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http://members.fortunecity.com/volcanopele/newsletter
Table of Contents
News and Stuf’
Editorials and Short Articles
1 Abstracts of Recently Published Papers
20 Titles or Abstracts of Accepted Papers
4 Titles of Submitted Papers
Conference Annoncements
Recent Conference Abstracts
Upcoming Events
Newsletter Info
In the Next Issue...
"That which I was in life, I am in death.
Though Jove wear out the smith from whom he took,
In wrath, the keen-edged thunderbolt with which
On my last day I was to be transfixed;
Or if he tire the others, one by one,
In Mongibello, at the sooty forge,
While bellowing: 'O help, good Vulcan, help!'-
Just as he did when there was war at Phlegra-
And casts his shafts at me with all his force,
Not even then would he have happy vengeance."
Capaneus, Inferno 14: 51-60
The resilient Galileo spacecraft doesn't know when it call it quits. So, NASA has outlined the details of one last mission extension, which includes five more flybys of the Jovian moons before a final plunge into the crushing pressure of the giant planet's atmosphere. On May 25, Galileo should pass about 123 kilometers (76 miles) above the moon Callisto, the second largest of Jupiter's 28 known moons. The effects of Callisto's gravity will set up the space probe for a swing over both polar regions of the intensely volcanic moon Io in August and October. Galileo will take pictures, measure magnetic forces, and study dust and smaller particles. Science goals include studying the extent of volcanism on Io, both in new and previously active sites; determining whether Io generates its own weak magnetic field; and gaining a better understanding of a doughnut-shaped ring, the Io Torus, that encircles Jupiter and contains electrically charged gases. In 2002, having completed its imaging mission, Galileo will continue studies of Jupiter's massive magnetic field with seven instruments. In January, the orbiter will fly near the equator of Io.
For more information: http://members.fortunecity.com/volcanopele/news010315.htm
The amount of lava gushing from individual volcanoes on Jupiter's moon Io dwarfs earthly comparisons, and the pace at which lava is repainting Io's surface suggests a novel technique for determining the relative ages of surface regions there. The latest research about Io, much of it based on data from NASA's Galileo spacecraft, was reported Wednesday at the Lunar and Planetary Science conference in Houston, Texas. Knowing the relative ages of surface features on a planet or moon is crucial for understanding the processes shaping that world. The favorite age gauge of planetary scientists is counting impact craters. The more impacts still showing, the older the surface. However, volcanoes are resurfacing Io so fast, not a single impact crater has been found there. "It appears that the same process that destroys the traditional way of dating surfaces is going to provide a new way to date surfaces," said Dr. Dennis Matson, a research scientist at NASA's Jet Propulsion Laboratory, Pasadena, Calif. "On Io, surface temperature can give us an indication of surface age."
For more information: http://members.fortunecity.com/volcanopele/news010314.htm
Two tall volcanic plumes and the rings of red material they have deposited onto surrounding surface areas appear in images taken of Jupiter's moon Io by NASA's Galileo and Cassini spacecraft in late December 2000 and early January 2001.
A plume near Io's equator comes from the volcano Pele. It has been active for at least four years, and has been far larger than any other plume seen on Io, until now. The other, nearer to Io's north pole, is a Pele-sized plume that had never been seen before, a fresh eruption from the Tvashtar Catena volcanic area.
The observations were made during joint studies of the Jupiter system while
Cassini was passing Jupiter on its way to Saturn. The two craft offered complementary
advantages for observing Io, the most volcanically active body in the solar
system. Galileo passed closer to Io for higher-resolution images, and Cassini
acquired images at ultraviolet wavelengths, better for detecting active volcanic
plumes.
The Cassini ultraviolet images, upper right, reveal two gigantic, actively erupting plumes of gas and dust. Near the equator, just the top of Pele's plume is visible where it projects into sunlight. None of it would be illuminated if it were less than 240 kilometers (150 miles) high. These images indicate a total height for Pele of 390 kilometers (242 miles). The Cassini image at far right shows a bright spot over Pele's vent. Although the Pele hot spot has a high temperature, silicate lava cannot be hot enough to explain a bright spot in the ultraviolet, so the origin of this bright spot is a mystery, but it may indicate that Pele was unusually active.
Also visible is a plume near Io's North Pole. Although 15 active plumes over Io's equatorial regions have been detected in hundreds of images from NASA's Voyager and Galileo spacecraft, this is the first image ever acquired of an active plume over a polar region of Io. The plume projects about 150 kilometers (about 90 miles) over the limb, the edge of the globe. If it were erupting from a point on the limb, it would be only slightly larger than a typical Ionian plume, but the image does not reveal whether the source is actually at the limb or beyond it, out of view.
A distinctive feature in Galileo images since 1997 has been a giant red ring of Pele plume deposits about 1,400 kilometers (870 miles) in diameter. The Pele ring is seen again in one of the new Galileo images, lower left. When the new Galileo images were returned this month, scientists were astonished to see a second giant red ring on Io, centered around Tvashtar Catena at 63 degrees north latitude. (To see a comparison from before the ring was deposited, see PIA-01604 or PIA-02309.) Tvashtar was the site of an active curtain of high-temperature silicate lava imaged by Galileo in November 1999 and February 2000 (image PIA-02584). The new ring shows that Tvashtar must be the vent for the north polar plume imaged by Cassini from the other side of Io! This means the plume is actually about 385 kilometers (239 miles) high, just like Pele. The uncertainty in estimating the height is about 30 kilometers (19 miles), so the plume could be anywhere from 355 to 415 kilometers (221 to 259 miles) high.
