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Geological Society of America Special Papers
NASA volcanology field workshops on Hawai'i: Part 1. Description and history
Scott K. Rowland, Peter J. Mouginis-Mark and Sarah A. Fagents
Geological Society of America Special Papers 2011;483;401-434 doi: 10.1130/2011.2483(25)
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The Geological Society of America Special Paper 483 2011
NASA volcanology fi eld workshops on Hawai‘i: Part 1. Description and history
Scott K. Rowland1, †, Peter J. Mouginis-Mark2, and Sarah A. Fagents2 1Department of Geology and Geophysics, School of Ocean and Earth Science and Technology, University of Hawai‘i at Mnoa, 1680 East-West Road, Honolulu, Hawaii 96822, USA 2Hawai‘i Institute of Geophysics and Planetology, School of Ocean and Earth Science and Technology, University of Hawai‘i at Mnoa, 1680 East-West Road, Honolulu, Hawaii 96822, USA
ABSTRACT We have organized ten National Aeronautics and Space Administration (NASA)– sponsored planetary volcanology fi eld workshops on Hawai‘i since 1992, providing an opportunity for almost 140 NASA-funded graduate students, postdocs, and junior faculty to view basaltic volcano features up close in the company of both terrestrial and planetary volcanologists. Most of the workshops have been thematic, for example, concentrating on large structural features (rift zones and calderas) or lava fl ows, or features best viewed in high-spatial-resolution data, but they always include a broad set of topics. The workshops purposely involve long fi eld days—an appreciation of scale is important for planetary scientists, particularly if they are or will be working with slow-moving rovers. Our goals are to give these young scientists a strong background in basaltic vol- canology and provide the chance to view eruptive and volcano-structural features up close so that they can compare the appearance of these features in the fi eld to their representations in state-of-the-art remote-sensing images, and relate them in turn to analogous planetary features. In addition, the workshop enables the participants to start a collection of fi eld photographs and observations that they can use in future research and teaching. An added benefi t is that the participants interact with each other, forging collaborations that we hope will persist throughout their careers.
INTRODUCTION European Space Agency (ESA), have undertaken numerous exciting missions to Mercury (MESSENGER), Venus (Magellan), In the past 20 yr, the U.S. and European space agencies, the Moon (Lunar Reconnaissance Orbiter [LRO]), Mars (Path- National Aeronautics and Space Administration (NASA) and fi nder, Mars exploration rovers [MERs], Mars Reconnaissance
Rowland, S.K., Mouginis-Mark, P.J., and Fagents, S.A., 2011, NASA volcanology fi eld workshops on Hawai‘i: Part 1. Description and history, in Garry, W.B., and Bleacher, J.E., eds., Analogs for Planetary Exploration: Geological Society of America Special Paper 483, p. 401–434, doi:10.1130/2011.2483(25). For permission to copy, contact [email protected]. © 2011 The Geological Society of America. All rights reserved. 401 Downloaded from specialpapers.gsapubs.org on March 5, 2012 spe483-01 page 402
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Orbiter [MRO], Mars Express), and Jupiter and Saturn (Galileo with the third workshop, funding has been granted via the suc- and Cassini). Many of these missions have shown the importance cessful submittal of a proposal that is reviewed along with all of volcanism in creating and modifying the surfaces of planets other PG&G proposals. The typical budget is $60,000–$70,000, and moons. The importance of fi eld experience for geologists which includes all travel, food, and lodging costs for the partici- studying other worlds, who by necessity have to conduct their pants and staff, plus 1 mo of salary for a principal investigator studies remotely, cannot be overstated. Field experience intro- (PI) and co-investigator (Co-I). duces a geologist to the complications and variability of natural Formal presentations about the workshops were given at the features in a way that no textbook, satellite