Io's Alien Volcanoes
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Scientists are eager for a closer look at the solar
system's strangest and most active volcanoes when Galileo flies
by Io on October 11.
October 4, 1999: Thirty years
ago, before the Voyager probes visited Jupiter, if you had described
Io to a literary critic it would have been declared overwrought
science fiction. Jupiter's strange moon is literally bursting
with volcanoes. Dozens of active vents pepper the landscape which
also includes gigantic frosty plains, towering mountains and
volcanic rings the size of California. The volcanoes themselves
are the hottest spots in the solar system with temperatures exceeding
1800 K (1527 C). The plumes which rise 300 km into space are
so large they can be seen from Earth by the Hubble Space Telescope.
Confounding common sense, these high-rising ejecta seem to be
made up of, not blisteringly hot lava, but frozen sulfur dioxide.
And to top it all off, Io bears a striking resemblance to a pepperoni
pizza. Simply unbelievable.
Right: Digital Radiance simulation of Pillan Patera just before the Galileo flyby. click for animation.
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For a world dominated by fiery volcanoes, it's curious that Io is also very, very cold. The ground just around the volcanic vents is literally sizzling, but most of Io's surface is 150 degrees or more below 0 C. The moon's negligible atmosphere traps little of the meager heat from the distant Sun. As soon as volcanic gases spew into the air they immediately begin to freeze and condense. The plumes of Io's sizzling volcanoes are very likely made up of sulfur dioxide snow.
Above: This false color infrared
composite of Jupiter's moon Io was produced from images acquired
in July and September, 1996 by NASA's Galileo spacecraft. The
area shown is 11,420 kilometers in width. Deposits of sulfur
dioxide frost appear in white and gray hues while yellowish and
brownish hues are probably due to other sulfurous materials.
Sulfur dioxide is normally a gas at room temperatures, but it
exists on Io's surface as a frost after condensing there from
the hot gases emanating from the Io volcanoes. Bright red materials
(such as the prominent ring surrounding the currently erupting
plume Pele) and spots with low brightness or albedo ("black"
spots) mark areas of recent volcanic activity and are usually
associated with high temperatures and surface changes.
"Io has lots of thermal areas just like Yellowstone," says JPL's Bill Smythe. "The volcanic plumes get most of the attention but there are probably also things like fumeroles and geysers. On a previous flyby the Particles and Fields instruments saw a deficit of energetic particles over Io where gas was probably coming out of the surface -- but no plumes were seen. We call this the 'stealth plume hypothesis.' The closest Earthly analog to what's happening would be a water geyser like Old Faithful. In fact, if you put Old Faithful on Io it would be about 37 km high!"
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"For the October flyby we'll be targeting four major volcanoes," says JPL's Duane Bindschadler, the manager of Galileo's Science Planning and Operations Team, "Pillan Patera, Prometheus (the most prominent one on the surface), Loki, and Pele. The pictures will be great. To put this in perspective, the very best images from Voyager had 500 m resolution. We'll be getting over 100 images at least that good, and the best images will show details only 7 meters across."
"But we won't just be running the camera," he continued. "Just about every instrument on the spacecraft will be turned on during the flyby. The most important ones for volcano science are probably the solid state imaging camera (SSI), the near infrared spectrometer (NIMS) and the photopolarimeter-radiometer (PPR)."
Each of these instruments does something different. NIMS spectra can be used to deduce the composition of plumes, flows and other surface features. The PPR measures the polarization and intensity of sunlight and thermal radiation. This helps scientists understand what atmospheric and volcanic gases are made of and how things are heated. The SSI camera takes high resolution pictures in optical light. Each of the three can also be used like a thermometer to measure the temperature of features on Io. The NIMS and PPR instruments are better at reading the temperature of cool material like plumes and ground frost. Around hots spots warmer than 700 K, where the NIMS and PPR detectors saturate, the SSI camera can be used to estimate temperature. By using the SSI, NIMS and PPR together scientists hope to get a more complete picture of Io's volcanic activity.
Above: The bright spots in this image indicate the locations of volcanic vents on Io, which are spewing hot lava. This image and other data from NASA's Galileo spacecraft indicate that the lava at Pillan Patera (marked Pillan) exceeded 1,700 degrees kelvin (2,600 degrees Fahrenheit) and may have reached 2,000 degrees kelvin (3,140 degrees Fahrenheit). The hottest eruptions on Earth today reach temperatures of about 1,500 kelvin (2,240 degrees Fahrenheit), but hotter lava erupted billions of years ago. [more information]
"The biggest mystery about Io's volcanoes is why they're so hot," says Bill Smythe, a co-investigator on JPL's NIMS team. "At 1800 K, the vents are about 1/3 the temperature of the surface of the sun! Billions of years ago basaltic lava on Earth was about that hot, but now -- thanks to mixing in subduction zones -- terrestrial basalts have a lower melting point. Lavas we see now on Earth are about 300 K cooler than they used to be. It's very surprising to see lava flows on Io as hot as these ancient flows on Earth. Why? Simply because Io's soil has been reworked many, many times, so the melting temperature should be lower for the same reason that Earth's basalts melt at a lower temperature. It's a real mystery."
