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Volume 1, Number 1
January 2001
Table of Contents
News and Stuf’
Editorials and Short Articles
6 Abstracts of Recently Published Papers
2 Titles of Accepted Papers
10 Titles of Submitted Papers
Table of Contents of Books
Conference Annoncements
Recent Conference Abstracts
Upcoming Events
Newsletter Info
In the Next Issue...
This is the premier issue of Pillanian News. The idea of a newsletter for the Io community is not an old one. The Galileo Project had a newsletter until a few years ago. The International Jupiter Watch Satellite Discipline had a newsletter called Ole Roemer (after the 17th century Danish astronomer Olaus Roemer) until 1996. But over the last 3-4 years, there has been no newsletter to carry the torch. I created this newsletter in December 2000 as a possible way to fill that gap. I have been bouncing around the idea of creating an Io newsletter for several months now but never felt it was the right time to do so. Now as we begin a new millennium and head toward another renaissance of Ionian exploration, I feel now is the right time to start an Io newsletter. The name of the newsletter is not as good as I hoped but since it appears that it has stuck, meaning I see people putting it into search engines to find my home page and this newsletter, I guess it will have to stay.
As most of you know by now, the newsletter does have a website now. It is located at http://members.fortunecity.com/volcanopele/newsletter/index.html . This website includes information on submitting articles and abstracts, subscribing (if you are reading this on the website), and on the newsletter itself. On the website you can find current and past issues of the newsletter as they are posted. They come in four different file formats for your convience: PDF, Microsoft Word, PostScript, and HTML. The version sent to subscribers is the PDF version.
One of the first things people ask me is, "Are you really 17?" Yes, I am really 17. I really am a high school junior. I really do watch the Simpsons. Second thing people ask me is, "Why are you so interested in Io?" That’s a much tougher question. I have been interested in Io since the 7th grade. I guess what got me interested in Io is all the neat colors displayed on the surface and the fact that stuff happens every day on Io, not just billions of years ago like on Dione or something (though those wispy markings might be something interesting). I have always been interested in space and since I was 5 I was always reading and watching stuff about space. It was never an "I want to be an astronaut"-type thing. I was always interested in what was going on on other worlds. Disappointed that for the most part the answer was "not much," I became interested in the worlds were "stuff" was going. These worlds included Io, Triton, and Venus. Since the Galileo mission was just beginning and images showing "stuff" going on started coming in, my primary interest was Io. Over the years, I learned more and more about Io and became more and more interested in Io. This interest led to my website and now this newsletter. This summer, that interest will lead me to Arizona to work with Dr. Alfred McEwen and his team of researchers down at the University of Arizona. With a little luck, a nice essay, and a better grade in AP Calculus, I hope that I come back the next summer.
I hope you learn a little something from this first newsletter. There are still a few kinks to work out, mainly due to the short notice I gave people about the first issue of the newsletter, but by issue two these will be worked out. Two final notes, first concerns the JGR-Planets Io Special section. I am looking for a current listing for what will be in this issue. I know that these papers have not been accepted so I am not looking for abstracts, just titles and authors. Second, if you haven’t visited my Io Website, called the Ionian Web, I encourage you to do so. Its got tons of information that you will not find in any of those overview pages. My website has scientific articles, articles I have written myself, a VERY large Io image and movie gallery, science fiction stories concerning Io, a page where you can buy books and DVDs concerning Io (any of you ever seen Outland which takes place on Io), news articles, maps of Io from Galileo, to Voyager, to the 1961 A. Dollfus map of Io, an extensive links page, and a page with information on Galileo’s 7 flybys of Io. My website is located at http://members.fortunecity.com/volcanopele/index.html .