image, or computer 2000 Lunar and Planetary Science Conference and 2008 Geo- model can. Usually, it strengthens those textbook, image, or logical Society of America (GSA) Cordilleran Section meetings model ideas, but occasionally (and more importantly), it contra- (Rowland et al., 2000, 2008). The GSA presentation was part of dicts them. An appreciation for the limits of one’s own, and the a session dedicated specifi cally to the use of Earth analog fi eld community’s, understanding of a problem is a key for conducting visits to support planetary geology. That session, and in turn meaningful planetary science. this Special Paper, grew out of a collaborative effort by two Hawai‘i has a long history as a planetary analog to extra- alumni of our 2003 workshop. In this paper, we will present a terrestrial volcanic landforms (e.g., Greeley, 1974; Carr and brief summary of each workshop and its particular theme, and Greeley, 1980); we have tried to continue this tradition by then discuss the specifi c locations on Hawai‘i that we visited. introducing successive generations of planetary geologists to Some of these locations present specifi c logistical and access Hawaiian volcanoes via a series of fi eld workshops. Because challenges, which we discuss as well (Appendix 1). Finally, we Hawai‘i has been the focus of many remote-sensing studies, provide some advice for anyone who might be considering a both for planetary analogs and for better understanding of ter- similar planetary analog workshop. Appendix 2 lists the partici- restrial geology, we have a considerable in-house collection of pants of each workshop. A companion paper (Mouginis-Mark analog data sets comparable to those collected for the planets, et al., 2011, Chapter 26, this volume) discusses some intriguing including complete IKONOS 1 m panchromatic and 4 m color planetary questions for which fi eld analogs in Hawai‘i provide coverage of the island of Hawai‘i. In addition to these very high- important perspectives and key constraints. spatial-resolution visible and near-infrared (IR) images, we have high-spatial-resolution thermal infrared images, SAR (Synthetic WORKSHOPS AND WORKSHOP THEMES Aperture Radar) backscatter images, and high-spatial-resolution topographic data (e.g., LiDAR [Light Detection and Ranging], The workshops have evolved over the years because we TOPSAR [Topographic Synthetic Aperture Radar], and SIR-C learn from each experience, because we incorporate sugges- [Shuttle Imaging Radar-C]). For our workshops, we collate the tions and comments of participants, and because new plane- image data most suitable to studying important volcanological tary data sets (and consequently new science opportunities and topics, and most days of each workshop are spent, images in interests) have become available. hand, examining these features in the fi eld, discussing their ori- gins, and pointing out the aspects that can or cannot be identifi ed Workshop 1 (June 1992, 19 Participants) in remotely sensed data. The image data are provided in hard- copy format so that participants can annotate them and use them The theme was a general introduction to basaltic volca- to compare with their own observations. nism in the fi eld, and topics included lava fl ows, vent structures, Prior to each workshop, we provide an extensive reading pyroclastic deposits, and volcano morphology. We presented a list that covers both the terrestrial aspects of features we plan mix of fi eld excursions and indoor lectures. We had guest lec- to visit and relevant studies of similar features on other plan- tures on radar remote sensing from Dr. Bruce Campbell (Smith- ets. This reading list is quite long and more than most partici- sonian Institution) and on thermal infrared remote sensing from pants want to read. However, we feel that it is important that Dr. Vince Realmuto (Jet Propulsion Laboratory). Jim Garvin the resource be available for those who want it. Additionally, talked about landing site geology on Venus and Mars as viewed we provide (digitally) a set of remote-sensing data for a map- by Venera and Viking, respectively. Considerable effort went ping site. The participants are strongly encouraged to