If this new plume deposit is just one millimeter (four one-hundredths of an inch) thick, then the eruption produced more ash than the 1980 eruption of Mount St. Helens in Washington.
NASA recently approved a third extension of the Galileo mission, including a pass over Io's north pole in August 2001. The spacecraft's trajectory will pass directly over Tvashtar at an altitude of 200 kilometers (124 miles). Will Galileo fly through an active plume? That depends on whether this eruption is long-lived, like Pele, or brief, and it also depends on how high the plume is next August. Two Pele-sized plumes are inferred to have erupted in 1979 during the four months between Voyager 1 and Voyager 2 flybys, as indicated by new Pele-sized rings in Voyager 2 images. Those eruptions, both from high-latitude locations, were shorter-lived than Pele, but their actual durations are unknown. Before its August flyby, Galileo will get another more-distant look at Tvashtar in May.
It has been said that Io is the heartbeat of the Jovian magnetosphere. The two giant plumes evidenced in these images may have had significant effects on the types, density and distribution of neutral and charged particles in the Jupiter system during the joint observations of the system by Galileo and Cassini from November 2000 to March 2001.
These Cassini images were acquired on Jan. 2, 2001, except for the frame at the far right, which was acquired a day earlier. The Galileo images were acquired on Dec. 30 and 31, 2000.Cassini was about 10 million kilometers (6 million miles) from Io, ten times farther than Galileo.
For more information: http://members.fortunecity.com/volcanopele/galileo010327.htm
NASA recently extended the successful Galileo spacecraft's mission until January 2003 to continue study of Jupiter's fascinating moons, particularly the extremely volcanic moon Io. Io - the most active world yet discovered - features modes of eruption not seen on Earth for billions of years, mountains taller than Mt. Everest, and a unique and poorly understood surface chemistry based on sulfur. But scientists say that a planned powerdown of Galileo's imaging suite at the end of this year will hamstring efforts to solve Io's many mysteries.
NASA has funded Galileo's instrument package through 2001 to include two further flybys of Io. NASA has also planned another Io flyby, during Galileo's thirty-third orbit (I33), on January 17, 2002. Dipping to within 100 km (62 miles) of Io's surface - lower than any previous Jupiter-system flyby - Galileo will fly over Io's sub-jovian hemisphere, which has never been imaged before at high resolution.
Unfortunately, funding for all imaging during the I33 flyby has recently been withdrawn, and the only chance to image the mysterious features on this hemisphere of Io at high resolution will be lost unless the decision is reversed.
The only images of this hemisphere returned from Galileo so far have been at low resolution, taken at very long range during the orbital tour - show several gigantic volcanoes and still-hot lava fields of varying composition. If funds are reinstated, Galileo will image the mountains Hi'iaka, Gish Bar, and Pan, a pair of enigmatic lava domes named Apis and Inachus Tholi, and the volcanoes Kanehekili and Mbali. Galileo will also measure the temperature of the volcanoes Kanehekili, Prometheus, Marduk, and Pillan and search for hot spots, which provide clues to the way Io dissipates its tidal heat.
"Every time we look at Io we see something unexpected and amazing. I33 gives Io one more chance to blow our socks off! The fact that we will be looking at a hemisphere not seen close-up since Voyager increases the chances of new and surprising discoveries," commented John Spencer of the Lowell Observatory.
"This is an exceptional opportunity to view Io's Jupiter facing hemisphere at high-resolution using Galileo's remote sensing capabilities. We have already done a lot of the necessary work. The observations are already planned and designed. Nobody wants to miss this unique chance," says Rosaly Lopes of NASA's Jet Propulsion Laboratory in Pasadena, Calif.
Jason Perry, a high school junior from Leavenworth, Kansas, has created a petition to persuade NASA to reverse its decision. The petition - "Pennies for Pele" - was started on March 30, 2001 and has already been signed by 650 Io scientists and others from around the world.
The cost of performing remote sensing during the January 2002 flyby is only $1.5 million dollars. This represents 0.1% of the funds spent to send Galileo to Jupiter, and a ten-thousandth of NASA's annual budget.
"The funding/science ratio for imaging at the January 2002 flyby is ridiculously cheap. Considering the amount of money it took us to get there, not funding I33 imaging makes absolutely no sense," commented Joseph Plassmann of the Planetary Image Research Laboratory in Tucson, Arizona.
It is hoped that 1000 signatures can be obtained before August 6, the date of the next Io flyby. Copies of the petition will then be passed to the NASA's Office of Space Science.
The petition can be signed online at:- http://fullspeed.to/Io
The last few weeks have been quite hectic for me. As most of you know, I have started a petition to convince NASA to fund remote sensing during I33. Against this online activity, I have had Calculus tests, an AP Chemistry presentation on the Outer Solar System (don’t ask), a report on Coleridge’s Rime of the Ancient Mariner in British Literature, and a downed tree in the backyard. However, luckily, summer is almost upon us (or winter for those reading from the Southern Hemisphere). My summer is going to be quite interesting. I will be working at the Lunar and Planetary Laboratory in Tucson, Arizona. I will be working on processing Io images from G29 and C30 as well as the Io flybys in 1999 and 2000. I will be heading out there on June 6th and coming back home on August 11th. Hopefully, work from this trip will provide some great articles for the next issue due out in July and the one after that in September. Wish me luck on this trip. I hope I don’t have to write a report about English poetry from the Romantic Age while there J
By Jason Perry
This is Part One of a Two Part series. This part describes the history of volcanic eruptions at Tvashtar and the observations of them. The second part, due out with Issue 4, will look at the changes in theories of Ionian volcanoes caused by the many Tvashtar eruptions.
