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Table of Contents
News and Stuf’
Editorials and Short Articles
3 Abstracts of Recently Published Papers
20 Titles or Abstracts of Accepted Papers
3 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

Imke de Pater, Franck Marchis, H. Roe, B. Macintosh, S. Acton and D. Le Mignant observed Io using Keck II's Adaptive Optics system on February 19, 20, and 22. On February 22, they observed an outburst at 334 ± 3 W, 40 ± 3 N, consistent with Surt, a plume site from Voyager 2. The J, H, and K' photometry suggests a temperature of 1000-1100 K but the H-band photometry suggests temperatures of up to 1700-1800 K, indicating ultramafic eruption. Follow-up observations are needed to look at the time evolution of this eruption.

This is the 2 major outburst in 2 months. In December 2000, Franck Marchis observed an outburst at Tvashtar Catena using the ADONIS Adaptive Optics system at the European Southern Observatory in La Silla, Chile.

Surt has been the site of short-lived eruptions before. Between the Voyager 1 and 2 encounters in 1979, a high temperature eruption may have been seen at this volcano. When Voyager 2 passed by in July 1979, a Pele-type plume deposit was seen around the volcano. Another eruption may have been seen in late March 1995. Faint activity at Surt was also noted in June 1996.

More information can be found in IAUC circular #7588 at http://cfa-www.harvard.edu/iauc/07500/07588.html. Figure 1 below shows Surt and a nearby volcano, Manua Patera. This image is based on Voyager 1 data.

John Spencer observed Io on January 16 and 18 and found that activity at Loki was pretty constant and that Tvashtar was fainter than when it erupted in December 2000.

Speaking of Tvashtar, John Spencer reported on the IJW Satellites mailing list preliminary information on images taken of Tvashtar by Galileo and Cassini in December 2000 and January 2001. Galileo images show a large, red plume deposit surrounding Tvashtar, similar in size and shape to that seen at Pele. Cassini observed a large, Pele-type plume at Tvashtar during this same time. This new plume and subsequent deposits appear to stem from an outburst seen at Tvashtar by Franck Marchis on December 16.

In the next couple of years, Galileo will take a dive into Io's mammoth parent, Jupiter, ending the mission. With the exception of possible opportunistic observations by the Europa Orbiter in 10 years hence, no mission to Io is currently planned. However, in the last couple of years, several missions have been proposed. One mission, known as Firebird, would consist of a Discovery-class flyby mission, which would take 50 Gbits of data in one pass of Io. Another mission, known as Volcan, would consist of a Discovery-class spacecraft, like Firebird. Unlike Firebird, Volcan would orbit Jupiter and flyby Io four to six times for better temporal and spatial coverage. Building on that idea, John Spencer, William Smythe, Rosaly Lopes-Gautier, and Alfred McEwen today proposed a possible mission to Io at the Forum on Innovative Approaches to Outer Planetary Exploration: 2001-2020 in Houston, Texas. This proposal would orbit Jupiter like Volcan but obtain more data over a longer period of time than either Firebird or Volcan. The importance of Io as a model for the geology of early Earth and the interior of Europa was emphasized at the talk.

Article: http://members.fortunecity.com/volcanopele/news022001.htm

Abstract for conference talk: http://www.lpi.usra.edu/meetings/outerplanets2001/pdf/4076.pdf

Several new Io images were released on February 27, 2001. These images included a mosaic and topographic model of Tohil Mons, a map of surface changes on the Amirani flow field between October 1999 and February 2000, and a comparative images showing Tvashtar in November 1999 and February 2000. These images are available at http://pirlwww.lpl.arizona.edu/Galileo/Releases/ .

It takes a lot of stress, and a little chaos, to create some of the tallest mountains in our solar system. That is the theory proposed by earth and planetary scientists at Washington University in St. Louis studying mountain formation and volcanic activity on Io, one of Jupiter's many moons. The researchers analyzed images taken by the Galileo and Voyager spacecraft and found that Io’s enigmatic mountains may be the combined result of heating, melting, and tilting of giant blocks of crust.