produce into preparing an introduction to Hawaiian volcanism and a fi eld a geologic map of the site prior to arriving in Hawai‘i, and we guide to the locations that we visited. The Hawaiian volcanism spend an evening discussing the image data, and then a full introduction is available on the Web page of VolcanoWorld: day ground-truthing their maps. This mapping exercise consis- http://volcano.oregonstate.edu/education/hawaii/intro/intro. tently is rated as the top experience of the workshop for many html. The fi eld guide has gone through many revisions and iter- reasons. These include exposing participants to data sets they ations, and it was split into two parts (K lauea and Old Hawai‘i do not usually work with, providing a direct image-to-feature Island), both of which are available in pdf format at the fol- comparison, and providing fi rst-hand experience with the limits lowing Web site: http://www.soest.hawaii.edu/GG/resources/ imposed by spatial resolution. gg_documents.html. During this workshop, we realized that The fi rst two workshops were funded directly by NASA’s formal lectures were not such a great idea, not only because Planetary Geology and Geophysics (PG&G) program. Starting participants were pretty tired from fi eld work and found staying Downloaded from specialpapers.gsapubs.org on March 5, 2012 spe483-01 page 403
NASA volcanology fi eld workshops on Hawai‘i: Part 1 403 awake in dark rooms very challenging, but also because the lava fl ows at the fi eld-observable scale. New activities included time could be spent better in the fi eld. a walk from Mauna Ulu, a satellitic shield on K lauea’s east rift zone, down a particularly prominent lava channel (Muliwai a Workshop 2 (August 1995, 9 Participants) Pele). We also visited the ~200-m-thick Pu‘u Anahulu trachyte fl ow. We modifi ed the fi eld exercise yet again by providing the The theme again was general, but we concentrated some- image data to the participants prior to the workshop. Given this what on lava fl ows and vent structures, and we were thus able extra time and the ability to work with familiar software (or color to present more in-depth information on these topics. This was pencils) at their home institutions, the quality of the participants’ the fi rst time that we included fi eld mapping exercises (two, maps was considerably better than those of previous groups. in fact), where the students were given raw image data and allowed to examine the localities independently to make their Workshop 7 (August 2003, 18 Participants) own observations and interpretations. They could then compare what they were able to determine in the fi eld with what was The emphasis for this workshop was on volcanic features available in the images. These mapping exercises turned out to that are studied best using high-spatial-resolution images. We be very valuable, and thus became a feature of all subsequent spent most of the days with a collection of such images in hand, workshops. comparing them to the appearance of features in the fi eld. The weather was quite uncooperative, but the participants managed Workshop 3 (February 1997, 10 Participants) to gain a reasonable understanding of the relationship between image views and real-life views of volcanic features. They also This time, the participants were postdocs and young got a taste of the navigational diffi culties that a rover might NASA-funded PIs, and the focus was on large-scale structures experience during an epic high-elevation hike in the rain and fog of basaltic volcanoes, namely, calderas, rift zones, and unstable on Mauna Loa’s NE rift zone. Visibility decreased to 10–20 m, fl anks. We included new sites on the SW rift zone of Mauna Loa so navigation relied solely on georegistered images and handheld that highlighted these structural features. We incorporated pre- global positioning system (GPS) units. vious participants’ comments by having only one full-day fi eld mapping exercise. This was also the fi rst time that we compiled Workshop 8 (August 2005, 17 Participants) a reading list and made copies of the papers available to the participants during the workshop. This workshop was Mars-specifi c and concentrated on vol- canic