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Shields Up!

Sol and the local Milky Way. More at APOD
by Dr Tony Phillips
for NASA Science News
Huntsville (SPX) Sep 28, 2004
If you've ever watched Star Trek, you know the importance of shields. When a star explodes or a Klingon death ray lances out of the darkness, the captain yells two words, "Shields up!", and all is well. Deflector shields: Don't leave home without one.

The solar system, believe it or not, has got one.

The solar system's deflector shield is a giant magnetic bubble called "the heliosphere." It's part of the sun's magnetic field. No one knows the precise dimensions of the heliosphere, but it's bigger than the orbit of Pluto. All nine planets are inside it.

The heliosphere is important to life on our planet. A few million years ago, for instance, a cluster of massive stars drifted through our part of the Milky Way and exploded, one after another, like popcorn. Cosmic rays from the blasts were mostly deflected, sparing early humanoids a radiation bath.

But the bubble isn't perfect. The fact is, "it's leaky," says space scientist Eberhard Moebius of the University of New Hampshire. "Some things do get through." (This happens on Star Trek, too. If the ship's shields were impenetrable, there would never be any drama.)

Take cosmic rays for example. They are fragments of atoms shattered and accelerated to light speed by supernova blasts. The heliosphere deflects about 90% of them; the rest, the most powerful 10%, penetrate the inner solar system.

The bubble is even more vulnerable to particles with no electric charge. Magnetic fields can deflect charged particles like cosmic rays, but not neutral atoms and molecules or bits of dust and rock. The bubble is an open door to these.

To wit: a stream of neutral helium atoms--"an interstellar breeze," says Moebius--is flowing into the solar system right now. "It's coming from the direction of the constellation Sagittarius. Because the atoms in the stream are uncharged, the magnetic bubble does nothing to stop them."

Studying this stream is important because it can teach us a great deal about the heliosphere--How big is it? How leaky is it? It can also teach us about the interstellar "stuff" lurking just outside, says Moebius.

The stream, discovered 30 years ago, is actively monitored by a flotilla of NASA and European Space Agency spacecraft: SOHO, EUVE, ACE and, especially, Ulysses. Each measures something different. EUVE, for instance, can sense ultraviolet sunlight scattered from the stream, while Ulysses samples the stream itself, snatching atoms directly from the flow.

For many years the physical characteristics of the stream were only vaguely known. "But the ability we have now to take a close-up look at the stream using these modern spacecraft has made a difference," says Moebius. He recently led a research team at the International Space Science Institute in Switzerland; using data from the spacecraft they were able to pinpoint the stream's temperature, density and velocity:

Its temperature, 6000 C, is about the same as the surface temperature of the sun. A spacecraft flying through the stream won't melt, though, or even notice the heat. The gas in the stream is too wispy-thin, explains Moebius. "There are only 0.015 helium atoms per cubic centimeter." Earth's atmosphere at sea level, for comparison, is a thousand billion billion (1021) times denser. And, finally, the velocity of the stream is 26 km/s or 58,000 mph.

These numbers confirm what astronomers have long suspected. The solar system is colliding with a vast interstellar cloud.

Most people think space is empty, but it's not. The "void" between the stars is crowded with clouds of gas. Clouds on Earth are miles wide. Clouds in space are light years across. They range in character from inky-black and cold to colorful and glowing-hot. Stars are born in clouds, and they hurl even more clouds into space when they die. Interstellar clouds are everywhere, so it's no surprise that the solar system is running into one.

The question is, what kind of cloud?

This cloud, like most things in the Universe, consists mainly of hydrogen. We know this because the hydrogen absorbs telltale colors from the light of nearby stars. Astronomers use this absorption effect to trace the cloud's general outline: it is several light years wide and ragged-edged.

The cloud's abundant hydrogen doesn't easily penetrate the heliosphere because hydrogen atoms in the cloud are ionized by interstellar ultraviolet radiation. Like cosmic rays the hydrogen atoms are charged and, thus, held at bay. Helium atoms, on the other hand, are mostly neutral, so they slip into the solar system.

Although helium is only a minor ingredient of the cloud, it tells the researchers what the whole is like. The cloud's temperature is 6000 C, the same as the helium stream. Its velocity, 26 km/s, is the same, too. If the cloud contains a standard cosmic mix of hydrogen and helium--a reasonable assumption--then its overall density must be 0.264 atoms per cubic centimeter.

Arcania? Not at all.

These numbers are important. They are vital to the size and "leakiness" of the heliosphere. The bubble is inflated from the inside by the solar wind and compressed on the outside by the cloud. It's a balancing act. If the pressure of the cloud (a function of temperature, density and velocity) is high, it defeats the solar wind and makes the bubble smaller, lowering our defenses against cosmic rays.

Thousands of years from now, some researchers believe, the solar system will pass completely through this cloud and emerge in a low-pressure cavity blown by those supernovas a few million years ago. The heliosphere will expand, providing improved protection against cosmic rays.

After that who knows? Another cloud might come along compress the bubble again. The ISSI team's research, eventually, could tell us how the heliosphere will react.

Shields up? Shields down? It's not science fiction any more.

Related Links
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NASA Announces Space Radiation Materials Research Grants
Washington DC (SPX) Aug 04, 2004
NASA has selected 19 researchers to conduct ground-based research in space radiation biology and space radiation shielding materials. Sponsored by NASA's Exploration Systems Mission Directorate, this research will use the NASA Space Radiation Laboratory (SRL) and the Alternating Gradient Synchrotron at the Department of Energy's Brookhaven National Laboratory on Long Island, N.Y.

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