On November 25, 1999, Galileo flew over Io’s South Pole. Due to a fault in Galileo’s computer system, close-up images of this region were unable to be taken. However, the medium-resolution images planned for this orbit were taken, thanks to the hard work of Galileo’s engineers on Earth. One of the observations saved was of a giant caldera recently named Tvashtar Catena. The observation was designed to observe the morphology of calderas near the poles. What was seen has ignited a debate over outburst volcanism on Io and how lava flows on the surface.
Tvashtar Catena is located near the North Pole of Io on the anti-jovian hemisphere. It consists of a chain of four calderas, all but one of which is active in some way, surrounded by a flat, one-kilometer tall mesa. The calderas at Tvashtar show various types of volcanism: classic calderas, long, ultramafic lava flows, long fissures, and explosive sapping.
The activity seen at Tvashtar in November 1999 was the first time major, active volcanism was seen there. SSI noted some small activity there before. In addition, some moderate activity was noted by ground-based observations in September 1999. This was likely a precursor to the activity seen in November 1999.
During the I25 pass of Io, Galileo took a medium-resolution observation of Tvashtar. This observation consisted of two images at 183 m/pixel. Originally, this observation was to consist of six images at a resolution of 366 m/pixel. However, due to problems seen during the previous Io flyby with the camera’s AI8 mode, the images were changed to IM8 mode. This increased the resolution of the images, but increased the amount of memory needed for each image. So the observation was cut to two images. This eliminated planned images of another giant northern caldera known as Savitr Patera (images of this volcano are planned during a flyby in August 2001).
When portions of the images were returned to earth in December 1999, scientists were astonished to find one of the calderas erupting. They found that portions of the images were bleeding. Bleeding occurs when a few pixels are so bright that they bleed into other pixels on a CCD. The only way such brightness can occur is if an area has an albedo of 1.0 or is very hot. Images taken in June 1999 show the area as being very dark so it must be the latter. Based on knowledge of how the camera responds to hot regions, a reconstruction of the hot area was possible. It was determined that the top part of the bleeding areas was the hot region. This hot area was along a linear line. Based on knowledge of volcanoes on earth and their eruption styles, the eruption was determined to be a lava curtain, 1.5 km tall.
Several observatories around the world, observing in conjunction with the Galileo spacecraft, witnessed the eruption. According to their observations, the eruption began as early as November 24. They noted it as a bright spot on Io in the 2-5 micron region indicating a very hot eruption. Another aspect of the ground-based observations was that Tvashtar was observed as being very bright even though it was near the bright limb of Io as seen from earth. Lave flows would appear to dim as the eruption site neared the limb. Based on these observations, the lava had to be moving vertically in a lava fountain or curtain, consistent with the Galileo observations. This gives more confidence in conclusions of Ionian volcanism based solely on ground-based data.
This remarkable discovery led to frantic plans to follow up. So Galileo imaging planners added a color Tvashtar observation to the next Io flyby, which took place on February 22, 2000. This observation was designed to look for small- to medium-scale changes due to the outburst in November 1999. The observation was to be in color to look for new surface deposits that were not seen in June 1999. When the observation was returned in the ensuing weeks, scientists were in for more surprises.
Most eruptions on Io, such as the eruption at Pillan in the summer of 1997, make some kind of surface change on Io, be it new deposits of frost, pyroclastic material, or sulfur, or new lava flows. However, when comparing the area around the eruption site in the February 2000 images to those taken in November 1999 and June 1999, few changes were found. The lava seen at the fissure was in the exact same shape as those seen in June 1999. The pyroclastic deposit surrounding the eruption site was the same size as those seen in June 1999. Therefore, something must be keeping the lava flows and pyroclastic material the same size or smaller. The lava flow shape is likely dominated by topographic constraints, like a caldera wall scarp. The pyroclastic flows may not have been as bad as previous eruptions at the site.
Galileo also observed active lava flows in the western caldera in the form of 50-km long lava flows. The main body of the lava flow was bright in the near-infrared filters of the camera. Also seen were bright spots at the ends of two "tongues" at the northern end of the lava flow. These either marked the vents that supplied the lava flow, or two flow fronts. It would be unique if two vents were sources for a single lava flow and both are active.
Monitoring of Io slowed through the spring and summer of 2000 so researchers could sift through all the new data that the three flybys of Io and associated activities created and to prepare for the Cassini flyby of Jupiter at the end of the year. In November of 2000, Io monitoring picked up again. On December 16, 2000, Franck Marchis, using the 3.6-m telescope at the La Silla Observatory in Chile, discovered a very bright eruption at Tvashtar Catena. The eruption had a radiance of 115 GW/micron/sr, similar to Loki at the height of its 1999 brightening.
Cassini saw the eruption as well. Eclipse images taken at end of 2000 and the beginning of 2001 showed a plume similar to that of Pele over the North Pole of Io. Galileo also observed Tvashtar Catena and found a bright red ring surrounding it, again similar to that around Pele. One could then conclude that the plume seen by Cassini formed the red ring and thus had to come from Tvashtar.
Tvashtar will be the star of the C30 and I31 encounters. During C30, Tvashtar’s plume will be observed at a resolution of 3.5 km/pixel in the violet filter. Tvashtar will also be observed in color at 3.9 km/pixel to further examine the plume deposit and to find the source of the newest eruption. During I31, Galileo will fly within 350 km of Tvashtar. Galileo will image the site of the 1999 eruption at resolution of 5 m/pixel. Galileo will also observe Tvashtar at 50 m/pixel for context and to observe the sapping scarps seen at Tvashtar. Tvashtar will also be observed in the next encounter, I32, in October, at 204 m/pixel.