"Originally we thought all the lava flows were sulfurous, but sulfur vaporizes at ~700K. The 1800 K regions have to be basaltic. Now the questions is 'are any of the lava flows sulfurous?' Galileo has detected areas on Io with temperatures between 300 and 600 K. That's about right for molten sulfur. But those could also be places where tiny volcanic vents at ~1800 K are surrounded by cold ground. From a distance the average temperature would appear to be 300 - 600 K. We need higher resolution data to figure out what's going on. If we're lucky Galileo will fly right over one of these spots in October and we'll have the answer."
Understanding the balance between sulfur and silicate (basaltic) volcanism is important for scientists who are trying to understand how Io's interior is heated. Sulfur has a lower melting point so it doesn't need as much energy to make lava. The basaltic flows require much more internal heat.
Right: This Voyager image of Ra Patera, a large shield volcano on Io, shows colorful flows up to 200 miles long emanating from the dark central volcanic vent. Copyright Calvin J. Hamilton More information.
"Another thing we'll be going for with these close-up flybys are high resolution pictures of the lava flows," continued Smythe. "We really want to know what the shapes and edges of the flows look like because that can tell us a lot about the properties of the lava. On Earth lava flows form little side lobes, or extrusions that look like arms, feet and toes. They range in size from a few centimeters to meters. From experiments on Earth, we know how to estimate the viscosity of the lava and other material properties from the shapes and sizes of the toes. That's what we want to do on Io, but the best resolution we have now is 1 km. At closest approach we'll have resolutions of only 7 meters. When we start seeing how the toes form we'll know what kind of flows these are."
Some of the most exciting results from the upcoming flybys will result from great improvements in resolution. For example, the best resolution of previous NIMS data is only 60 km.
"You can hide a lot in 60 km," points out Smythe. "During the closest flybys NIMS will see things just a few hundred meters across. That'll be a first."
"Another thing we're hoping to get in October is a plume seen in profile as the spacecraft passes by Io and looks back over the limb," continues Smythe. "By looking at the polarization of sunlight passing through the plume with the PPR, we ought to get some really valuable information about the temperature and density of particles coming out of the vents."
Here on Earth scientists will be eagerly awaiting the new
data. For instance, at the University of Texas, Dr. David Goldstein
and graduate students J. Victor Austin and Ju Zhang, following
the pioneering work of Sue Keefer, have been working for years
on computer simulations of Io's volcanic plumes. Using a technique
called Monte Carlo direct simulation, they send computerized
test particles blasting out of a model volcanic vent. The University
of Texas program tracks the motion of ejected molecules taking
into account intermolecular collisions, energy input from the
Io torus, and energy lost to infrared radiation. By varying the
size of the vent, the temperature and velocity of the ejected
gas, and the temperature of the surrounding terrain they can
match the appearance of their computerized plumes with the ones
photographed by NASA space probes. Sometimes this leads to new
insights about the fluid dynamics and physics of Io's volcanoes.
"The upcoming flybys could substantially improve our models by providing better boundary conditions," says Goldstein. "We need to know lots of things. What are the particle velocities and temperatures coming out of the volcanic vents? How do the molecules interact with the surface? Do they stick immediately or do they bounce? etc..."
"Right now when we look at a photograph of a plume, we really are not certain what we're seeing. It might be gas, it might be dust entrained in the gas, or gas that has condensed out to form ice crystals. We assume that whatever it is traces volcanic gas but we can't be sure. Hopefully the flybys will resolve some of these issues."
In one of the University of Texas sample models, pictured right, gas erupts from a vent at 2.7 times the velocity of sound into Io's tenuous atmosphere. The ejecta soar to a height of about 120 km. Much of the material lands about 150 km away where it hits the ground and bounces. Just before it hits the surface, the gas passes through a shock wave and heats up to 200 - 300 K.
