is a joint collaboration between the
Smithsonian Astrophysical Observatory and the Harvard College
Observatory. CfA scientists organized into seven research divisions
study the origin, evolution, and ultimate fate of the universe. The
Solar and Heliospheric Observatory (SOHO) is a mission of
international cooperation between the European Space Agency and NASA.

Note to editors: A high-resolution image of a coronal mass ejection
is online at http://cfa-www.harvard.edu/press/uvcs_images.html.