The origin of Io's prodigious mountains has intrigued planetary scientists for over 20 years. Io, about the size of Earth's moon, is the most geologically active body in the solar system, with mountains up to 55,000 feet tall (the summit of Mt. Everest is a meager 29,000 feet). Io's surface is dotted with active volcanoes spewing plumes of sulfurous gas and emitting vast streams of scorching lava. The heat released from Io -- from lavas as hot as 1,800 Kelvin or 2,800 degrees Fahrenheit -- is about 25 to 30 times greater per square foot than the heat released from Earth. This makes Io's mountains, which are not themselves volcanoes, all the more interesting, because at these temperatures planetary scientists would expect the surface to be liquid or soft, with little topography to speak of.

The rest of the news release is available at http://members.fortunecity.com/volcanopele/news022701.htm

By Jason Perry

At the upcoming Lunar and Planetary Sciences Conference and in the upcoming JGR-Planets special section on the geology of Io, several mountain formation methods will be proposed in addition to some already proposed. Many of these models have quite a few similarities. Some models contradict one another; most models debunking another model through whatever methods the authors used to determine their models. There are four main theories for Ionian mountain formation or orogenesis. Turtle et al. propose that mountains are formed when diapirs, or large upwellings of magma in Io’s mantle, imping on the crust, forming mountains due to enhanced compressive stresses above the diapir. Jaegar et al. propose that subsidence and thermal expansion provide stresses that cause mountain formation, but, like the model proposed by Turtle et al., diapirs impinging on focus these stresses randomly over the surface. McKinnon et al. (2001) propose that mountains are formed in areas where volcanic activity has waned, raising the thermal stresses in these areas. Schenk and Balmer (1998) proposed that compression in Io’s crust due to its high resurfacing rate create mountains.

Io has as many as 150 mountains spread roughly even across its surface with a slight abundance in the northern leading hemisphere. The tallest mountain is the "south peak" of Boosaule Montes northwest of Pele, which reaches at height of 17 km. Many mountains reaches heights of 5-10 km, though some, which are best described as raised plateaus rather than true mountains, reach heights of 2-4 km. The mountains we see today are all in various stages of death. Some, like Euboea Montes and "Gish Bar Mons," are quite young and have prominent debris aprons near them. These debris aprons, though indicative of decay and mass wasting, indicate the mountains relative youth because they have not been covered by lava or, to any real measure, volatiles. Others, like Ot Mons, "Monan Mensa" and Skythia Mons, are quite old and have lost their angular peaks and thick, extensive debris fields. Though Monan’s deposit is still noticeable, it is not as thick as the deposits seen at Euboea or Gish Bar. A few mountains, like Ionian Mons, Mongibello Mons, "Pillan Mons," Hi’iaka Montes, and Danube Planum, shows signs of extension as the mountains have rifted down the center of the mountain, sometimes spliting the mountain in two, like at Hi’iaka Montes. Studies by Jaeger et al. show that about 40% of mountains on Io have volcanoes very close to them, indicating a close association between these mountains and volcanoes. Despite this, McKinnon et al. (2001) show that that an area of increased mountain concentration in the northern half of leading hemisphere is anti-correlated with concentrations of volcanoes at the sub- and anti-jovian points.

In 1998, Schenk and Bulmer proposed that Io’s mountains were tilted crustal blocks formed by compressive stresses in the crust. The compressive stresses are caused by Io’s high resurfacing rate, which creates compressional shortening in the crust. Mountain formation is triggered in this model along thrust faults to relieve the crust of these stresses by weaknesses in the crust near volcanoes or by anisotropies in the crust.