features similar to those found in recently collected Mars Workshop 4 (August 1998, 13 Participants) Orbiter Camera (MOC) image data. This was the fi rst year that Dr. Sarah Fagents participated as a workshop leader (she is a Similar to the fi rst and second workshops, the fourth was graduate of the fourth workshop), and her quantitative model- a more general introduction to basaltic volcanic features. We ing skills were a very positive addition to the knowledge base. spent considerable time discussing volcanic surfaces, their We also invited Dr. Steve Baloga to participate as a guest vol- weathering characteristics, and their appearance in remotely canologist, and his input and experience were very valuable. sensed images. We overlapped our fi eld activities on K lauea Dr. Baloga’s insights about the NASA Planetary Geology and with a NASA Jet Propulsion Laboratory–sponsored surface Geophysics Program from the dual perspectives of both an ex– coatings workshop and were able to call upon the expertise of program manager and a principal investigator were signifi cant. some of their organizers during extended fi eld discussions. These programmatic and practical training aspects of a young scientist’s education are commonly overlooked, and it was clear Workshop 5 (August 1999, 10 Participants) that the participants appreciated learning from Dr. Baloga’s experience in these realms. Similar to the third workshop, we concentrated on large- scale basaltic volcano structures. We made an important modi- Workshop 9 (July–August 2008, 13 Participants) fi cation to the mapping exercise, namely, scheduling time for the participants to work on their maps prior to going into the In somewhat of a combination of the seventh and eighth fi eld. We also spent considerable time discussing the specifi c workshops’ themes, we concentrated on volcanic features anal- data sets that were part of the mapping exercise because few of ogous to those on Mars that have been imaged by recent high- the participants were familiar with all of them. spatial-resolution images. Our guest volcanologist was Dr. Bruce Houghton (University of Hawai‘i), and we were also for- Workshop 6 (August 2001, 18 Participants) tunate that Dr. Jim Bell (Cornell University) was able to attend. Bruce’s insights into the interpretation of pyroclastic deposits In this workshop, the theme was lava fl ow morphology. Our and Jim’s years of experience with the Spirit and Opportunity aim was to give participants an appreciation of the complexity of rovers were both very valuable additions to the workshop. Downloaded from specialpapers.gsapubs.org on March 5, 2012 spe483-01 page 404
404 Rowland et al.
Workshop 10 (July 2010, 17 Participants) 1. Kapoho
We essentially repeated the high-spatial-resolution theme Kapoho (the depression; Fig. 2) lies at the easternmost tip of with the additional consideration of the types of features, as Hawai‘i, and it was the site of a 36-d-long eruption in early 1960 well as the views of these features, that a planetary rover might (Macdonald, 1962; Richter et al., 1970). The eruption was charac- encounter. This was accomplished most explicitly by including terized by lava fountains and lava fl ows erupted at a moderately “rover” analog photos as part of the data set that was provided high volumetric fl ow rate (~35 m3 s–1), i.e., conditions that typi- to the participants for their fi nal-day mapping project. Dr. Bruce cally produce ‘a‘ fl ows. However, Kapoho lies within a graben Houghton again provided excellent insights and fi eld activities (hence its name), and the nearly horizontal slopes meant that the relating to pyroclastic deposits and lava ponds. lavas mostly fl owed very slowly; these are conditions conducive to crust growth and later breakage, as well as breakouts of partially PLANETARY ANALOG SITES cooled “toothpaste” lava, which has characteristics that are transi- tional between p hoehoe and ‘a‘ (Rowland and Walker, 1987). We have visited numerous sites on Hawai‘i during our work- shops (Fig. 1). Some of them were included in all ten workshops, Objectives and others only once. In this section, we briefl y outline these The objective here is to investigate