Three data sets of Io (composed of 3 or 4 final processed images in L' band) were taken, for each of them we have a PSF data set. On the 5 hours of observation, wee can not only determine the center-to-limb variation of any bright hot spots, but we also increase the spatial coverage of our survey. After applying a deconvolution process (called MISTRAL, see Conan et al., SPIE, 4007, 913-924), we can identify several well-known hot spots. The brightest one on this side seems to correspond to Loki (309W, 13N). Furthermore, the emission is quite extended in direction of Daedalus and the center-to-limb variation do not follow a classical cosine theta law. One basic interpretation could be the presence of another hot spot close to Loki which may contaminate the flux calculated. The flux estimated on the images with Loki nearest the central meridian indicates a vertical brightness of 85±10 GW/Sr/µm (similar the medium activity determined in September 1998).
Another important active area corresponds to the Janus-Kanehikili (J-K) group
which approximately follows a cosine theta law and is estimated to have
a vertical brightness of 46±10 GW/Sr/µm.
We also isolated other possible sources of emission on the last data set (SEP
longitude=3°). Two eastern limb emissions correspond to Hi'iaka and Gish
Bar. Two unknown faint emissions are located on the internal disc: one at the
NW (astronomical) of J-K (0011A) located at (27±10°W, 20±7°N)
and another one (0011B?) close to the northern pole (55±15°W,
58±15°N). In our previous survey, this part of the Io surface has
been poorly imaged (near-limb geometry). Therefore, it is not possible to compare
and confirm the presence of such emissions. Sengen Patera area seems not to
be active on our data (close-limb position).
Other broad band observations (L and M) will be processed soon. They will allow
to better constrain the nature and temperature of emission.
For More information and images: http://astron.berkeley.edu/~fmarchis/Io_OA/Run2000/
Contact: fmarchis@astron.Berkeley.edu
John Spencer and coworkers had two successful IRTF Io runs on December 24 and 29, 2000 and report that Loki is at moderate brightness (32 GW/µm/str at 3.5 microns), with nothing else unusual happening on the Jupiter-facing hemisphere.
John Spencer stepped down as head of the IJW Satellite Discipline on January 4. Robert Howell is now the new head of the discipline. To reflect this, the Discipline's website has moved to http://goshawk.uwyo.edu/ijw . Please update your bookmarks to reflect this change.
Here is a list of news articles on the internet from the last two months:
491st Anniversary of Io's Discovery
Probably the most significent contribution that Galileo Galilei made to science was the discovery of the four satellites around Jupiter that are now named in his honor. Galileo first observed the moons of Jupiter on January 7, 1610 through a homemade telescope. He originally thought he saw three stars near Jupiter, strung out in a line through the planet. The next evening, these stars seemed to have moved the wrong way, which caught his attention. Galileo continued to observe the stars and Jupiter for the next week. On January 11, a fourth star (which would later turn out to be Ganymede) appeared. After a week, Galileo had observed that the four stars never left the vicinity of Jupiter and appeared to be carried along with the planet, and that they changed their position with respect to each other and Jupiter. Finally, Galileo determined that what he was observing were not stars, but planetary bodies that were in orbit around Jupiter. This discovery provided evidence in support of the Copernican system and showed that everything did not revolve around the Earth.
For more information: http://www.jpl.nasa.gov/galileo/ganymede/discovery.html
Cassini Encounter with Jupiter/Io
NASA's $3.4 billion Cassini spacecraft passed Jupiter at the closest point of its trip Saturday, using gravity from the solar system's largest planet to swing it toward Saturn. While passing Jupiter over the next few months, Cassini will team up with the Galileo spacecraft to make dual observations of the planet and its surroundings.
For more information: http://dailynews.yahoo.com/h/ap/20001230/sc/cassini_jupiter_1.html
Cassini Images of Io
Jupiter and Io Observe Each Other
http://members.fortunecity.com/volcanopele/cassini121100.htm
Io in front of Jupiter
http://members.fortunecity.com/volcanopele/cassini122000.htm
Io: Jupiter’s Volcanic Moon
Educational Website
An educational website devoted exclusively to the study of Io has been created.
"Io: Jupiter’s Volcanic Moon" provides an in depth examination of
the volcanic features and processes on Io, including plume eruptions, lava flows,
tidal heating, the Io plasma torus, and much more. The site provides up-to-date
information from JPL and NASA, and the latest images of Io taken by the Galileo
spacecraft.
