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437:. Since steep-sided shield volcanoes have not been observed inside collapsed calderas, this indicates a failure to reform steep-sided volcanoes after the collapse, which can be associated with various variables such as change in temperature, eruptive rate, and/or lava composition. Failure to reform shield volcanoes is caused by failure to supply magma through the magma chamber. These interpretations might be a sign that current shield volcanoes will follow this pattern and transform to caldera-forming eruptive sites.
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eruption. This most prominent central eruption was the first to take place (18° N, 171° W). The total area changed was about 136,000 km (53,000 sq mi). Second, a new eruption caused broadening in the central dark deposits of the western side and new bright rings were deposited along the margins of the lava flows. The total area effected was about 37,000 km (14,000 sq mi). Third, Zamama's third plume was actively erupting while
192:, which identified two types of volcanic activity: persistent and sporadic. The NIMS instrument detected activity at Zamama lasting longer than one year; therefore, it is considered the persistent type. It has only been NIMS-detected five times, but NIMS-observed nine times. This lower incidence of detection could be due to observational constraints or temporary waning of activity.
457:-class; 2) a space-based UV telescope with diffraction-limited capability; 3) space-based missions that enable long-term monitoring of Io over a variety of time scales (seconds, minutes, hours, days, months, years); and 4) expanded time for Io observation on ground-based 8- to 10-m class telescopes, particularly those with nighttime Adaptive Optics capability."
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Zamama A (18°N, 175°W), is about 40 km (25 mi) wide, 1.5 km (0.93 mi) high, and has an average slope of 40°. Slope and height were estimated by PC. It extends about 140 km (87 mi) east and beyond the topographic margin of the observed steep-sided shield. Zamama A is the
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observations. Zamama has shown three notable surface changes in the SSI collected images. Images show them as bright rings, placed within the dark lava flows, with diameters of about 370 km (230 mi). In addition, new black rings were deposited north and northeast of the central prominent
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Io is one of the most challenging Jovian moons for which to establish topography. A couple techniques aided in the making of Io's topography, such as "3D" stereo photogrammetry (SP) and "2D" photoclinometry (PC). Ionian volcanoes have been poorly characterized because of their volcanic construct,
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visit. The flow field appeared narrow/thin closer to the center, and wide/broad away from the center. This behavior might be due to a change in slope from the volcano rim to the nearby plains. The central vent emanates bright flows, due to sulfurous lava composition or silicate lava coated by
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both used thermal remote sensing to accomplish this task. Thermal remote sensing is a branch of remote sensing which deals with processing and interpretations of data in the thermal infrared (TIR) region of the electromagnetic (EM) spectrum. Zamama is a hotspot/volcanic center among 61 active
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The graph of eruption rate shows plunges which indicate lessening in diffusive activity or cooling of old flow surface. As well, it shows a spike, which indicates the beginning of a new eruption. The power output flux graph compares Zamama with other Ionian volcanoes of the same eruptive
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flows with high silica content can have temperatures as high as 1,200 °C (1,470 K; 2,190 °F). Since Zamama volcanoes have such high temperatures, this indicates siliceous magma. No actual samples of Zamama's magma have been retrieved and processed for composition.
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NIMS instrument collected data on volcanic emissions to analyze the power output. A two-temperature model is used to determine the temperature and power output. Models have shown that Zamama has a temperature of 1,173 ± 243 K (900 ± 243 °C;
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spacecraft—the Near-Infrared
Mapping Spectrometer (NIMS), Solid-State Imager (SSI), Photopolarimeter-Radiometer (PPR)—collect and analyze volcanism on Io's surface. Since there are no samples collected from Io, all of the interpretations are made by studying
876:
Williams, David A.; Keszthelyi, Laszlo P.; Schenk, Paul M.; Milazzo, Moses P.; Lopes, Rosaly M. C.; et al. (September 2005). "The Zamama–Thor region of Io: Insights from a synthesis of mapping, topography, and
Galileo spacecraft data".
