Volcanoes on Jupiter’s moon found in the wrong place
Washington: Concentrations of volcanic activity in Jupiter`s moon Io are significantly displaced from where they are expected to be based on models that predict how the moon`s interior is heated, according to NASA and European Space Agency researchers.
Io is the most volcanically active world in the solar system, with hundreds of volcanoes, some erupting lava fountains up to 250 miles high.
It is caught in a tug-of-war between Jupiter`s massive gravity and the smaller but precisely timed pulls from two neighboring moons that orbit further from Jupiter-Europa and Ganymede.
Io orbits faster than these other moons, completing two orbits every time Europa finishes one, and four orbits for each one Ganymede makes. This regular timing means that Io feels the strongest gravitational pull from its neighboring moons in the same orbital location, which distorts Io`s orbit into an oval shape. This in turn causes Io to flex as it moves around Jupiter.
The flexing creates friction in Io`s interior, which generates the tremendous heat that powers the moon`s extreme volcanism.
The question remains regarding exactly how this tidal heating affects the moon`s interior. Some propose it heats up the deep interior, but the prevailing view is that most of the heating occurs within a relatively shallow layer under the crust, called the asthenosphere. The asthenosphere is where rock behaves like putty, slowly deforming under heat and pressure.
"Our analysis supports the prevailing view that most of the heat is generated in the asthenosphere, but we found that volcanic activity is located 30 to 60 degrees East from where we expect it to be," said Christopher Hamilton of the University of Maryland, College Park.
Hamilton, who is stationed at NASA`s Goddard Space Flight Center in Greenbelt, Md., is lead author of a paper about this research.
Hamilton and his team performed the spatial analysis using the a new, global geologic map of Io, produced by David Williams of Arizona State University, Tempe, Ariz., and his colleagues using data from NASA spacecraft. The map provides the most comprehensive inventory of Io`s volcanoes to date, thereby enabling patterns of volcanism to be explored in unprecedented detail.
Assuming that the volcanoes are located above where the most internal heating occurs, the team tested a range of interior models by comparing observed locations of volcanic activity to predicted tidal heating patterns.
"We performed the first rigorous statistical analysis of the distribution of volcanoes in the new global geologic map of Io. We found a systematic eastward offset between observed and predicted volcano locations that can`t be reconciled with any existing solid body tidal heating models," said Hamilton.
Possibilities to explain the offset include a faster than expected rotation for Io, an interior structure that permits magma to travel significant distances from where the most heating occurs to the points where it is able erupt on the surface, or a missing component in existing tidal heating models, like fluid tides from an underground magma ocean, according to the team.
The magnetometer instrument on NASA`s Galileo mission detected a magnetic field around Io, suggesting the presence of a global subsurface magma ocean. As Io orbits Jupiter, it moves inside the planet`s vast magnetic field. Researchers think this could induce a magnetic field in Io if it had a global ocean of electrically conducting magma.
"Our analysis supports a global subsurface magma ocean scenario as one possible explanation for the offset between predicted and observed volcano locations on Io," said Hamilton.
"However, Io`s magma ocean would not be like the oceans on Earth. Instead of being a completely fluid layer, Io`s magma ocean would probably be more like a sponge with at least 20 percent silicate melt within a matrix of slowly deformable rock," he added.
"The unexpected eastward offset of the volcano locations is a clue that something is missing in our understanding of Io," said Hamilton.
The research was published January 1 in Earth and Planetary Science Letters.
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