In the next issue of Tvashtar Sun, I will profile some new theories about Ionian volcanism and geology due to observations of Tvashtar.
By Jason Perry
This week, Galileo entered the heart of the Jupiter system for the first time since its historic dual mission with the passing Cassini spacecraft. Rather than Jupiter and Ganymede being the stars, Callisto and Io star on this pass. Galileo flew by Callisto on Friday, May 25 at a distance of 125 km, the closest flyby of any satellite so far in the tour. Galileo will also observe Io from a distance. This flyby provides the best opportunity to observe Io on a global scale since June 1999.
Plans call for two dayside observations of Io and one eclipse observation. The first takes place while Io is in eclipse by Jupiter. This will be the highest resolution observation of Io while it is in eclipse at a resolution of 3.9 km/pixel allowing for the possibility to observe small, very hot hotspots on Io. SSI is capable of observing areas on Io hotter than 700 K, if it fits the entire pixel. Because of the higher resolution of this observation, smaller hotspots, which would not fill an entire pixel in previous observations, would be seen. Target hotspots in this observation include Zal, Amirani, Zal, and Kanehekili.
The other two images show Io while it is out of the eclipse. This first shows the leading hemisphere (called leading because it always faces the direction of motion as Io orbits Jupiter). This image has a resolution of 3.4 km/pixel and consists of a color mosaic and a partial frame in the violet filter. The color observation will show Hi’iaka, Masubi, Kanehekili, and Lei Zi. This mosaic would provide context for high-resolution images planned during I31 and I32 later this year. The partial frame was recently added in the hopes that the Tvashtar plume can be imaged, if it is still active. The plume was seen by Cassini during it flyby of Jupiter and it is hoped that it will still be active during the I31 flyby of Io. Galileo will pass only 350 km over the source of the plume. The partial frame will also determine the source of the plume. There are several active volcanoes at Tvashtar and G29 images did not provide enough resolution to determine the exact source (see Tvashtar article above).
The final image is a color observation of the antijovian hemisphere. This was the area imaged in July 1999 at global scales at a resolution of 1.5 km/pixel. This observation has a resolution of 3.9 km/pixel and would allow for detailed searches for surface changes since 1999. The most notable that was seen in a much lower resolution image from G29 is a new red ring around Tvashtar, similar to the one seen around Pele. Other notable volcanoes to be imaged include Prometheus and Amirani.
Other instruments have observations planned for C30. PPR will image Io as it enters an eclipse on May 23 and exits it to observe how the surface cools during an eclipse and how it warms up after one. This is important to determine porosity properties of the surface. NIMS will also observe Io while in eclipse and when it’s not to monitor volcanic activity.
C30 is just the tip of the iceberg. In a little less than three months, Galileo will begin a series of encounters with Io to again observe it up close. This time, Galileo will observe Io’s leading and projovian hemisphere to give scientists a good overview of the entire planet, not just the side that faces away from Jupiter. In Issue 4, I will preview the I31 encounter. In Issue 5, due out in September, I will preview the I32 encounter. Finally, in issue 7, due out in January, I will preview the I33 encounter.
Volcanism on Io: The View from Galileo
Ashley G. Davies
1 Jet Propulsion Laboratory-California Institute of Technology, Pasadena, CA, 91109
Io, Jupiter’s innermost Galilean satellite, is the most volcanically active body in the solar system. Ashley Gerard Davies reviews the wealth of data returned by NASA’s veteran spacecraft Galileo, that has led to a better understanding of the volcanic processes wracking Io.
Published in Journal of the Royal Astronomical Society 42, 4 (2001)
For reprints, contact: Ashley.Davies@jpl.nasa.gov
Robert R. Howell1, John R. Spencer2, Jay D. Gougen3, Franck Marchis4,5, Renée Prangé5, Thierry Fusco6, Diana L. Blaney3, Glenn J. Veeder3, Julie A. Rathbun2, Glenn S. Orton3, Aaron J. Grocholski1,7, John A. Stansberry2,8, Gary S. Kanner2, E. Keith Hege8
1 Department of Physics and Astronomy, University of Wyoming,
Laramie.
2 Lowell Observatory, Flagstaff, Arizona
3 Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
4 European Southern Observatory, Santiago, Chile
5 IAS, Université ParisSud, France
6 ONERA, Chatillon, France
7 Department of Physics, Georgia Southern University, Statesboro
8 Steward Observatory, University of Arizona
Ground-based observations of volcanism on Io during the period of the 1999 and early 2000 Galileo close flybys have detected several types of activity, providing information which complements the spacecraft observations. At Loki a brightening began between August 25 and September 9 and continued through February. On August 2 a major outburst was observed near (14 N, 74 W) whose brightness corresponds to area of approximately 350 km2 at a temperature of 1100 K. Observations of eruptions in late June (9906A) and in late November (9911A, at Tvashtar) provide temporal and photometric constraints on activity also seen by Galileo. High resolution adaptive optics images provide further information on the fainter sources distributed across the surface.