In a recent paper, McKinnon et al. (2001) propose a model of mountain formation based on thermal stresses. When volcanic activity wanes in a region, thermal stresses build up causing thrust faults. Heat buildup in the lower parts of the crust cause thermal uplift to occur, forming mountains. The thermal stresses are relieved when volcanic activity commences in the process. This model of mountain formation is analogous to the formation of chaos on Europa. The authors of McKinnon et al. (2001) used distribution maps of volcanoes and mountains as evidence to support their model. Mountains have higher concentration in the northern leading hemisphere and northwest of Pele (near Boosaule Montes) while volcanoes have higher concentrations near the sub- and anti-jovian points. Volcanoes seem to be less concentrated in the areas where there are higher concentrations of mountains. This would seem to indicate that mountains form where volcanic activity has waned.

Turtle et al. will propose at the upcoming Lunar and Planetary Sciences Conference and in the upcoming JGR-Planets special section that Io’s mountains are formed when diapirs imping on the lithosphere creating increased compressive and thermal stresses, inducing thrust faults and mountains. This model explains several features seen in mountains. First, some mountains on Io have rifts splitting the mountain. Diapirs imping on the lithosphere would create extensional faults immediately above them. If a mountain were right above it, it would be split apart. A diapir would also create a lot of magma and create quite a bit of pressure on the crust. To relieve the pressure, magma could use the faults it created and erupt on the surface near the mountains. Indeed, many mountains have volcanoes close to them and these volcanoes appear to be tectonically controlled. One example of this can be seen at Zal Patera where lava issues from a fault west of N. Zal Montes.

A final theory will be proposed by Jaeger et al. at the upcoming Lunar and Planetary Sciences Conference and in the upcoming JGR-Planets special section. This model is very similar to the Turtle et al. model. Like the last model, diapirs imping on the crust give the spark for forming mountains. However, rather than compression and thermal stresses as the primary stresses that form faults in Io’s crust, a combination of subsidence and thermal stress create the faults in Io’s crust. Mantle plumes focus these stresses to form mountains.

These four theories are by no means the last word in how mountains on Io form. New observations over the next year could propel one model as the accepted theory or force a new model to be made. What ever creates these mysterious structures, Galileo did show that mountains on Io meet similar fates, to be shaken to nothing more than a raised plateau of rounded hills.

By Jason Perry

Jupiter Odyssey, written by David Harland (Exploring the Moon: The Apollo Expeditions), describes not only the journey of Galileo through the inner solar system and Jovian system, but also the worlds it explored. Harland does this masterfully. Ever world, no matter how small or seemingly insignificant, is described in full detail as though Harland and each of us were with Galileo, along for its magnificent voyager. The book starts with a brief description of the trials and tribulation that Galileo went through before it got off the ground. Thankfully, Harland moves on fairly quickly through this and gets to the real meat of the Galileo story, the wonderful worlds it saw. From the asteroids Ida and Gaspra, to the Shoemaker-Levy 9 impact, and finally to encounter day, the cruise of Galileo is described in great detail. The probe mission is discussed in also discussed in great detail, much of it I had never known. Finally, the mission in the Jovian mission is discussed by world or set of worlds. In the end, a brief description of the Cassini mission is given.

This book is the best overview of any planetary mission I have read. Harland describes the mission is such a way that it seems as grand as the Apollo missions he discusses in his previous book. I did have two problems with the book for which the author can not be blamed. First, though the book is heavily illustrated, the images are in black and white, which for some images makes them hard to interpret. Secondly, the book was published before the mission was completely over. This is in no way Harland’s fault. The Galileo spacecraft has survived much more than it was designed to survive, stubbornly resisting the punishment its operators put it through. The spacecraft continues on, slightly used, and now we have a great chronicle of its journey to read.