Right: This image is one frame from a computer simulation of gas flowing in a volcanic plume. The vent is at the intersection of the vertical and horizontal axes. To view the flowing gas click on the image for a 0.4 MB MPEG animation. Colors in this picture represent gas temperature. Red is warm and blue is cooler. The gas in this model starts out at 200+ K near the vent. It cools as it rises and expands, then heats up again as it passes through the canopy shock. An important feature can be seen about 150 km from the vent where falling gas strikes the ground. The gaseous ejecta heats up and possibly scours away the sulfurous surface frost, exposing dirt and rock underneath. [more information]
"One of the most important features of this model is the canopy shock," points out Victor Austin. "It's where the gas rises to its apex and then falls back on itself. One way to think of the shock is to imagine a running water hose held straight up in the air. The water decelerates due to gravity and then comes back down. The same thing happens to a volcanic plume. It rises into the atmosphere and then gravity pulls it back. On Io the rising gaseous 'fluid' is supersonic so it forms a shock near the turnaround point."
"This is where the Io flybys might confirm some of our results. Gas cools very quickly after it passes through the shock, so it's possible that a layer of SO2 snow will form in the postshock region. Vertically the shock is very thin, so the layer of ice crystals is probably going to be thin, too. That's something we might see in the high resolution Galileo images."
"Another thing," said Goldstein, "many of our simulations show that warm material from the plume crashes down about 150 km from the vent. We think this might explain the dark rings we see in some of the spacecraft images (see left). These could be 'scouring rings' -- places where the SO2 frost is worn down to dirt and rock. Victor's calculations show that these rings themselves are wide but the edges are sharp. If we can see those edges in the close-up photos, it would help confirm our results. Some of the models also show a secondary scouring ring much further from the vent. We'll be looking for those in the new images, too. Scouring is one possibility, but the dark coloration may also simply be due to deposition of a different colored material coming out of the vent."
Above: Volcanoes on Jupiter's moon Io are compared in these images from NASA's Galileo spacecraft (right) taken in early September 1996, and from the Voyager spacecraft (left) taken in 1979. Prometheus (bright ring in upper right) was first seen as an erupting volcano by the Voyager spacecraft and still features an active plume. A smaller active plume was discovered at the volcano Culann Patera (dark feature at lower left) by the Galileo spacecraft. [more information]
Whatever the upcoming flybys reveal, the data are bound to improve our understanding of Io's volcanoes. "The programs we're running are unique," says Goldstein, "and we're looking forward to running our code with the very latest data."
Galileo has been orbiting Jupiter and its moons since December 1995. Its primary mission ended in December 1997. The spacecraft is currently near the end of a two-year extended mission that will culminate in two daring flybys of volcanoes on Io later this year. More information about the Galileo mission is available at: http://www.jpl.nasa.gov/galileo/
JPL manages Galileo for NASA' s Office of Space Science, Washington, D.C. JPL is a division of the California Institute of Technology, Pasadena, CA.
- Sulfuric Acid Discovered on Europa -- September 30, 1999. Sulfur from Io's fiery volcanoes may be responsible for a battery acid chemical on Europa with implications for astrobiology.
- Io or Bust -- September 16, 1999. Galileo braves extreme radiation as it plunges toward a close encounter with Io's volcanoes.
- Divining Water on Europa -- September 9, 1999. As circumstantial evidence for an underground ocean mounts, JPL scientists try an ingenious experiment to look for hexagonal ice crystals on the surface of Europa.
- Taking the Scenic Route to Io -- June 30, 1999. What's happening to the small craters on Callisto? That's the mystery scientists were contemplating as Galileo zoomed past Jupiter's pockmarked moon this morning in an orbit-changing maneuver designed to bring the spacecraft closer to volcanic Io.
- Turn Left at Callisto -- May 5, 1999. Galileo heads for a daring encounter with Io's volcanoes.
- Galileo buzzes Europa -- Feb. 2, 1999. Galileo executes a close flyby of Europa for the last time during the current mission.
- The Frosty Plains of Europa -- Dec. 3, 1998. As Galileo returns new images of Europa, NASA scientists prepare to study samples from a potentially similar environment here on Earth.
- Callisto makes a big splash -- Oct. 22, 1998. Scientists may have discovered a salty ocean and a possible ingredient for life on Jupiter's moon.
- Galileo takes a close look at icy Europa -- Oct 2, 1998. The spacecraft flew within 2300 miles of the mysterious satellite last weekend.
- Clues to possible life on Europa may lie buried in Antarctic ice -- Mar. 5, 1998. Exotic microbial forms turn up in ice above Antarctica's Lake Vostok.
- Ice, Water and Fire the Galileo Europa Mission
- Galileo home page at JPL, with the latest on Europa, Callisto and Io
- Jet Propulsion Laboratory home page
- Io from the SEDS Nine Planets web site
- Callisto from the SEDS Nine Planets web site
- Jupiter from the SEDS Nine Planets web site
- Io: The Prometheus Plume Aug. 18, 1997 Astronomy Picture of the Day
- Close-up of an Io volcano Aug. 4, 1995 Astronomy Picture of the Day
- Sizzling Io July 6, 1998 Astronomy Picture of the Day
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