To Appear in JGR-Planets
For Preprints, contact: rhowell@uwyo.edu
Laszlo Keszthelyi1, Alfred McEwen1, Cynthia Phillips, Moses Millazzo1, Paul Geissler1, David Williams2, Elizabeth Turtle1, Jani Radebaugh1, Damon Simonelli3, and the Galileo SSI Team
1 Lunar and Planetary Laboratory, University of Arizona, Tucson,
AZ, 85719
2 Department of Geology, Arizona State University, Tempe,
AZ, 85287
3 Center for Radiophysics and Space Research, Cornell University,
Ithaca, NY, 14853
The Solid State Imaging (SSI) camera provided stunning views of Io's volcanoes as the Galileo spacecraft closed in on the fiery body in late 1999 and early 2000. While each volcanic center has many unique features, the majority can be placed into one of two broad categories. The "Promethean" eruptions, typified by the volcanic center Prometheus, are characterized by long-lived steady eruptions producing a compound flow field emplaced in an insulating manner over a period of years to decades. In contrast, "Pillanian" eruptions are characterized by large pyroclastic deposits, short-lived but high effusion rate eruptions from fissures feeding open channel or open sheet flows. Both types of eruptions often have ~100 km tall bright, SO2-rich plumes forming near the flow fronts and smaller deposits of red material mark the vent for the silicate lavas.
To Appear in JGR-Planets
For Preprints, contact: lpk@LPL.arizona.edu
Davies, A.G.1, L. P. Keszthelyi2, D. A. Williams3, C. B. Phillips4, A. S. McEwen2, R. M. C. Lopes1, W. D. Smythe1, L. W. Kamp1, L. A. Soderblom5 and R. W. Carlson1
1 Jet Propulsion Laboratory-California Institute of Technology,
Pasadena, CA, 91109
2 Lunar and Planetary Laboratory, University of Arizona,
Tucson, AZ, 85719
3 Department of Geology, Arizona State University, Tempe,
AZ, 85287
4 Center for the Study of Life in the Universe, SETI Institute,
Mountain View, CA 94043.
5 U.S. Geological Survey, Flagstaff, AZ, 86001
The Galileo spacecraft has been periodically monitoring volcanic activity on Io since June 1996 making it possible to chart the evolution of individual eruptions. We present results of co-analysis of NIMS and SSI data of eruptions at Pele and Pillan, especially from a particularly illuminating dataset consisting of mutually-constraining, near-simultaneous NIMS and SSI observations obtained during orbit C9 in June 1997. The observed thermal signature from each
hot spot, and the way in which the thermal signature changes with time, tightly constrains the possible styles of eruption. Pele and Pillan have very different eruption styles. From September 1996 through May 1999 Pele demonstrates an almost constant total thermal output, with thermal emission spectra indicative of a long-lived, active lava lake. The NIMS Pillan data exhibit the thermal signature of a "pillanian" eruption style, a large, vigorous eruption with associated open channel, or sheet flows, producing an extensive flow field by orbit C10 in September 1997. The high mass eruption rate, high liquidus-temperature (at least 1870 K) eruption at Pillan is the best candidate so far for an active ultramafic (magnesium-rich, "komatiitic") flow on Io, a style of eruption never before witnessed. The thermal output per unit area from Pillan is, however, consistent with the emplacement of large, open-channel flows. Magma temperature at Pele is ³ 1600 K. If the magma temperature is 1600 K it suggests a komatiitic-basalt composition. The power output from Pele is indicative of a magma volumetric eruption rate of ~250 to 340 m 3 s -1 . Although the Pele lava lake is considerably larger than its terrestrial counterparts, the power and mass fluxes per unit area are similar to active terrestrial lava lakes.
To Appear in JGR-Planets
For Preprints, contact: Ashley.Davies@jpl.nasa.gov
Russell, C.T.1, and M.G. Kivelson1
1 Department of Earth and Space Sciences and Institute of Geophysics and Space Physics University of California Los Angeles
To Appear in JGR-Planets
For preprints, go to: http://www.agu.org/pubs/pip/2000JE001342.pdf
Jani Radebaugh1, Laszlo Keszthelyi1, Alfred McEwen1, and the Galileo SSI Team
1 Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, 85719
To Appear in JGR-Planets
For preprints, contact: jani@LPL.arizona.edu
Elizabeth Turtle1, Windy Jaeger1, Laszlo Keszthelyi1, Alfred McEwen1, Moses Milazzo1, Jeff Moore2, Cynthia Phillips1, Jani Radebaugh1, Damon Simonelli3, Frank Chuang4, and the Galileo SSI Team
1 Lunar and Planetary Laboratory, University of Arizona, Tucson,
AZ, 85719
2 NASA Ames Research Center, Moffett Field, CA, 94035
3 Center for Radiophysics and Space Research, Cornell University,
Ithaca, NY, 14853
4 Department of Geological Sciences, Arizona State University,
Tempe, AZ, 85287
To Appear in JGR-Planets
For Preprints, contact: turtle@lpl.arizona.edu
Jeff Moore1, Robert J. Sullivan2, Frank Chuang3, James Head III4, Alfred McEwen5, Moses Milazzo5, Brian Nixon4, Robert Pappalardo4, Paul Schenk6, and Elizabeth Turtle5
1 NASA Ames Research Center, Moffett Field, CA, 94035
2 Center for Radiophysics and Space Research, Cornell University,
Ithaca, NY, 14853
3 Department of Geological Sciences, Arizona State University,
Tempe, AZ, 85287
4 Department of Geological Sciences, Brown University, Providence,
RI, 02912
5 Lunar and Planetary Laboratory, University of Arizona,
Tucson, AZ, 85719