the surface character- sites, their key volcanological aspects, and examples of their istics of lava fl ows that serve as an analog to the platy-ridged planetary analogs. Access and logistical issues can be found in Amazonian-age lava fl ows seen on Mars (Keszthelyi et al., Appendix 1. Location 3 (sometimes) and locations 4–12 (all the 2000, 2004). Discussions here include the debate about whether time) are within Hawai‘i Volcanoes National Park, and maps of the platy surfaces in the Cerberus region of Mars are lava fl ows the park are available at the park entrance and headquarters, at or ice deposits (Murray et al., 2005). the Jaggar Museum, and on the park’s map Web site at http:// www.nps.gov/havo/planyourvisit/maps.htm. Additional discus- 2. Ka mana Cave sion of the sites can be found in the online fi eld guides referenced previously, and a more detailed discussion of a small subset of Ka mana cave is a lava tube within the 1880–1881 tube- these sites and their relevance to planetary volcanology is pre- fed p hoehoe lava fl ow of Mauna Loa (Brigham, 1909; Bar- sented in Mouginis-Mark et al. (2011, Chapter 26, this volume). nard, 1990; Rowland and Walker, 1990). This location is ~6 km Translations of place names (initial use in italics), where known, upslope from the distal end of the fl ow in a somewhat neglected come from Pukui and Elbert (1971) and Pukui et al. (1974). county park along Ka mana Dr. (State Hwy 200). Note that the Many of the names are ancient, and for some, the original mean- tube ceiling is unstable, and it is unwise to go more than 10 m ing is unknown. Up until the 1970s, new volcanic features were beyond the entry skylight. named by the U.S. Geological Survey (USGS) and National Park Service (NPS). Since then, new features are given names by the Objectives k 156 155 O O W W 20 km KOHALA 23 N 20O N 22 MAUNA KEA 21 2 - HUALALAI 20 MAUNA LOA 19 - 1 KILAUEA 9 8 11 7 12104 3 13 6 5 14 17 18 16 15 to Hilo 19O N HVO calderacalderacaldera Na- Huku 10 km Crater - Rim Dr. Kilauea Iki 1959 tephra Sand Sept. Devil’s Throat Wash 1982 flow Mauna HWY 11 1974 Ulu flow C upper SW rift zone h a in Muliwai Mauna fault zone o a f C - Iki Koa‘e fault zone ra Pele te rs R to Pahala d. i P a l n a i l i H Mauna Ulu flow field Figure 1. Cloud-free Landsat mosaic showing the locations of fi eld sites discussed in this paper. The Landsat data are available on the HawaiiView Web site at http://hawaiiview.higp.hawaii.edu/. HVO—Hawaiian Volcano Observatory. Downloaded from specialpapers.gsapubs.org on March 5, 2012 spe483-01 page 406 406 Rowland et al. Figure 2. Images of the 1960 Kapoho lava fl ow and a Martian analog. (A) Oblique view of the fl ow fi eld. Note person (circled) for scale, stand- ing at the right-hand end of a large toothpaste lava–surfaced plate, surrounded by ‘a‘ . (B) Close-up of a late-stage spreading area. The edges of the ~10-cm-thick plates have been highlighted for clarity, the straight-edge (circled) is 15 cm long, and numbers indicate the relative ages of the crust surfaces (1—oldest, 3—youngest). (C) Segment of High-Resolution Science Experiment (HiRISE) image (ESP_014184-2070) of a lava fl ow within Elysium Planitia, showing clear evidence for plate formation followed by subsequent spreading, and translation. A C eruption, and this is clearly one of the benefi ts of holding a c workshop on an active volcano (workshops 1 and 3 happened to coincide with pauses in the eruption). No Powerpoint presenta- tion or video can convey the concept of lava fl ow emplacement s ‘a‘a- as well as watching a fl ow in person. Most commonly, we have encountered slowly advancing, infl ating, tube-fed p hoehoe, ‘a‘a- s but participants in the fourth workshop, in 1998, were fortunate ‘a‘a?- enough to view and study some impressively fast-moving ‘a‘ fl ows (Fig. 4). During the ongoing eruption, lava has commonly been entering the ocean, so we have also had the opportunity to s witness small littoral explosions (Fig. 5). 