A special feature of the website is an eleven page photoglossary. These pages
define through photographs, illustrations, and text, some of the scientific
terms and geological concepts used throughout the site which may be unfamiliar
to some users. Examples include planetary magnetosphere, aurora, shield volcano,
and lava tubes.
The site was created and is maintained by Janet Wood, a graduate student in
geoscience education at Mississippi State University. The website is appropriate
for Grades 6 and above.
"Io: Jupiter¹s Volcanic Moon" can be found at http://people.we.mediaone.net/hwood1/io/
.
Rarefied Gas Model of Io’s Sublimation-Driven Atmosphere
J. Victor Austin1, David B. Goldstein1
1 Department of Aerospace Engineering, The University of Texas at Austin, Austin, Texas, 78712
The circumplanetary flow of Io's SO2 atmosphere is modeled using the direct simulation Monte Carlo (DSMC) method. This flow develops as gas sublimates from SO2 frost in the warm subsolar region and flows toward the colder night-side, where it condenses. The axisymmetric model presented extends from the subsolar point past the terminator into the night-side. The remaining portion of the night-side atmosphere is assumed to be static. The DSMC method solves the fully viscous and compressible, non-local thermal equilibrium (non-LTE), rarefied flow problem by statistically extrapolating from the motions and collisions of representative molecules. Heating due to neutral plasma bombardment and cooling by non-LTE radiation are modeled. Quantities of a second, non-condensible gas are also added to simulate the possible effects of H2S or O2 in the atmosphere.
It is found that, except in the subsolar region, the flows are predominately rarefied. For high subsolar temperatures, the atmospheric flow may become supersonic and then decelerate through a diffuse, oblique shock upstream of the terminator. Appreciable local condensation occurs below the shock while the atmosphere above the shock is significantly inflated. These hydrodynamic features, among others, have implications for the observations of frost cover, atmospheric flow, and the ionosphere.
Published in: Icarus 148, 370-383 (2000)
For reprints, contact victor@cfdlab.ae.utexas.edu
.
Adaptive Optics Mapping of Io’s Volcanism in the Thermal IR (3.8 µm)
Franck Marchis1,2, Renée Prangé2, Julian Christou3
1 European Southern Observatory, Casilla 19001, Santiago, 19,
Chile
2 Institut d'Astrophysique Spatiale, Université Paris Sud, Orsay, France
3 Starfire Optical Range, U.S. Air Force Research Laboratory, Kirtland, New
Mexico, 87117
Two opposite hemispheres of Io were observed on October 20 and 21, 1996, through an L' broadband filter, using the high-resolution capability of the Adaptive Optics (AO) system implemented on the ESO 3.6-m telescope at La Silla, Chile. These observations, performed at thermal wavelengths when Io is in daylight, have been carefully processed to improve the sharpness of the initial, diffraction-limited, images. The myopic deconvolution process used (idac) achieved an angular resolution estimated to be 0.15 arcsec, corresponding to a spatial resolution of ~570 km on Io's disc at the time of the observations. The final images show a number of bright features which have been compared with the Galileo/NIMS data, the only data set with a comparable resolution available for the anti-Jovian side of the satellite as well as its Jupiter-facing side. Our maps of the hot spot distribution are quite consistent with the Galileo data. The Jupiter-facing side is dominated by emission from Loki, which accounts for ~25% of the total hot spot emission from that side (and 45% of that we were able to resolve and identify), although Loki was in a phase of decreasing activity (but not yet quiescent), as derived from ground-based monitoring observations. A few more hot sources are detected, including Pele-Pillan. The other hemisphere is characterized by a large number of moderately bright hot spots which are distributed around Bosphorus Regio. These preliminary observations fully demonstrate the capabilities of an AO system coupled with a thermal camera to monitor the volcanic activity of Io, in terms of morphology as well as thermal output. These monitoring capabilities will become especially important when the Galileo mission ends.
Published in: Icarus 148, 384-396 (2000)
For reprints, contact fmarchis@eso.org
.
