Io Volcanism Seen by New Horizons: A Major Eruption of the Tvashtar Volcano

@article{Spencer2007IoVS,
  title={Io Volcanism Seen by New Horizons: A Major Eruption of the Tvashtar Volcano},
  author={John R. Spencer and S. Alan Stern and Andrew F. Cheng and H. Weaver and Dennis C. Reuter and Kurt D. Retherford and Allen W. Lunsford and J. M. Moore and Oleg Abramov and R. M. C. Lopes and Jason E. Perry and Lucas W. Kamp and M. W. Showalter and Kandis Lea Jessup and Franck Marchis and Paul M. Schenk and Christophe Dumas},
  journal={Science},
  year={2007},
  volume={318},
  pages={240 - 243}
}
Jupiter's moon Io is known to host active volcanoes. In February and March 2007, the New Horizons spacecraft obtained a global snapshot of Io's volcanism. A 350-kilometer-high volcanic plume was seen to emanate from the Tvashtar volcano (62°N, 122°W), and its motion was observed. The plume's morphology and dynamics support nonballistic models of large Io plumes and also suggest that most visible plume particles condensed within the plume rather than being ejected from the source. In images… 

DSMC simulation of Io’s unsteady Tvashtar plume

Jupiter’s moon Io supports its rarefied atmosphere with prolific tidally-driven episodic volcanism. Its largest volcanic plumes erupt violently and exhibit intricate structure, their canopies rising

The Global Distribution of Active Ionian Volcanoes and Implications for Tidal Heating Models

Tidal heating is the major source of heat in the outer solar system. Because of its strong tidal interaction with Jupiter and the other Galilean satellites, Io is incredibly volcanically active. We

Io Volcanic Plumes: Spacecraft Flythrough Hazard Evaluation

A S THE only other world in the solar system with active silicate volcanism [1,2], Jupiter’s moon Io attracts particular interest among planetary targets, and the National Academy of Science

Auroral evidence of Io's control over the magnetosphere of Jupiter

Contrary to the case of the Earth, the main auroral oval on Jupiter is related to the breakdown of plasma corotation in the middle magnetosphere. Even if the root causes for the main auroral

Chapter 43-Volcanism on Io

differentiation The process by which planets and satellites develop layers or zones of different chemical and mineralogical composition. flyby Term used to describe the close approach of a spacecraft
...

References

SHOWING 1-10 OF 17 REFERENCES

Active Volcanism on Io as Seen by Galileo SSI

Abstract Active volcanism on Io has been monitored during the nominal Galileo satellite tour from mid 1996 through late 1997. The Solid State Imaging (SSI) experiment was able to observe many

High-temperature silicate volcanism on Jupiter's moon Io.

Infrared wavelength observations of Io by the Galileo spacecraft show that at least 12 different vents are erupting lavas that are probably hotter than the highest temperature basaltic eruptions on

Io after Galileo

Io, the volcanically active innermost large moon of Jupiter, was a target of intense study during the recently completed NASA Galileo mission to Jupiter (1989–2003). Galileo's suite of instruments

Ground‐based observations of volcanism on Io in 1999 and early 2000

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

Violent silicate volcanism on Io in 1996

We monitored Io's volcanic thermal emission from 1.7 to 4.8 µm in 1995/96. The data reveal a number of brightenings when Io's thermal emission increased several‐fold. We use a model of emission from

High-Resolution Keck Adaptive Optics Imaging of Violent Volcanic Activity on Io

Io, the innermost Galilean satellite of Jupiter, is a fascinating world. Data taken by Voyager and Galileo instruments have established that it is by far the most volcanic body in the Solar System

Thermal signature, eruption style, and eruption evolution at Pele and Pillan on Io

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 coanalysis of