Post by Dr. Jim Zimbelman
Lava flows are one of the common landforms encountered on various objects throughout the inner solar system, as well as on Jupiter’s volcanically active moon Io. Cameras and other remote sensing instruments on various spacecraft have returned an incredible amount of data about lava flows on planetary surfaces. Here we will highlight a couple of examples, along with recent work on lava flows on Earth that is providing new insight into how we can study lava flows on other planets.
Mars displays a wide array of volcanic landforms on its surface, particularly in and around the large Tharsis and Elysium volcanic centers. Unfortunately, both of these volcanic centers are buried beneath one to several meters of dust that has severely hampered compositional remote sensing of the lava flows, as well as obscuring morphology in the highest spatial resolution images.
Io is the most volcanically active object in the solar system. Thermal imaging by Earth-based telescopes have monitored the volcanic activity on Io since active volcanoes were discovered by Voyager 1 in 1979. The Galileo mission also monitored the volcanic activity on this remarkable moon of Jupiter. Image 2 shows four distinct hot spots associated with the Amirani volcanic center on Io. Some nearby volcanoes also display hot (active) regions.
Studies of lava flows on Earth continue to provide new ways of studying and interpreting data of lava flows on other planets. The 1907 eruption of Mauna Loa volcano on the Big Island of Hawaii emplaced a basaltic lava flow that covered 25.1 km2 during the 15 days that the eruption was active. Today the flow is the site of one of the largest subdivisions in Hawaii; the quarter-mile (400 m) road grid system provides excellent access to the lava flow (Image 3, a). Differential Global Positioning System surveys (Image 3, c) provide a precise view of the topography across the flow which shows the gentle slopes leading away from the central channel of the flow. The central channel at this location is quite deep because the last lava to this part of the flow was diverted by a breakout several hundred meters upslope of where the profile was measured. Field documentation of the topography and the flow surface texture of the 1907 flow will provide a valuable new data set to which planetary lava flows can be compared in the future.
Baloga, S. M., P. J. Mouginis-Mark, and L. S. Glaze (2003), Rheology of a long lava flow at Pavonis Mons, Mars, J. Geophys. Res., 108(E7), 5066, doi:10.1029/2002JE001981 [abstract]
Garry, W. B., J. R. Zimbelman, and T. K. P. Gregg (2007), Morphology and emplacement of a long channeled lava flow near Ascraeus Mons Volcano, Mars, J. Geophys. Res., 112, E08007, doi:10.1029/2006JE002803. [abstract]
Glaze, L. S., and S. M. Baloga (1998), Dimensions of Pu’u ‘O’o lava flows on Mars, J. Geophys. Res., 103(E6), 13,659-13,666. [abstract]
Keszthelyi, L., Self, S. and Thordarson, T. (2006) Flood lavas on Earth, Io and Mars Journal of the Geological Society 163: 253-264 [abstract]
A. S. McEwen, et al,. (2000) Galileo at Io: Results from High-Resolution Imaging Science 288 (5469), 1193. DOI: 10.1126/science.288.5469.1193 [abstract]
Peitersen, M. N., and D. A. Crown (1999), Downflow width behavior of Martian and terrestrial lava flows, J. Geophys. Res., 104(E4), 8473-8488. [abstract]
J.R. Zimbelman, W.B. Garry, A.K. Johnston, and S.H. Williams, (in press) Precision topography applied to an evaluation of the emplacement of the 1907 Mauna Loa basalt flow, Hawaii, Journal of Volcanology and Geothermal Research [abstract]