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was on its 14th orbit around
Jupiter. New deposits enlarged to 150 ± 5 km (93.2 ± 3.1 mi) and are centered east of the eruptive center. Total affected area was about 96,000 km (37,000 sq mi).
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Average volumetric rates decreased at the beginning of the period, which indicates a lessening in diffusive activity, or cooling of old flow surface. Later, there was an increase in volcanic activity, indicating the beginning of an
526:
McEwen, Alfred S.; Simonelli, Damon P.; Senske, David R.; Klaasen, Kenneth P.; Keszthelyi, Laszlo; et al. (October 1997). "High-temperature hot spots on Io as seen by the
Galileo Solid State Imaging (SSI) experiment".
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Zamama C (15°N, 170°W) is located 175 km (109 mi) southeast of the Zamama volcanic center, is about 250 m (820 ft) high, and has a slope that ranges between 3°-5°. Height was determined by
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Zamama B is located 75 km (47 mi) southeast of Zamama A, and is about 40 km (25 mi) wide and 1–1.5 km (0.62–0.93 mi) high. Height was estimated by PC shadow measurements.
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NIMS data analysis was conducted to determine the variability of thermal emissions from volcanoes on Io—particularly Zamama—for 1,038 days (28 June 1996 to 2 May 1999) and the results showed:
742:; Milazzo, M.; Geissler, P.; et al. (December 2001). "Imaging of volcanic activity on Jupiter's moon Io by Galileo during the Galileo Europa Mission and the Galileo Millennium Mission".
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Lopes-Gautier, Rosaly; McEwen, Alfred S.; Smythe, William B.; Geissler, P. E.; Kamp, L.; et al. (August 1999). "Active
Volcanism on Io: Global Distribution and Variations in Activity".
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Zamama has lower volumetric emission rates, compared with other Ionian volcanoes of the same eruptive style, and is more powerful than its terrestrial counterparts such as the volcano
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Davies, Ashley Gerard; Lopes-Gautier, Rosaly; Smythe, William D.; Carlson, Robert W. (November 2000). "Silicate
Cooling Model Fits to Galileo NIMS Data of Volcanism on Io".
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Zamama region on Io showing three volcanoes (Zamama A, B, and C) marked by white arrows. Zamama (A) shield volcano and the dark main flow complex spreading eastward.
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Williams (2013) suggests the need for a variety of methods for observing Io in the future: "Future Io exploration is recommended to include: 1) a
Jupiter-orbiting
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The Zamama active volcanic center is characterized morphologically by a radially centered flow field. Multiple steep-sided shield volcanoes lie in this area:
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In general, Io's eruptions have larger volumetric fluxes and active areas than terrestrial volcanoes, compared with volcanoes of the same eruption style.
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flyby in 1979, making it one of the few planetary volcanoes known to have activated during this generation's lifetime. Further analysis and study by the
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Most Ionian volcanoes start as steep-sided shield volcanoes. After an eruptive construct-building phase, the central region collapses to form a
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which is different from well-studied planetary volcanoes such as those on Mars. Two common flow field morphologies have been identified on Io:
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source of the Zamama flow field. The origin of volcanism is both siliceous and sulfuric, although Zamama originates from a
Prometheus-type
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861:. Geological Society of America 125th Anniversary Annual Meeting & Expo. 27–30 October 2013. Denver, Colorado. Paper No. 305-6.
487:"Temperature and area constraints of the South Volund volcano on Io from the NIMS and SSI instruments during the Galileo G1 orbit"
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visit, or, it may have been buried by the Volund deposits. In contrast, Zamama appeared as a very active hot spot during the
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Thermal
Emission Variability of Zamama, Culann and Tupan on Io Using Galileo Near-Infrared Mapping Spectrometer (NIMS) Data
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Schenk, P. M.; Wilson, R. R.; Davies, A. G. (May 2004). "Shield volcano topography and the rheology of lava flows on Io".
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Davies, Ashley Gerard (September 2003). "Volcanism on Io: Estimation of eruption parameters from
Galileo NIMS data".
