Highest resolution image of the Masubi volcanic lava flow. Image taken by Voyager 1 in March 1979.

Masubi is an active volcano on Jupiter's moon Io. It is located on Io's leading hemisphere at 49°36′S 56°11′W / 49.6°S 56.18°W / -49.6; -56.18[1] within a bright terrain region named Tarsus Regio. A volcanic plume has been observed at Masubi by various spacecraft starting with Voyager 1 in 1979, though it has not been persistent like similar Ionian volcanoes Amirani and Prometheus.[2] Masubi is also notable for having one of the largest active lava flows on Io, with an additional 240 km (150 mi) flow forming between 1999 and 2007.[3]

Observations by Voyager 1

The volcano was first observed during the Voyager 1 encounter with the Jupiter system on March 5, 1979. Voyager discovered a 64 km (40 mi) tall, 177 km (110 mi) wide volcanic dust plume, composed primarily of sulfur dioxide, at the northern end of a 501 km (311 mi) long dark lava flow.[4][5] To date, images taken by Voyager 1's Imaging Science Sub-system Wide-Angle Camera shortly before the spacecraft's closest approach to Io have the highest spatial resolution coverage of this volcano at two kilometers per pixel.[6] These images reveal a lava flow with a V-shaped northern end, associated with the plume source as noted by the dark plume deposit ring surrounding it, and bifurcated southern section.[6] The two-lobed shape of the plume deposit may result from the Masubi volcanic plume during Voyager 1 encounter having two sources on the flow field and two eruption columns.[7] This was the faintest of the plumes on Io observed by the two Voyager spacecraft. It was initially designated as Plume 8, but in 1979 the International Astronomical Union formally named it Masubi, after a Japanese fire god called Ho-Masubi.[1] The lava flow associated with the plume was named Masubi Fluctus shortly after the start of the Galileo mission.[8]

Observations by Galileo

The Galileo spacecraft and ground-based astronomers observed volcanic activity at Masubi on several occasions in the late 1990s, but it was not a persistent thermal hotspot.[9] The camera on Galileo observed a volcanic plume along Masubi Fluctus during the Galileo extended missions, in July/August 1999 and August 2001.[2] Galileo's cameras also observed a plume deposit form in September 1997. In each of these cases, the volcanic plumes emanated from different parts of Masubi Fluctus, providing further evidence that dust plumes like the one at Masubi result from the rapid sublimation of surficial sulfur dioxide frost by warm, advancing lava flow fronts, rather than erupting from the primary volcanic vent.[10] Ground-based astronomers in August 1998 briefly observed a high-temperature eruption at Masubi, confirming Masubi Fluctus' silicate mafic to ultramafic composition.[11]

Observations by New Horizons

Masubi was last observed by a spacecraft during New Horizons' February 28, 2007 encounter with the Jupiter system. During this encounter, two plumes were observed along Masubi Fluctus. One was seen at the northern end of the flow, interpreted as the main source vent for the flow. The second was observed near the middle of the elongated flow field.[3] These two plumes were 70 and 80 kilometers tall respectively. New Horizons also observed a fresh, 240-kilometer lava flow at Masubi, which formed between Galileo's last observation of Masubi Fluctus in 1999 and the New Horizons flyby in 2007.[3] This was the largest new lava flow observed anywhere in the solar system since extraterrestrial volcanism was discovered on Io in 1979.[12] The two plumes observed emanate from the northern and southern ends of this new flow. Fallout from the two volcanic plumes produced a two-lobed dark deposit around the new lava flow, similar to the deposit seen during the Voyager encounters.

New Horizons images also highlighted the fact that the visibility of the older, 500-km long flow varies depending on the phase angle of the observation. Phase angle is the angle between the observer, Io, and the Sun. Io appears "full" at low phase angles near 0°, "half-full" at moderate phase angles near 90°, and crescent shaped at high phase angles approaching 180°. The older portion of Masubi Fluctus is nearly invisible at low phase angles and only shows up at high phase angles.[3] This may be due to sulfur dioxide frost on top of the now cooled lava flow obscuring it, but this deposit is not yet thick enough to obscure the texture of the flow.[3] A similar phase angle effect at Masubi Fluctus was also observed by Voyager and Galileo, though this was limited to longer visible wavelengths.[13]

References

  1. 1 2 "Masubi". Gazetteer of Planetary Nomenclature. USGS Astrogeology Research Program.
  2. 1 2 Geissler, P. E.; M. T. McMillan (2008). "Galileo observations of volcanic plumes on Io". Icarus. 197 (2): 505–18. Bibcode:2008Icar..197..505G. doi:10.1016/j.icarus.2008.05.005.
  3. 1 2 3 4 5 Spencer, J. R.; et al. (2007). "Io Volcanism Seen by New Horizons: A Major Eruption of the Tvashtar Volcano". Science. 318 (5848): 240–43. Bibcode:2007Sci...318..240S. doi:10.1126/science.1147621. PMID 17932290. S2CID 36446567.
  4. ↑ Davies, Ashley (2007). "Io, 1610-1979". Volcanism on Io: A Comparison with Earth. Cambridge University Press. pp. 7–26. ISBN 978-0-521-85003-2.
  5. ↑ Strom, R. G.; et al. (1979). "Volcanic eruption plumes on Io". Nature. 280 (5725): 733–736. Bibcode:1979Natur.280..733S. doi:10.1038/280733a0. S2CID 8798702.
  6. 1 2 Perry, Jason (March 9, 2009). "Taking another look at Voyager 1 images of Io". The Gish Bar Times. Retrieved 2010-01-30.
  7. ↑ Perry, Jason (March 8, 2009). "30th Anniversary of the Discovery of Volcanism on Io". The Gish Bar Times. Retrieved 2010-01-30.
  8. ↑ "Masubi Fluctus". Gazetteer of Planetary Nomenclature. USGS Astrogeology Research Program.
  9. ↑ Lopes, R. M. C.; et al. (2001). "Io in the near infrared: Near-Infrared Mapping Spectrometer (NIMS) results from the Galileo flybys in 1999 and 2000". Journal of Geophysical Research. 106 (E12): 33, 053–33, 078. Bibcode:2001JGR...10633053L. doi:10.1029/2000JE001463.
  10. ↑ Phillips, Cynthia (October 7, 1999). "Migrating Volcanic Plumes on Io". Planetary Image Research Laboratory. Retrieved 2010-01-30.
  11. ↑ Geissler, Paul (2003). "Volcanic Activity on Io During the Galileo Era". Annu. Rev. Earth Planet. Sci. 31 (31): 175–211. Bibcode:2003AREPS..31..175G. doi:10.1146/annurev.earth.31.100901.145428.
  12. ↑ "Changes on Io". New Horizons: NASA's Pluto-Kuiper Belt Mission. October 9, 2007. Archived from the original on November 13, 2014. Retrieved 2010-01-30.
  13. ↑ Simonelli, D. P.; et al. (2001). "Regolith Variations on Io: Implications for bolometric albedos". Journal of Geophysical Research. 106 (E12): 33, 241–33, 252. Bibcode:2001JGR...10633241S. doi:10.1029/2000JE001350.
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