6 Lunar and Planetary Institute, 3600 Bay Area Boulevard,
Houston, TX, 77058
To Appear in JGR-Planets
For Preprints, contact: jmoore@mail.arc.nasa.gov
Franck Marchis1,2, Renée Prangé2, Thierry Fusco3
1 European Southern Observatory, Casilla 19001, Santiago, 19,
Chile
2 Institut d'Astrophysique Spatiale, Université Paris
Sud, Orsay, France
3 ONERA, Chatillon, France
To Appear in JGR-Planets
For Preprints, contact: fmarchis@astron.berkeley.edu
Windy Jaeger1, Elizabeth Turtle1, Laszlo Keszthelyi1, Jani Radebaugh1, and Alfred McEwen1
1 Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, 85719
To Appear in JGR-Planets
For Preprints, contact: windy@lpl.arizona.edu
David Williams1, Ashley Davies2, Laszlo Keszthelyi3, and Ronald Greeley1
1 Department of Geology, Arizona State University, Tempe, AZ,
85287
2 Jet Propulsion Laboratory-California Institute of Technology,
Pasadena, CA, 91109
3 Lunar and Planetary Laboratory, University of Arizona,
Tucson, AZ, 85719
To Appear in JGR-Planets
For Preprints, contact: dwilliams@dione.la.asu.edu
Lopes, R.M.C.1, S. Doute2, L.W. Kamp1, W.D. Smythe1, R.W. Carlson1, A.S. McEwen3, P.E. Geissler3, S.W. Kieffer4, F.E. Leader2, A.G. Davies1, E. Barbinis1, R. Mehlman2, M. Segura1, J. Shirley1, and L.A. Soderblom5
1 Jet Propulsion Laboratory-California Institute of Technology,
Pasadena, CA, 91109
2 Institute of Geophysics and Planetary Physics, University
of California-Los Angeles, Los Angeles, CA, 90095
3 Lunar and Planetary Laboratory, University of Arizona,
Tucson, AZ, 85719
4 S.W. Kieffer Science Consulting Inc., Bolton, Ont, L7E
5T4
5 U.S. Geological Survey, Flagstaff, AZ, 86001
To Appear in JGR-Planets
For Preprints, contact: rlopes@lively.jpl.nasa.gov
Paul Geissler1, Alfred McEwen1, Cynthia Phillips2, Damon Simonelli3, Rosaly Lopes-Gautier4, S. Doute5
1 Lunar and Planetary Laboratory, University of Arizona, Tucson,
AZ, 85719
2 Center for the Study of Life in the Universe, SETI
Institute, Mountain View, CA 94043.
3 Center for Radiophysics and Space Research, Space Science Building,
Cornell University, Ithaca, NY 14853
4 Jet Propulsion Laboratory-California Institute of Technology,
Pasadena, CA, 91109
5 Institute of Geophysics and Planetary Physics, University
of California-Los Angeles, Los Angeles, CA, 90095
To Appear in JGR-Planets
For Preprints, contact: geissler@lpl.arizona.edu
David Williams1, Ronald Greeley1, Rosaly Lopes-Gautier2, and Ashley Davies2
1 Department of Geology, Arizona State University, Tempe, AZ,
85287
2 Jet Propulsion Laboratory-California Institute of Technology,
Pasadena, CA, 91109
To Appear in JGR-Planets
For Preprints, contact: dwilliams@dione.la.asu.edu
Wilson, L.1, and J.W. Head2
1 Dept. of Geological Sciences, Brown University, Providence,
RI, 02912
2 Environmental Sciences Dept., Lancaster University, Lancaster
LA1 4YQ
To Appear in JGR-Planets
For Preprints, contact: L.Wilson@lancaster.ac.uk
Simonelli, D.P.1, C. Dodd, and J. Veverka,
1 Center for Radiophysics and Space Research, Space Science Building, Cornell University, Ithaca, NY 14853
To Appear in JGR-Planets
For Preprints, contact: simonelli@cuspif.tn.cornell.edu
Milazzo, M.P.1, L. Keszthelyi1, and A.S. McEwen1
1 Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, 85719
To Appear in JGR-Planets
For Preprints, contact: mmilazzo@pirl.lpl.arizona.edu
Leone, G., and L. Wilson
To Appear in JGR-Planets
Matson, D.L., T.V. Johnson, G.J. Veeder, D.L. Blaney, and A.G. Davies
To Appear in JGR-Planets
Anderson, J.D., R.A. Jacobsen, E.L. Lau, G. Schubert, and W.B. Moore
To Appear in JGR-Planets
Julianne I. Moses1, Mikhail Yu. Zolotov2, and Bruce Fegley, Jr.3
1 Lunar and Planetary Institute, 3600 Bay Area Blvd., Houston,
TX 77058-1113
2 Department of Earth and Planetary Sciences, Washington
University, St. Louis, MO, 63130-4899
3 Planetary Chemistry Laboratory, Department of Earth and
Planetary Sciences, Washington University, St. Louis, MO, 63130-4899
Submitted to Icarus
For preprints, contact: moses@lpi.usra.edu
Julianne I. Moses1, Mikhail Yu. Zolotov2, and Bruce Fegley, Jr.3
1 Lunar and Planetary Institute, 3600 Bay Area Blvd., Houston,
TX 77058-1113
2 Department of Earth and Planetary Sciences, Washington
University, St. Louis, MO, 63130-4899
3 Planetary Chemistry Laboratory, Department of Earth and
Planetary Sciences, Washington University, St. Louis, MO, 63130-4899
Submitted to Icarus
For Preprints, contact: moses@lpi.usra.edu
Damon P. Simonelli1, Jeffery McLean, Laura Rossier, Paul Helfenstein, and Joseph Veverka
1 Center for Radiophysics and Space Research, Space Science Building, Cornell University, Ithaca, NY 14853
Submitted to Icarus
For Preprints, contact: simonelli@cuspif.tn.cornell.edu
Kivelson, M.G., K.K. Khurana, C.T. Russell, S.P. Joy, M. Volwerk, R.J. Walker, C. Zimmer, and J.A. Linker
Submitted to JGR-Space Physics
Boulder, Colorado
June 25 - 30, 2001
An international conference to discuss our understanding of the Jovian system
in light of the scientific results from the Galileo spacecraft (which has been
orbiting Jupiter since December 1995), the Galileo probe (which entered Jupiter's
atmosphere on December 7, 1995), the Cassini spacecraft (which passes Jupiter
in December 2000) as well as the Hubble Space Telescope and numerous ground-based
and theoretical studies. For information about the program, the meeting, etc.