1 km Objectives B The objective here is to observe active lava fl ows, investigate 1 km infl ation features on a compound lava fl ow fi eld, and discuss the D 1.5 m 100 m Figure 3. Skylights. (A) Portion of a vertical air photo showing a line of skylights (S) in the 1855–1856 Mauna Loa fl ow. Note that their dis- continuous nature differs morphologically from the continuous negative topography produced by a lava channel (C). (B) View out one of the sky- lights in this fl ow. (C) Skylights (S) in a lava fl ow on the fl ank of Olym- pus Mons, Mars (Mars Orbiter Camera [MOC] image no. R2000500). In A, most of the dark lava fl ows are young ‘a‘ , and note that their margins have a crenulated outline. The large fl ow in the central part of C has a similar margin morphology, and is likely also ‘a‘ (e.g., Bruno Figure 4. Aileen Yingst (left) and Pete Mouginis-Mark (right) observ- et al., 1994). (D) Steep-sided pit in Mare Ingenii (illumination is from ing 1–2-m-thick ‘a‘ fl ows advancing over a slightly older p hoehoe the upper right). This is Lunar Reconnaissance Orbiter Camera (LROC) surface during our fourth workshop, in August 1998. This location frame: NAC M128202846LE. Credit: National Aeronautics and Space was about halfway between the ends of the buried coastal road, and Administration (NASA)/Goddard/Arizona State University. ~2 km inland. Downloaded from specialpapers.gsapubs.org on March 5, 2012 spe483-01 page 407 NASA volcanology fi eld workshops on Hawai‘i: Part 1 407 Sakimoto et al., 1997; Fagents and Greeley, 2001), the thermal characteristics of lava fl ows and lava lakes on Io (Davies et al., 2001; Lopes et al., 2001, 2004), thermal remote sensing (Flynn et al., 1994; Wright and Flynn, 2003), and the long-term evolution of lava fl ow fi elds on Mars and Venus (Roberts et al., 1992; Kes- zthelyi et al., 2000; Plescia, 2003a). Rootless explosions are pos- tulated to have been the formation mechanism for fi elds of small cones on Mars (Greeley and Fagents, 2001; Lanagan et al., 2001; Fagents et al., 2002; Fagents and Thordarson, 2007; Hamilton et al., 2010), and discussions of these explosions while they are occurring a couple hundred meters away is an experience that is hard to beat. 4. Mauna Ulu Satellitic Shield and Muliwai a Pele Lava Channel Figure 5. Littoral explosions at the ocean-entry site, viewed during our eighth workshop, in August 2008. We estimate that the larger frag- The Mauna Ulu (growing mountain) eruption lasted from ments were 20–30 cm in size, and that they were being thrown ~50 m 1969 to 1974 (Swanson et al., 1979; Tilling et al., 1987) and at the into the air. time was considered to be a long-duration rift zone eruption. The early phase of the eruption consisted of high fountains and chan- growth of Hawaiian Islands and the dynamic topography at the nelized ‘a‘ lava fl ows, but these eruptive products were mostly coast. Observations of active fl ows have relevance to a host of buried by subsequent years of low-effusion-rate tube-fed p hoehoe numerical models on the emplacement of lava fl ows on planetary lavas erupted from an ever-growing satellitic shield (Mauna Ulu surfaces (e.g., Hon et al., 1994; Keszthelyi and Denlinger, 1996; proper; Fig. 6). This was the fi rst long-duration eruption to occur A D B C B C Figure 6. Mauna Ulu and a Martian analog. (A) Low-altitude oblique air photo (view to south; arrows indicate loca- tions from which photos B and C were taken, both during our 1992 workshop). (B) View south along the east rim of the crater—in the mist to the right of the overhung rim, there is a drop of ~85 m. (C) View north down a prominent channel, which ends in a perched lava pond (Carr and Greeley, 1980; Wilson and Parfi tt, 1993). (D) Thermal Emission Imaging System (THEMIS) panchromatic image of two small shield volcanoes at 5.5°S, 245°E, Mars, within the Pavonis Mons South volcanic fi eld (Bleacher et al., 2009). Illumination is from the left. Image is a segment of frame number V03862002. Downloaded from specialpapers.gsapubs.org on March 5, 2012 spe483-01 page 408 408 Rowland et al. after Hawaiian Volcano Observatory became modern and well eruption (Carr and Greeley, 1980; Wilson and Parfi tt, 1993), and staffed, and many landmark papers about lava fl ow emplacement, it provides excellent exposures that illustrate the complexity that long-duration eruptions, and long-term magma supply to K lauea can develop even during