Mountains are distributed across the surface of Io, the fiercely tidally heated moon of Jupiter. The large crustal thicknesses implied by their great heights can be reconciled with Io’s high heat

flow, if most of the heat escapes directly via volcanic eruptions (the heat-pipe model), but the origin of the mountains has remained obscure. Recent images show that many of Io’s mountains are tilted blocks undergoing tectonic collapse, and we propose here that the volcanic heat-pipe (and continuous terrain burial) model naturally leads to such unstable topography. That is, burial (1) generates horizontal tensile stresses as the volcanic crustal stack is loaded, (2) creates large horizontal compressive confining stresses as Io’s crust subsides (moves to a smaller effective radius), and importantly, (3) allows for potentially large horizontal compressive thermal stresses as the base of the crust reheats owing to fluctuations in the efficiency of the volcanic heat piping. Faulting associated with these stresses may raise mountain scarps directly or in concert with thermal uplift due to the crustal reheating; continued crustal heating and melting then lead to mountain collapse (all over ,1 m.y. to a few million years). Our model predicts that regions

of active mountain formation and volcanic activity on Io should be anticorrelated, which is observed. Moreover, substantial tidal heating and disruption of planetary crust are seen elsewhere in the Jupiter system, in the chaos terrains of Europa. There may be stronger commonalities between the two inner jovian moons (and early Earth) than previously realized.

For reprints, contact mckinnon@levee.wustl.edu .

We analyze a collection of hyperspectral images of Io acquired by the near infrared mapping spectrometer (NIMS) of Galileo during the G2 to E16 orbits of Jupiter. This analysis leads to the geographical distribution and physical characterization of SO₂ frost deposits over about three-fourths of Io's surface. These deposits are excellent tracers of various phenomena, including volcanic production and emission, atmospheric transportation, condensation, metamorphism, irradiation, and sublimation, that occur throughout the SO₂ cycle. We assume that the deposits of solid SO₂ are optically thick and are geographically mixed with other sulfur-bearing compounds. We first assess the mean moderate backscattering behavior of the SO₂ frost (Henyey Greenstein phase function parameter g=-0.27±0.05) using a sequence of spectra at two different locations over a large range of phase angles. This behavior may indicate a granular texture with many defects or a fluffy texture. Second, a more systematic inversion of the hyperspectral images is achieved based on a linear spectral model of pure SO₂ with variable grain size mixed with a spectrally neutral unit. As a result, we produce two global mosaics that map SO₂ frost coverage and mean grain size. SO₂ deposits are omnipresent on Io's surface at the spatial scale of this study (~200 km), but the SO₂ frost is concentrated within several large areas centered at medium latitudes. These SO₂-rich regions (surface coverage higher than 60%) show a longitudinal correlation with plumes located lower in latitude, suggesting that these plumes are the principal sources of SO₂ gas. After a possible dynamic condensation around the plumes or at the equator, the gas is remobilized by the solar or thermal fluxes and flows mostly latitudinally toward the coldest and nearest regions devoid of hot-spots. Third, the correlation of the distribution and grain size mosaics distinguishes four different SO₂ physical units that indicate relative regional variations of condensation, metamorphism, and sublimation. Finally, comparisons with Voyager ultraviolet (A. S. McEwen, T. V. Johnson, D. L. Matson, and L. A. Soderblom, 1988, Icarus, Vol. 75, pp. 450-478) and Galileo visible (P. Geissler, A. S. McEwen, L. Keszthelyi, R. M. C. Lopes-Gautier, J. Granahan, and D. P. Simonelli, 1999, Icarus, Vol. 140, pp. 256-282) observations demonstrate molecular contamination of SO₂ at medium and high latitudes and that these contaminated SO₂ deposits may be optically thin.

¹ Department of Earth and Space Sciences, University of California, Los Angeles, 595 Charles Young Drive East, Los Angeles, California, 90095-1567.
2 Earth Sciences Department and Institute of Geophysics and Planetary Physics, University of California, Santa Cruz, 1156 High Street, Santa Cruz, California, 95064
3 Lunar and Planetary Institute, 3600 Bay Area Boulevard, Houston, Texas, 77058
4 Space Geodetic Science and Applications Group, Jet Propulsion Laboratory, 4800 Oak Grove Drive, MS 238-332, Pasadena, California, 91109-8099
5 Ecole Normale Superiere, Lyon, France