Color and Morphology of Lava Flows on Io
Jennifer L. Piatek1, Sarah B. Z. McElfresh1, Jeffrey M. Byrnes1, Amy Snyder Hale2, David A. Crown1
1 Department of Geology and Planetary Science, 321 Engineering
Hall, University of Pittsburgh, Pittsburgh, Pennsylvania, 15260
2 Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA.
Analyses of color and morphologic changes in Voyager images of lava flows on Io were conducted to extend previous flow studies to additional volcanoes in preparation for comparison to Galileo data. Blue and orange filter images of Atar, Daedalus, and Ra Paterae were examined to identify systematic downflow decreases in blue/orange reflectivity suggested in earlier studies as diagnostic of color changes in cooled sulfur flows. Analyses of the color and morphology of 21 lava flows were conducted at these volcanoes, with additional morphologic analysis of lava flows at Agni, Masaaw, Mbali, Shoshu, and Talos Paterae. A total of 66 lava flows of up to 245 km in length were mapped to identify morphologic changes consistent with the rheologic changes expected to occur in sulfur flows. Although downflow color changes are observed, the trends are not consistent, even at the same edifice. Individual flows exhibit a statistically significant increase in blue/orange ratio, decrease in blue/orange ratio, or a lack of progressive downflow color variation. Color changes have similar magnitudes downflow and across flow, and the color ranges observed are similar from volcano to volcano, suggesting that similar processes are controlling color ratios at these edifices. In addition, using flow widening and branching as an indicator of the low viscosity exhibited by sulfur cooling from high temperatures, these flows do not exhibit morphologic changes consistent with the systematic behavior expected from the simple progressive cooling of sulfur.
Appeared in: Icarus 148, 407-418 (2000)
For reprints, contact lpst81@pitt.edu
.
Bruce Fegley Jr.1, Mikhail Yu. Zolotov2
1 Planetary Chemistry Laboratory, Department of Earth and Planetary
Sciences, Washington University, St. Louis, Missouri, 63130-4899
2 Department of Earth and Planetary Sciences, Washington University, St. Louis,
Missouri, 63130-4899
We used thermochemical equilibrium calculations in the O-S-Na-K-Cl-H system to model the speciation of volcanic gases emitted from high-temperature (1000-2000 K) silicate magmas on Io. The effects of temperature, pressure, and bulk composition of the gases are explored. The bulk compositions are based on atomic ratios observed in Io's plasma torus and extended atmosphere, and from chondritic abundances. The results show that chlorides of Na and K are the major Cl gases, NaCl, Na, and (NaCl)2 are the major Na gases, and KCl, (KCl)2, and K are the major K gases for systems with (Na+K)/Cl>1. The abundances of Na, K, and Cl gases change dramatically at (Na+K)/Cl=1. As the (Na+K)/Cl ratio decreases below unity, which is possible for lower temperature volcanic vents, the major Cl gases change to Cl2, Cl, S2Cl, and SCl2. The results show that abundances of H-bearing gases are insignificant for plausible hydrogen abundances in Io. Higher temperatures and lower pressures increase the abundances of monatomic Na and K. Sodium, K, and Cl compounds condense as Na2S (at higher temperatures and lower O/S ratios), Na2SO4 (at lower temperatures and higher O/S ratios), and NaCl and KCl. Under some conditions, Na2SO4 and Na2S condense simultaneously. These condensates can form coatings on silicate ash particles in the vicinity of volcanic vents. Condensation temperatures decrease as pressure decreases, and condensation is not favored by low-pressure volcanic vents. Silicate magmas, especially alkaline ultrabasic magmas may be important sources of S, alkalis, and Cl on Io. Our predictions agree with spectral absorption features indicating that sodium sulfate and/or sodium sulfide may be present in red deposits on Io's surface. The two major sources of Na, K, and Cl in the plasma torus are sputtering from solid Na2S/Na2SO4/chloride surface condensates and ionization of alkali chloride and monatomic alkali gases that could be present in volcanic plumes and Io's volcanic atmosphere.