a short-lived event (Harris et al., 2009). resulted from observations at this time (e.g., Swanson, 1973; Peterson and Tilling, 1980; Kilburn, 1981; Peterson et al., 1994). Objectives The Muliwai a Pele (river of Pele) channel (Fig. 7) formed during Mauna Ulu is a classic satellitic shield, and as such, it is an a brief return to ‘a‘ production near the end of the Mauna Ulu excellent analog to the small shields that have been described Mauna Ulu ABsummit A B C D E F G H I J ~25 km N 0 5 km D E F 0 500 m 0 500 m 0 500 m Figure 7. Lava channels. (A) Mauna Ulu. Dashed white line indicates outlines of 1-m spatial resolution IKONOS data that workshop participants use as they walk from Mauna Ulu along the Muliwai a Pele channel. IKONOS images D, E, and F are enlarged below, and illustrate some of the complexity along even a short-lived channel (B) Synthetic Aperture Radar (SAR) image of a channel on Venus that fl owed from upper right (NE, in Fortuna Tessera) to lower left (SW, in Sedna Planitia). This channel is ~2 km wide. Magellan image F-MIDR 45N019;1, framelet 18. Downloaded from specialpapers.gsapubs.org on March 5, 2012 spe483-01 page 409 NASA volcanology fi eld workshops on Hawai‘i: Part 1 409 recently on Mars (Fig. 6; Mouginis-Mark, 2003; Bleacher respectively, and typically cannot be used as proxies for slope- et al., 2007, 2009; Baptista et al., 2008; Baratoux et al., 2009; rheology relationships or volumetric fl ow-rate calculations Hauber et al., 2009). It is instructive to discuss the complex- (Harris et al., 2009). ity of the Mauna Ulu shield, including the subsidiary shield that developed over the now-buried ‘Alae (mud hen) pit crater 5. Lower Mauna Ulu Flow Field, Hilina Pali (Swanson et al., 1972; Tilling et al., 1987), in light of models of small-shield development. The walls of the crater clearly show From the Ke ala komo (the entrance path) and Holona how a small shield is constructed of multiple overfl ows, and Kahakai (sailing, traveling seacoast) overlooks along Chain of the Mauna Ulu fl ow fi eld itself shows considerable complex- Craters Road, there are spectacular views downslope over the ity, with overlapping fl ow units and fl ow types. Although much unstable south fl ank of K lauea (Fig. 8). Because of a lack of smaller than many planetary lava channels (Fig. 7), Muliwai a any buttressing to the south, this unstable fl ank slips downward Pele nevertheless provides a host of discussion points regarding via series of large normal faults, together comprising the Hilina channel development and the assumptions and care required pali (cliff struck by wind). This downward slippage occurs dur- when modeling channelized lava fl ows. One concept to discuss ing, but is not the cause of, large, south fl ank earthquakes. These is the fact that variations in the overall fl ow width and channel earthquakes occur on the landward-dipping interface between depth are often due to complex overfl ow and blockage events, the base of K lauea and the underlying ocean crust (Swanson A caldera C East rift zone t e m S y s u l t F a a Southwest rift nzone i collapse i l B H pit N 10 km B Pu‘ukapukapu Figure 8. Hilina Pali and a Martian analog. (A) Shaded relief image (illuminated from the NW and 45° above the horizon, created from a U.S. Geological Survey 10 m digital elevation model; http://hawaii.gov/dbedt/gis/hill.htm) showing the numerous downdropped blocks that comprise the unbuttressed south fl ank of K lauea (B and arrow indicate location and view direction of B). (B) Low-altitude oblique air photo looking to the west. Almost all of the Hilina faults are down- dropped to the south, but one is down dropped to the north, forming a small horst, the summit of which is Pu‘ukapukapu (regal hill), visible in middle ground. Note the fl ows exposed in the 3.20-m-high cliff below Pu‘ukapukapu and the talus slopes extending to near sea level. (C) A portion of the basal escarpment of Olympus Mons, Mars, at 14.8°N, 229.6°E (Thermal Emission Imaging System [THEMIS] image V01415006; illumination is from the left). Note how lava has fl owed around a high point on the scarp that is topped by a collapse pit. Downloaded from specialpapers.gsapubs.org on