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Total volume erupted through this period was 3.5 ± 1.4 km (0.84 ± 0.34 cu mi).
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104:. Zamama has a fissure-fed-type flow that is 150 km (93 mi) long with temperatures of 1,100
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Average volumetric flux was 39.4 ± 15.5 m/s (1,390 ± 550 cu ft/s).
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sulfurous deposits. The composition of the lava emitted from the volcano is still mysterious.
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Zamama has lower volumetric emission rates compared to various styles of eruptions on Io.
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Lava flow field on Zamama. Image was captured using Solid-State Imaging during the
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analysis is strictly used to study such specific planetary structures.
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was derived from geomorphologic interpretations of orbital imaging.
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Zamama is more powerful than its terrestrial counterparts such as
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108:(830 °C; 1,520 °F), and the volcanic center site has
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spacecraft helped with the overall study of Io's volcanism.
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characteristics. The flow appears to be emanating from the
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Zamama appears to have been inactive during the 1979
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139:effects, morphology and/or spectral variations in
391:Comparisons with Ionian and terrestrial volcanoes
313:Lava flows at Zamama suggest that it is a shield
781:; Keszthelyi, Laszlo; Spencer, John (May 2004).
25:Image of the Zamama volcanic center, taken by
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664:Ennis; M. E.; Davies, A. G. (March 2005).
481:Davies, Ashley Gerald; McEwen, Alfred S.;
354:Total power output observed at Zamama was
222:Large broad irregular flows (flow sheets).
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53:. This volcanic center erupted after the
572:Volcanism on Io: A Comparison with Earth
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411:Evolution of Ionian shield volcanoes
163:Most of the data acquired from the
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777:Geissler, Paul; McEwen, Alfred;
300:1,652 ± 437 °F).
822:Journal of Geophysical Research
744:Journal of Geophysical Research
738:Keszthelyi, L.; McEwen, A. S.;
1478:Jupiter Magnetospheric Orbiter
570:Davies, Ashley Gerard (2007).
225:Radially centered flow fields.
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899:10.1016/j.icarus.2005.03.005
858:The Future of Io Exploration
807:10.1016/j.icarus.2003.09.024
642:10.1016/j.icarus.2004.01.015
529:Geophysical Research Letters
491:Geophysical Research Letters
16:Active volcanic center on Io
855:Williams, David A. (2013).
483:Lopes-Gautier, Rosaly M. C.
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1436:Jupiter Icy Moons Explorer
576:Cambridge University Press
317:with a central vent and a
1468:Jupiter Icy Moons Orbiter
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368:Average power output was
130:instruments built on the
425:Model demonstrating how
386:Comparison and evolution
1529:Volcanoes of Io (moon)
1473:Jupiter Europa Orbiter
1211:Lava flows or channels
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720:10.1006/icar.1999.6129
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1503:Io in popular culture
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1461:Cancelled / Concepts
950:at Wikimedia Commons
842:10.1029/2001JE001509
764:10.1029/2000JE001383
750:(E12): 33025–33052.
1452:Io Volcano Observer
1292:Plains and plateaus
920:2000Icar..148..211D
891:2005Icar..177...69W
834:2003JGRE..108.5106D
799:2004Icar..169...29G
756:2001JGR...10633025K
712:1999Icar..140..243L
676:2005LPI....36.1474E
634:2004Icar..169...98S
584:2007vice.book.....D
541:1997GeoRL..24.2443M
503:1997GeoRL..24.2447D
429:volcanoes collapse.
330:Volcanic parameters
201:Volcanic topography
196:Volcanism on Zamama
143:data. Furthermore,
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779:Phillips, Cynthia
593:978-0-521-85003-2
549:10.1029/97GL01956
535:(20): 2443–2446.
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36:is an active
35:
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1428:
1410:
1394:New Horizons
1392:
1385:
1378:
1369:
1362:
1348:
1341:
1266:
911:
907:
885:(1): 69–88.