Io has very high surface heat flow and an abundance of volcanic activity, which are thought to be driven by nonuniform tidal heating in its interior. This nonuniform heat is transported to the base of the lithosphere by very vigorous convection in Io's silicate mantle, the form of which is presumably responsible for the distribution of surface features such as volcanoes and mountains. We here present three-dimensional spherical calculations of mantle convection in Io, in order to ascertain the likely form of this convection and the resulting distribution of heat flow at the surface and core-mantle boundary. Different models of tidal dissipation are considered: the endmember scenarios identified by M. N. Ross and G. Schubert (1985, Icarus 64, 391-400) of dissipation in the entire mantle, or dissipation in a thin (~100-km-thick) asthenosphere, as well as the "preferred" distribution of M. N. Ross et al. (1990, Icarus 85, 309-325) comprising 1/3 mantle and 2/3 asthenosphere heating. The thermal structure of Io's mantle and asthenosphere is found to be strongly dependent on tidal heating mode, as well as whether the mantle-asthenosphere boundary is permeable or impermeable. Results indicate a large-scale flow pattern dominated by the distribution of tidal heating, with superimposed small-scale asthenospheric instabilities that become more pronounced with increasing Rayleigh number. These small-scale instabilities spread out the surface heat flux, resulting in smaller heat flux variations with increasing Rayleigh number. Scaled to Io's Rayleigh number of O (10¹²), variations of order a few percent are expected. This small but significant variation in surface heat flux may be compatible with the observed distributions of volcanic centers and mountains, which appear fairly uniform at first sight but display a discernible distribution when suitably processed. The observed distribution of volcanic centers is similar to the asthenosphere heating distribution, implying that most of the tidal heating in Io occurs in an asthenosphere.

For reprints, contact: ptackley@ucla.edu .

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.

For Preprints, contact: rhowell@uwyo.edu

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.

For Preprints, contact: lpk@LPL.arizona.edu

For preprints, contact: jani@LPL.arizona.edu

For Preprints, contact: turtle@lpl.arizona.edu

For Preprints, contact: jmoore@mail.arc.nasa.gov

For Preprints, contact: fmarchis@astron.berkeley.edu

For Preprints, contact: windy@lpl.arizona.edu

For Preprints, contact: dwilliams@dione.la.asu.edu

For Preprints, contact: rlopes@lively.jpl.nasa.gov

For Preprints, contact: geissler@lpl.arizona.edu

For Preprints, contact: dwilliams@dione.la.asu.edu

For Preprints, contact: L.Wilson@lancaster.ac.uk

For Preprints, contact: simonelli@cuspif.tn.cornell.edu

For Preprints, contact: mmilazzo@pirl.lpl.arizona.edu

1 Planetary Science Research Group, Environmental Science Division, Lancaster University, Lancaster LA1 4YQ, UK

For preprints, contact: leone@unix.lancs.ac.uk

For preprints, contact: moses@lpi.usra.edu

For Preprints, contact: moses@lpi.usra.edu

For Preprints, contact: simonelli@cuspif.tn.cornell.edu

Jupiter Planet, Satellites & Magnetosphere

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:

• Origin of the Satellites
• Plasma Tori & Dust
• Plasma-Satellite Interactions
• Orbital and Rotational Dynamics of Satellites
• Satellite Interiors
• Io Surface Processes
• Satellite Atmospheres

For more information on this conference, go to http://lasp.colorado.edu/jupiter/index.html or contact JupMeet@lasp.colorado.edu

Houston, Texas

March 12-16, 2001

The 32nd Lunar and Planetary Science Conference will be held in Houston, Texas, on March 12–16, 2001. Technical sessions will be held at the NASA Johnson Space Center (JSC) and at the University of Houston-Clear Lake. The conference encompasses all aspects of planetary science. Abstracts and the final announcement are now available on the web.

For more information on this conference, go to http://www.lpi.usra.edu/meetings/lpsc2001/index.html.

Boston, Massachusetts

May 29-June 2, 2001

For more information on this meeting go to:

http://www.agu.org/meetings/sm01call.html.