Published in: Icarus 148, 193-210 (2000).
For reprints, contact bfegley@levee.wustl.edu
.
Silicate Cooling Model Fits to Galileo NIMS Data of Volcanism on Io
Ashley Gerard Davies1, Rosaly Lopes-Gautier1, William D. Smythe1, Robert W. Carlson1
1 Jet Propulsion Laboratory-California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, 91109-8099
The Near Infrared Mapping Spectrometer (NIMS) has obtained spectra of volcanoes on the surface of the jovian satellite Io. Fits to data using a silicate cooling model allow us to constrain lava eruption rates and eruption age. The thermal signatures of the hot spots are indicative of active and cooling silicate lava flows. For large, active hot spots maximum ages of flow surfaces detected by NIMS typically range from days to months, although in one case it is nearly 30 years. Mass eruption rates for the main hot spots are in the range 7 m3 s-1 to 79 m3 s-1, using an average flow thickness of 1 m. These mass eruption rates are orders of magnitude less than those implied for large thermal outbursts on Io: the eruptions observed during June 1996 are most likely of a different eruption style, on a much smaller scale. The observation analyzed here may be representative of the current background level of volcanic activity on the anti-jove hemisphere of Io. The global mass eruption rate from these "non-outburst" hot spots is calculated to be 43 km3/year, equivalent to a global resurfacing rate of about 1 mm/year, about 10% of the minimum required global resurfacing volume. The total observed energy output from the 14 hot spots analyzed is 3.6×1012 W. Normalized globally, these hot spots contribute approximately 10% of Io's radiometric heat flux.
Published in: Icarus 148, 211-225 (2000).
For reprints, contact Ashley.Davies@jpl.nasa.gov
.
Eclipse Spectroscopy of Io's Atmosphere
Antonin H. Bouchez1, Michael E. Brown1, Nicholas M. Schneider2
1 Division of Geological and Planetary Sciences, California
Institute of Technology, Pasadena, California, 91125
2 Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder,
Colorado, 80309
High resolution optical (4193-6619 Å) spectra of Io in eclipse show auroral emission in five lines: [OI] 6300, 6363, 5577 Å and Na 5889, 5896 Å. We conclude that Io's diffuse red emissions imaged by the Galileo Solid State Imager (P. E. Geissler et al. 1999, Science 285, 870-874) are due to impact or dissociative excitation of oxygen, while diffuse green emissions are caused by the impact or dissociative excitation of sodium. No emission lines were detected in the blue region of the spectra, suggesting that the intense emission observed above Io's equatorial plumes is due to a molecular species such as SO2 or SO.
Published in: Icarus 148, 316-319 (2000).
For reprints, contact antonin@gps.caltech.edu
.
Mapping SO2 frost on Io by the modeling of NIMS
hyperspectral images
Sylvain Douté, Bernard Schmitt, Rosaly Lopes-Gautier, Robert
Carlson, Laurence
Soderblom, James Shirley, and the Galileo NIMS Team
To appear in Icarus 149, 107-132 (2001).
Three-dimensional simulations of mantle convection in Io
Paul J. Tackley, Gerald Schubrt, Gary A. Glatzmaier, Paul Schenk, J. Todd
Ratcliff and
J-P. Matas
To appear in Icarus 149, 79-93 (2001).
Photochemistry of a volcanically driven atmosphere on Io:
Sulfur and oxygen species from a Pele-type eruption
Julianne I. Moses1, Mikhail Yu. Zolotov2,
and Bruce Fegley, Jr.3
1 Julianne I. Moses, 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
Alkali and chlorine photochemistry in a volcanically driven
atmosphere on Io
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
Galileo observations of Io's disk-resolved opposition surge
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
Ground-based Observations of Volcanism on Io in 1999 and
early 2000
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
Submitted to JGR-Planets
For Preprints, contact: rhowell@uwyo.edu
Imaging of Volcanic Activity on Jupiter's moon Io by Galileo
during GEM and GMM
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, Tuscon,
AZ, 85719
2 Department of Geology, Arizona State University, Tempe, AZ, 85287
3 Center for Radiophysics and Space Research, Cornell University, Ithaca, NY,
14853
Submitted to JGR-Planets
For Preprints, contact: lpk@LPL.arizona.edu
Paterae on Io: A New Type of Volcanic Caldera?
