Cook et al. in 1981 examined this image, and found that most of the faint glows, smeared as they were by the multiple exposures, were related to the plumes detected in Voyager 1's daylight images of the satellite, including faint flows from Pele, Marduk, Amirani-Maui, Prometheus, and Volund. The poles of the moon were also faintly illuminated, with the north pole being a bit brighter than the southern one. No thermal emission from Io's volcanic hot spots were observed on this occasion because the vidicon sensors used by the Voyager camera system could not detect photons with wavelengths longer than the orange portion of the visible spectrum. This is much too short to detect thermal emission from all but the hottest of volcanic eruptions. Cook et al. concluded that the glowing gases were not the result of extremely hot plasmas, but were glowing due to being excited by electrons from Jupiter's magnetosphere. They suggest, however, that the polar glows are the result of gases emitted from numerous small vents, as opposed to plumes, which as we shall see from Galileo's results, may not be the correct interpretation.
The Galileo spacecraft arrived at Jupiter 16 years after the Voyager encounters, and stayed to observe Io every few months until its eventual destruction in Jupiter's atmosphere in September 2003. On Galileo's first orbit, it imaged Io in eclipse on June 29, 1996. These first images were taken in the Solid State Imager's clear filter, just as Voyager 1's eclipse observation was, but unlike Voyager's camera, the SSI was sensitive to photons from the near-infrared portion of the spectrum (0.7-1.0 microns). This allowed the SSI camera to detect volcanic hot spots with temperatures greater than 700 K. Scientists found several visible hotspots in this first observation (Pele, Reiden, Marduk, Isum, Mulungu, Fo, and Zamama), providing a proof of concept for this method, which supplemented the spectral observations of the Near-Infrared Mapping Spectrometer (NIMS). The greater sensitivity to high-temperature volcanism, and finding it all across Io's surface also provided further proof that basaltic volcanism was wide-spread. In addition to these more discreet glows, Galileo also observed fainter glows from volcanic plumes (such as Ra Patera), similar to the Voyager observation. The limb of Io also glowed, not just the poles Voyager had seen, though the south pole was brighter in this case (the north pole was brighter when Voyager observed Io in eclipse).
brilliant hot spot was seen at Pillan in June 1997, providing evidence for a massive volcanic eruption there, which would be confirmed by the presence of a volcanic plume in daylight images from that orbit and a massive surface change around the hotspot seen three months later. Eclipse images even showed how Pillan's hot spot had split by September and November 1997 due to lava flowing down into Pillan Patera from the plains above, thus creating a new source of thermal emission in the near-infrared. Such small-scale details were not visible to the NIMS instrument until Galileo's encounters with Io later in the mission. Images taken in the clear filter as well as SSI's near-infrared filters, such as the one at 1.0 micron, provided a way to crudely measure the blackbody temperature of Io's high-temperature volcanoes. This was accomplished by calculating the ratio between the clear filter radiance of a hot spot and its radiance in the one micron filter.
SO2 + hν → SO + O.The green glows are thought to caused by excitation of neutral atomic sodium, which releases photons in the sodium D lines at 589 and 590 nm, within the bandwidth of the green filter. Atomic sodium is another photolysis product, this time deriving from sodium chloride belched from Io's volcanoes. The bright blue glows along the limb near Io's equator are thought to be due to the excitation of molecular sulfur dioxide. Most of these glows are related to various plumes visible near Io's limb at the time of the observation, including Amirani, Acala, Prometheus, Zamama, and Culann. The identification of these chemical species are supported by ground-based and Hubble observations of Io's aurorae, which revealed the presence and absence of various atomic and molecular emission lines, including sulfur and oxygen lines in the ultraviolet at 190 and 135.6 nm, respectively.
Geissler et al. (2001) explored much of the available Galileo and Cassini eclipse image dataset and reported on the how the intensity and position of these auroral emissions change with time. For example, across the Galileo dataset, the red limb emissions were brightest over either Io's north or south pole. The bright equatorial glows, visible as blue glows in the E15 dataset, tend to be located either at plumes or near the sub- and anti-Jovian points on Io's surface. In the latter case, these glows at various times either appear north of the sub-Jovian point and south of the anti-Jovian point, or vice versa. Both temporal variations in the red limb glows and the blue equatorial glows are related to Io's position in the Jovian magnetosphere. Jupiter's magnetic field is tilted with respect to the orbital plane of its main satellites by 9 degrees, so at various times as Io's orbits the planet, the moon is either above or below the equatorial plane of Jupiter's magnetic field. At a system III longitude (λIII) of 0°, Io is below the normal plane of the magnetic field (this occurs with λIII between 290° and 110°). The ion flux from the plasma torus is greatest over the north polar region of Io, causing greater excitation and increasing the brightness of Io's red auroral glows over the north pole. Jupiter's magnetic field lines are also tilted with respect to Io's equatorial plane, so they are tangent to surface north of the equator near Io's sub-Jovian point, and south of the equator near the moon's anti-Jovian point. When the λIII longitude is between 110° and 290°, Io's situation is reversed as it is now above the plasma torus. This time, the south pole limb emissions are brighter than the north's, and the equatorial glows (that aren't related to volcanic plumes) have switched hemisphere as they are now bright south of the sub-Jovian point and north of the anti-Jovian point. This cycle recurs every 12.95 hours, the synodic period between Io's orbital period and the rotational period of Jupiter's magnetic field.
Future missions to Io will certainly use this technique to monitor changes in Io's volcanic activity and atmospheric emissions. Narrow-band filters on future cameras would allow researchers to focus on specific line emissions from various chemical species such as atomic oxygen, sulfur, and sodium. They would also allow for improved measurements of hot spot temperatures. With increased bandwidth, more images using different filters can be taken during each eclipse, allowing for temporal variability of auroral and volcanic thermal emission to be monitored. Finally, these measurements will allow researchers to determine the contribution outgassing from smaller volcanoes provides to Io's atmosphere. Previously modeling focused on the contribution a few volcanic plumes provide, but not weaker outgassing from cooler, but more numerous, volcanoes.
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McEwen, A. S.; et al. (1997). "High-temperature hot spots on Io as seen by the Galileo solid state imaging (SSI) experiment". Geophysical Research Letters 24 (20): 2443–2446.
McEwen, A. S.; et al. (1998). "High-Temperature Silicate Volcanism on Jupiter's Moon Io". Science 280 (5373): 87–90.
Geissler, P.; et al. (1999). "Galileo Imaging of Atmospheric Emissions from Io". Science 285 (5429): 870–874.
Geissler, P.; et al. (2001). "Morphology and time variability of Io's visible aurora". Journal of Geophysical Research 106 (A11): 26,137–26,146.