S.M. Baloga and L.S. Glaze

http://www.lpi.usra.edu/meetings/lpsc2001/pdf/1306.pdf

V. Cataldo and L. Wilson

http://www.lpi.usra.edu/meetings/lpsc2001/pdf/1553.pdf

W.L. Jaeger, E.P. Turtle, L.P. Keszthelyi, and A.S. McEwen

http://www.lpi.usra.edu/meetings/lpsc2001/pdf/2045.pdf

D.L. Matson, A.G. Davies, G.J. Veeder, D.L. Blaney, and T.V. Johnson

http://www.lpi.usra.edu/meetings/lpsc2001/pdf/1968.pdf

Tentative Identification of Local Deposits of Cl2SO2 at Io’s Surface

B. Schmitt and S. Rodriguez and the NIMS Team
http://www.lpi.usra.edu/meetings/lpsc2001/pdf/1710.pdf

J.C. Granahan et al.
http://www.lpi.usra.edu/meetings/lpsc2001/pdf/1650.pdf

R. Lopes-Gautier et al.
http://www.lpi.usra.edu/meetings/lpsc2001/pdf/2021.pdf

A.G. Davies and the Galileo NIMS Team
http://www.lpi.usra.edu/meetings/lpsc2001/pdf/1474.pdf

M.Y. Zolotov and B. Fegley
http://www.lpi.usra.edu/meetings/lpsc2001/pdf/1456.pdf

J.A. Rathbun et al.
http://www.lpi.usra.edu/meetings/lpsc2001/pdf/2036.pdf

S. Douté et al.
http://www.lpi.usra.edu/meetings/lpsc2001/pdf/1929.pdf

M. Milazzo et al.
http://www.lpi.usra.edu/meetings/lpsc2001/pdf/2088.pdf

J. Radebaugh et al.
http://www.lpi.usra.edu/meetings/lpsc2001/pdf/2088.pdf

D.A. Williams et al.
http://www.lpi.usra.edu/meetings/lpsc2001/pdf/1220.pdf

L. Keszthelyi et al.
http://www.lpi.usra.edu/meetings/lpsc2001/pdf/1523.pdf

V. Cataldo et al.
http://www.lpi.usra.edu/meetings/lpsc2001/pdf/1555.pdf

B.A. Archinal et al.
http://www.lpi.usra.edu/meetings/lpsc2001/pdf/1746.pdf

by R.R. Wilson and P.M. Schenk
http://www.lpi.usra.edu/meetings/lpsc2001/pdf/1834.pdf

E.P. Turtle et al.
http://www.lpi.usra.edu/meetings/lpsc2001/pdf/2104.pdf

M.P. Milazzo et al.
http://www.lpi.usra.edu/meetings/lpsc2001/pdf/2089.pdf

W.D. Smythe et al.
http://www.lpi.usra.edu/meetings/lpsc2001/pdf/2129.pdf

A. McEwen et al.
http://www.lpi.usra.edu/meetings/lpsc2001/pdf/1824.pdf

M. Monnereau and F. Dubuffet
http://www.lpi.usra.edu/meetings/lpsc2001/pdf/1784.pdf

If you have an event you would like to add here, email me at volcanopele@netzero.net.

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:

• Abstracts of accepted and recently published paper
• Titles of submitted (but not yet accepted) papers and conference articles
• Thesis abstracts
• Short articles, announcements, or editorials
• Status reports of on-going programs
• Requests for collaboration or observing coordination
• Table of contents/outlines of books
• Announcements for conferences
• Job advertisements
• Volcano News
• General news items deemed of interest to the Io community

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.

Pillanian News 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.

In Issue 3,

• An article on Tvashtar: the myth, the volcano, the plume
• A look at the upcoming JGR-Planets special section
• A preview of the C30 encounter
• A review of lessons learned from the Cassini flyby

Expect the next issue on May 21^st.

Written by Jason Perry
March 7, 2001

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