Jani Radebaugh1, Laszlo Keszthelyi1, Alfred McEwen1, and the Galileo SSI
Team
1 Lunar and Planetary Laboratory, University of Arizona, Tuscon, AZ, 85719
Submitted to JGR-Planets
For preprints, contact: jani@LPL.arizona.edu
Mountains on Io: High-Resolution Galileo Observations, Initial
Interpretations, and Formation Models
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, Tuscon,
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
Submitted to JGR-Planets
For Preprints, contact: turtle@lpl.arizona.edu
Landform Degradation and Slope Processes on Io: The Galileo
View
Jeff Moore1, Robert J. Sullivan2, Frank Chuang3, James Head III 4, 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, Tuscon, AZ, 85719
6 Lunar and Planetary Institute, 3600 Bay Area Boulevard, Houston, TX, 77058
Submitted to JGR-Planets
For Preprints, contact: jmoore@mail.arc.nasa.gov
Io's Volcanism by adaptive optics observations in the 3.8
micron thermal band
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
Submitted to JGR-Planets
For Preprints, contact: fmarchis@astron.berkeley.edu
Orogenic and Post-Orogenic tectonism on Io
Windy Jaeger1, Elizabeth Turtle1, Laszlo Keszthelyi1, J. Radebaugh1, and
Alfred McEwen1
1 Lunar and Planetary Laboratory, University of Arizona, Tuscon, AZ, 85719
Submitted to JGR-Planets
For Preprints, contact: windy@lpl.arizona.edu
Jupiter Odyssey: The Story of NASA's Galileo Mission
By David Harland
I will be reviewing this book next issue but I decided to present the table of contents here this issue. This book came out in November 2000 and most people seem to be giving it rave reviews.
1. Early Days.............................1
2. Reconnaissance..................5
3. Galileo's Ordeal..................20
4. An Exploring Machine.......27
5. The Long Haul...................45
6. Target in Sight...................89
7. Atmospheric Probe.........111
8. The Capture Orbit...........128
9. Tectonic Ganymede.......133
10. Battered Callisto...........163
11. Europan Enigma...........183
12. Jupiter from Orbit..........249
13. Moonlets and rings.......283
14. Fiery Io............................291
15. Passing the torch..........361
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:
For more information on this conference, go to http://lasp.colorado.edu/jupiter/index.html or contact JupMeet@lasp.colorado.edu
32nd Lunar and Planetary Science Conference
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 will be posted on their website on February 2, 2001.
For more information on this conference, go to http://www.lpi.usra.edu/meetings/lpsc2001/index.html.