882:
878:
857:
850:
825:
821:
815:
793:(1): 29–64.
790:
786:
772:
747:
743:
703:
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666:
625:
621:
571:
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33:
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29:in July 1999
26:
18:
1322:Exploration
1230:/ Volcanoes
1084:Kinich Ahau
1023:Quadrangles
447:Io Observer
370:139.8
309:Composition
302:Pyroclastic
280:Temperature
184:flybys, by
95: /
1523:Categories
1350:Pioneer 11
1343:Pioneer 10
1252:Prometheus
1119:Prometheus
461:References
453:-class or
342:in Hawaii.
118:Promethean
92:21°N 173°W
1371:Voyager 2
1364:Voyager 1
1228:Volcanism
1179:Mountains
1169:Viracocha
1154:Thomagata
1079:Kami-Nari
1044:Amaterasu
1013:Mountains
557:128551256
451:Discovery
403:, Hawaii.
351:eruption.
319:rift zone
264:Voyager 1
173:Voyager 1
110:explosive
56:Voyager 1
1445:Proposed
1164:Tvashtar
1074:Gish Bar
360:10
213:mission.
159:missions
97:21; -173
1404:Current
1387:Cassini
1380:Galileo
1276:Fluctūs
1237:Amirani
1218:Tawhaki
1197:Silpium
1149:Tawhaki
1059:Dazhbog
1039:Ah Peku
1032:Paterae
1008:Regions
993:Geology
916:Bibcode
887:Bibcode
830:Bibcode
795:Bibcode
752:Bibcode
708:Bibcode
672:Bibcode
630:Bibcode
580:Bibcode
537:Bibcode
499:Bibcode
435:caldera
427:caldera
401:Kīlauea
340:Kīlauea
323:Galileo
315:volcano
294:Galileo
273:Galileo
268:Galileo
211:Galileo
190:Galileo
186:Galileo
182:Voyager
177:Galileo
157:Galileo
153:Voyager
141:Galileo
132:Galileo
122:volcano
67:Galileo
62:Galileo
42:Jupiter
27:Galileo
1267:Zamama
1242:Masubi
1192:Euboea
1144:Svarog
1139:Shango
1134:Reiden
1124:Pyerun
1114:Pillan
1104:Mithra
1054:Babbar
908:Icarus
879:Icarus
787:Icarus
700:Icarus
622:Icarus
590:
555:
297:'s
289:style.
165:Jovian
137:albedo
120:-type
45:'s
34:Zamama
1496:Other
1202:Tohil
1187:Egypt
1159:Tupan
1109:Monan
1094:Manua
1069:Fuchi
1064:Estan
1001:Lists
553:S2CID
244:plume
167:moon
83:173°W
1508:Life
1483:FIRE
1412:Juno
1330:Past
1262:Thor
1257:Surt
1247:Pele
1099:Maui
1089:Loki
1049:Asha
588:ISBN
356:1.25
175:and
155:and
112:and
80:21°N
48:moon
924:doi
912:148
895:doi
883:177
838:doi
826:108
803:doi
791:169
760:doi
748:106
716:doi
704:140
638:doi
626:169
545:doi
507:doi
253:PC.
73:at
40:on
1525::
1129:Ra
985:Io
922:.
910:.
893:.
881:.
836:.
824:.
801:.
789:.
785:.
758:.
746:.
728:^
714:.
702:.
684:^
650:^
636:.
624:.
602:^
586:.
578:.
574:.
551:.
543:.
533:24
531:.
505:.
495:24
493:.
489:.
469:^
372:GW
169:Io
124:.
71:Io
51:Io
977:e
970:t
963:v
930:.
926::
918::
901:.
897::
889::
844:.
840::
832::
809:.
805::
797::
766:.
762::
754::
722:.
718::
710::
678:.
674::
644:.
640::
632::
596:.
582::
559:.
547::
539::
515:.
509::
501::
375:.
365:.
362:J
358:×
246:.
106:K
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