go to <http://lasp.colorado.edu/jupiter/index.html>
where you can submit abstracts (deadline April 1st 2001) and register. There
is substantial discount if you stay 3 or more nights at the meeting hotel and
register before January 15th, 2001.
Sessions in this conference related to Io are:
For more information on this conference, go to http://lasp.colorado.edu/jupiter/index.html or contact JupMeet@lasp.colorado.edu
Boston, Massachusetts
May 29-June 2, 2001
For more information on this meeting go to: http://www.agu.org/meetings/sm01call.html.
Cassini Imaging of Auroral Emissions on the Galilean Satellites
P. Geissler, A. McEwen, C. Porco
Cassini and Galileo Satellite Imaging Results; Giant North Polar Plume on
Io
Alfred McEwen, P. Geissler, M. Belton, C. Porco, R. Pappalardo, T. Johnson,
S. Squyres, D. Williams, J. Head
A Change in Io's Sodium Clouds During the Cassini/Jupiter Flyby
J.K. Wilson, M. Mendillo
Io's Volcanoes: Possible Influence on Spin Axis
Paul R. Stoddard and D M Jurdy
Mass eruption rates and magma temperatures for ionian volcanoes as determined
from Galileo NIMS data
A.G. Davies and the NIMS Team
"Active Volcanism on Io" by Lopes
http://ns1.boulder.swri.edu/jupiter/pdf/LopesRMC.pdf
"The Lithosphere of Io" by McEwen
http://ns1.boulder.swri.edu/jupiter/pdf/McEwenAS.pdf
"Eruption Styles on Io as Seen By Galileo: a Comparison With Earth Volcanism" by Davies
http://ns1.boulder.swri.edu/jupiter/pdf/DaviesA.G.pdf
"Spatial Distribution and Chemical Nature of the 1.0 mm Absorber on Io’s Surface Inferred by the Near Infrared Mapping Spectrometer and the Solid State Imager of Galileo" by Douté
http://ns1.boulder.swri.edu/jupiter/pdf/DouteS.pdf
"Report on the Io Volcanic Activity Observed From the Ground With the ADONIS ESO and Keck AO Systems" by Marchis
http://ns1.boulder.swri.edu/jupiter/pdf/MarchisF.pdf
"A Predictable Volcano? Loki: From Groundbased and Galileo Data" by Rathbun
http://ns1.boulder.swri.edu/jupiter/pdf/RathbunJA.pdf
"Thermal Output of Io Measured in the 1-5 Micron Region by the Galileo Near Infrared Mapping Spectrometer" by Smythe
http://ns1.boulder.swri.edu/jupiter/pdf/SmytheWD.pdf
"Non-Synchronous Rotation of Io?" by Milazzo, M. P.
http://ns1.boulder.swri.edu/jupiter/pdf/MilazzoMP.pdf
"Ionian Mountain Formation Models" by Turtle
http://ns1.boulder.swri.edu/jupiter/pdf/TurtleEP.pdf
"Investigation of Potential Ultrabasic Eruptions on Io: Latest Galileo Results" by Williams
http://ns1.boulder.swri.edu/jupiter/pdf/Williams.Dave.pdf
"Regional Topographic Mapping of Io From Stereo Imaging" by Wilson
http://ns1.boulder.swri.edu/jupiter/pdf/Wilson.Ronda.pdf
"Formation and Evolution of Paterae on Io From Galileo SSI" by Radebaugh
http://ns1.boulder.swri.edu/jupiter/pdf/RadenbaughJ.pdf
"Topography of Io - Methods, Knowledge and Limits" by Schuster
http://ns1.boulder.swri.edu/jupiter/pdf/SchusterP.pdf
"Upper Limits to Io’s Background Heat Flow From Diurnal Heat Balance Considerations" by Spencer
http://ns1.boulder.swri.edu/jupiter/pdf/Spencer.Io.pdf
"Io's Sodium Clouds During the Cassini/Jupiter Flyby" by Mendillo
http://ns1.boulder.swri.edu/jupiter/pdf/MendilloM.pdf
"Io in Eclipse: Keck LWS Images and the Detection of the a-X 0-0 SO Band" by de Pater
http://ns1.boulder.swri.edu/jupiter/pdf/dePaterI.pdf
"SI_1479 Emissions From Io’s Atmosphere and its Implications" by Feaga
http://ns1.boulder.swri.edu/jupiter/pdf/FeagaL.pdf
"28 Hours: Insights Into the Evolution of Io's Dayside Atmosphere" by Jessup
http://ns1.boulder.swri.edu/jupiter/pdf/JessupKL.pdf
"HST/STIS Visible Images of Io in Eclipse" by Oliversen
http://ns1.boulder.swri.edu/jupiter/pdf/OliversenRJ.pdf
"High Definition/Adaptive Optics Spectral Imaging of Jupiter’s Satellites" by Wilson
http://ns1.boulder.swri.edu/jupiter/pdf/Wilson.Jody.pdf
"A Comparison of Sodium, Oxygen, and Sulfur in Io’s Corona" by Burger
http://ns1.boulder.swri.edu/jupiter/pdf/BurgerM.H.pdf
"Chlorine Compounds on Io: Volcanic/Atmospheric Chemistry and Surface Spectroscopy" by Schmitt
http://ns1.boulder.swri.edu/jupiter/pdf/SchmittB.pdf