2000 AGU Fall Meeting
Io as a Plasma Source in the Jovian System
Russell, C T
http://www.agu.org/cgi-bin/SFgate/SFgate?&listenv=table&multiple=1&range=1&directget=1&application=fm00&database=/data/epubs/wais/indexes/fm00/fm00&maxhits=200&=%22P62D-02%22
Comparison of Torus Conditions Observed by HST and Galileo
F Bagenal, N M Schneider, L A Frank, W R Paterson, F Herbert, A Hendrix,
J Weiss
http://www.agu.org/cgi-bin/wais?q=P62D-03
Passage Through Io's Ionospheric Plasmas by the Galileo Spacecraft
W R Paterson, L A Frank
http://www.agu.org/cgi-bin/wais?q=P62D-04
On the Plasma Distribution in the Polar Regions of the Galilean Satellites,
particularly Io: Field-aligned Plasma Motion
F M Neubauer
http://www.agu.org/cgi-bin/wais?q=P62D-05
MHD Modeling of Io's Magnetic and Plasma Environment
J A Linker, M G Kivelson, R J Walker
http://www.agu.org/cgi-bin/wais?q=P62D-06
Io: In-Your-Face Active Geology
A McEwen, L Keszthelyi, E Turtle, M Milazzo, J Radebaugh, W Jaeger, P Geissler,
D Simonelli, D Williams, J Moore, C Phillips, G SSI Team
http://www.agu.org/cgi-bin/wais?q=P62D-07
Galileo at Io: New Results from the Near-Infrared Mapping Spectrometer
R Lopes-Gautier, S Doute, L Kamp, W Smythe, R Carlson, A Davies, A McEwen,
P Geissler, S Kieffer, F Leader, R Mehlman, Galileo NIMS Team
http://www.agu.org/cgi-bin/wais?q=P62D-08
Latest Results from the Galileo Photopolarimeter-Radiometer at Io and Ganymede
J R Spencer, J A Rathbun, L K Tamppari, T Z Martin, L Barnard, L D Travis
http://www.agu.org/cgi-bin/wais?q=P62D-09
Lava Lakes on Io and Earth
A G Davies, L P Keszthelyi, A Harris, D Williams
http://www.agu.org/cgi-bin/wais?q=P62D-10
Bounds on Io's Heat Flow
D L Matson, T V Johnson, G J Veeder, D L Blaney, A G Davies
http://www.agu.org/cgi-bin/wais?q=P62D-11
Io as seen by Galileo UVS and NIMS: Sulfur Dioxide Frost and Gas Variability
A R Hendrix, R W Carlson, W D Smythe, S Doute
http://www.agu.org/cgi-bin/wais?q=P62D-12
Galileo Imaging of SO2 Frosts on Io
P Geissler, A McEwen, C Phillips, D Simonelli, R Lopes-Gautier, S Doute
http://www.agu.org/cgi-bin/wais?q=P72A-18
Loki: History of eruptions from groundbased and Galileo data
J A Rathbun, J R Spencer
http://www.agu.org/cgi-bin/wais?q=P72A-19
The Effect of Volatile Content on Volcanic Plumes and Flows on Io
W Smythe, R Lopes-Gautier, S W Kieffer
http://www.agu.org/cgi-bin/wais?q=P72A-20
Model of the Internal Constitution of Io Consistent with an Equilibrium-Condensation
Origin
E K Graham Jr., R J Greenfield
http://www.agu.org/cgi-bin/wais?q=P72A-21
MHD Simulations for Galileo's Io Flyby in December 1995
A Kopp, W Ip
http://www.agu.org/cgi-bin/wais?q=P72A-29
UVSTAR Observations of the Io Plasma Torus
G E Ballester, F Herbert, A L Broadfoot, B R Sandel
http://www.agu.org/cgi-bin/wais?q=P72A-28
Waves in the Io torus
X Blanco-Cano, C T Russell, R J Strangeway, M G Kivelson, K K Khurana
http://www.agu.org/cgi-bin/wais?q=P72A-27
Moderate-Resolution EUV Spectra of the Io Plasma Torus During the Galileo
I24 Visit
F Herbert, G R Gladstone
http://www.agu.org/cgi-bin/wais?q=P72A-26
Understanding Io's Space Environment Interaction: Recent Energetic Electron
Measurements from Galileo
B H Mauk, D J Williams, R W McEntire, A Eviatar
http://www.agu.org/cgi-bin/wais?q=P72A-25
Propagation of an Alfven Wing Through the Io's Torus and Energetization
of Electrons
V J Dols, A Otto
http://www.agu.org/cgi-bin/wais?q=P72A-24
A Three Step Model of the Mass Loading of the Io Torus Using Fast Neutrals
Y L Wang, C T Russell, J Raeder
http://www.agu.org/cgi-bin/wais?q=P72A-23
| 32nd Lunar and Planetary Science Conference | March 12-16, 2001 |
| 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 Pillanian News 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 Pillanian News 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; Pillanian News is not a substitute for peer-reviewed journals.
In the March 2001 issue of Pillanian Web,
Look for the March 2001 issue sometime around March 5.
Written by Jason Perry
January 13, 2001
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