"2-D Modeling of the Structure, Composition, and Dynamics of Io’s Atmosphere" by Smyth
http://ns1.boulder.swri.edu/jupiter/pdf/Smyth.Atmosphere.pdf
"Structure, Composition, Dynamics, and Evolution of the Galilean Satellites of Jupiter" by Schubert
http://ns1.boulder.swri.edu/jupiter/pdf/SchubertG.pdf
"Surface Composition of the Major Jupiter Satellites: Summary of Current Knowledge and Outstanding Issues" by McCord
http://ns1.boulder.swri.edu/jupiter/pdf/McCordTB.pdf
"Galileo PPR Observations of the Galilean Satellites" by Spencer
http://ns1.boulder.swri.edu/jupiter/pdf/Spencer.PPR.pdf
"Satellite Atmospheres" by McGrath
http://ns1.boulder.swri.edu/jupiter/pdf/McGrathMA.pdf
"Cassini Imaging of Auroral Emissions From the Galilean Satellites" by Geissler
http://ns1.boulder.swri.edu/jupiter/pdf/GeisslerP.pdf
"On the Steady State Conditions in a Circum-Jovian Satellite Accretion Disk" by Canup
http://ns1.boulder.swri.edu/jupiter/pdf/CanupR.M.pdf
"Satellite Migration and Survival" by Ward
http://ns1.boulder.swri.edu/jupiter/pdf/WardWmR.pdf
"The Io Plasma Torus" by Thomas
http://ns1.boulder.swri.edu/jupiter/pdf/Thomas.Invited.pdf
"Is the Ribbon in the Io Plasma Torus Striated?" by Dessler
http://ns1.boulder.swri.edu/jupiter/pdf/DesslerA.J.pdf
"Fine Structure of the Io Plasma Torus Produced by the Centrifugal Interchange Instability" by Goldstein
http://ns1.boulder.swri.edu/jupiter/pdf/GoldsteinJ.W.pdf
"Cassini UVIS Observations of the Radial Plasma Distribution 6 RJ – 10 RJ" by Shemansky
http://ns1.boulder.swri.edu/jupiter/pdf/Shemansky.Observations.pdf
"Probing the Three-Dimensional Structure and Time Variability of the Plasma Torus" by Smyth
http://ns1.boulder.swri.edu/jupiter/pdf/Smyth.Torus.pdf
"Io Plasma Torus:Temporal and Spatial Variability" by Bagenal
http://ns1.boulder.swri.edu/jupiter/pdf/Bagenal.pdf
"High Resolution Spectra of the Io Plasma Torus Near the Time of Galileo I24 Encounter" by Thomas
http://ns1.boulder.swri.edu/jupiter/pdf/Thomas.Poster.pdf
"Detection of Chlorine Ions in the FUSE Spectrum of the Io Plasma Torus" by Feldman
http://ns1.boulder.swri.edu/jupiter/pdf/FeldmanP.D.pdf
"Moderate-Resolution EUV Spectra of the Io Plasma Torus" by Herbert
http://ns1.boulder.swri.edu/jupiter/pdf/HerbertF.pdf
"Narrow Band Imaging of the Io Torus in the Light of Singly and Doubly Ionized Sulfur" by Jockers
http://ns1.boulder.swri.edu/jupiter/pdf/JockersK.pdf
If you have an event you would like to add here, email me at volcanopele@netzero.net.
|
Galileo Flyby of Callisto (C30) |
May 25, 2001 (123 km) |
|
AGU 2001 Spring Meeting |
May 29-June 2, 2001 |
|
Jupiter: Planet, Satellites & Magnetosphere Conference |
June 25-30, 2001 |
|
Galileo Flyby of Io (I31) |
August 6, 2001 (200 km) |
|
Galileo Flyby of Io (I32) |
October 16, 2001 (190 km) |
|
Division of Planetary Science 33rd Annual Meeting |
November 26-December 1, 2001 |
|
AGU 2001 Fall Meeting |
December 10-14, 2001 |
The Tvashtar Sun Newsletter is dedicated to provide researchers with easy and rapid access to current work regarding Io, its interior, its surface, its atmosphere, and the Io Plasma Torus.
We accept submissions for the following sections:
The format for submitting articles, abstracts, and other items is included with each issue sent by email. You can submit items to the editor by send it by email to volcanopele@netzero.net .
The Tvashtar Sun Home Page is located at http://members.fortunecity.com/volcanopele/newsletter/ .
Recent and back issues of the Newsletter are archived there in various formats. The web pages also contain other related information and links.
Tvashtar Sun is not a refereed publication, but is a tool for furthering communication among people interested in Io research and exploration. Publication or listing of an article in the Newsletter does not constitute an endorsement of the article's results or imply validity of its contents. When referencing an article, please reference the original source; Tvashtar Sun is not a substitute for peer-reviewed journals.
Expect the next issue on July 23rd.