March 5, 2012 spe483-01 page 410 410 Rowland et al. et al., 1976; Lipman et al., 1985). An exhilarating way to expe- well as the manner in which they may deform over time (e.g., rience these fault scarps is to climb down one of them, from the McGovern and Solomon, 1993; McGovern and Morgan, 2009). Holona Kahakai overlook to the Alanui Kahiko (old highway) pullout. There is no trail, and the slopes approach 45°, but with 6. Mauna Ulu Mapping Exercise, East Rift Zone of K lauea care (avoid the ‘a‘ ) and proper fi eld gear (boots, long pants, and gloves), it is a very rewarding experience. We adopted this mapping site in 2008 because of unsafe SO2 Once on the lower (and more gradual) slopes, there are excel- levels at Mauna Iki (little mountain; see analog site 13). Image lent opportunities to observe features of ‘a‘ and p hoehoe lava and spectral data are provided to participants a couple months fl ows, often in close proximity, which are good for comparison prior to the start of the workshop, and they are encouraged to pro- purposes. Considerable work on the emplacement of p hoehoe duce a geologic map based on these data. We spend all of the fi nal fl ows has been conducted on the Mauna Ulu fl ows in this region workshop day ground-truthing their maps. Although not as good (Crown and Baloga, 1999; Byrnes and Crown, 2001), including a site as Mauna Iki due to fewer surface types and ages, there is the effects of the underlying slope on individual p hoehoe fl ow suffi cient variety for the mapping to be challenging, and it is eas- unit shape and size. The results have been used to characterize ily accessible via Chain of Craters Road. A study of the Mauna the emplacement processes of some Venusian lava fl ows (Byrnes Ulu fl ow fi eld that includes a similar data set of multiple remotely and Crown, 2002). The studies were partially inspired by these sensed images along with fi eld observations was published by authors’ visits to this area as participants in our workshops. three of our workshop participants (Byrnes et al., 2004). Objectives Objectives Up-close and distant views of the Hilina Pali lead into dis- Objectives here are to put the previous week’s knowl- cussions of the growth and collapse of volcanoes on Mars, as edge to practical use, and to use remote-sensing data to map fl ow textures, collapse features, tectonic features, etc. In the A HVO process of completing a reconnaissance map of lava textures and rift zone features, the participants are required to utilize Byron B C Ledge high-lava mark B Pu‘u Pua‘i main 1959 vent ~1 km A Figure 9. K lauea Iki. (A) View west, along the ~90-m-high north wall of the crater. Note the smooth ponded lava surface and the high-lava mark Figure 10. Coalescence of collapse pits. Photo insets show uncoalesced (see text). The Hawaiian Volcano Observatory (HVO) is in the distance, (A) and coalesced (B) collapse pits developed in K lauea Iki tephra and note that it sits atop a satellitic shield (the Observatory shield; Hol- (see Fig. 12 for location). These pits overlie fi ssures that predate de- comb, 1987). (B) View south to the main 1959 vent (elev. 1067 m) and position of the tephra. (C) Collapse pits in lava plains NE of Ascraeus Pu‘u Pua‘i (elev. 1184 m). See Figure 11 for photo locations. Mons, Mars (Mars Orbiter Camera [MOC] image no. MOC2-1476). Downloaded from specialpapers.gsapubs.org on March 5, 2012 spe483-01 page 411 NASA volcanology fi eld workshops on Hawai‘i: Part 1 411 multiple remote-sensing images that are analogs to various into the main vent and observe all manner of lava lake features planetary data sets. This is an excellent opportunity to test (Stovall et al., 2009), including a so-called bathtub ring, which photogeologic mapping skills that might be developed using records the highest level that the lava lake achieved before drain- MGS (Mars Global Surveyor), MRO (Mars Reconnaissance back into the vent, cooling-induced contraction, and degassing, Orbiter), MO (Mars Observer), LRO (Lunar Reconnaissance all lowered the surface to its present level. Excellent examples of Orbiter), Magellan, or MESSENGER data sets. Field valida- rheomorphic spatter fl ows can be found on the fl anks of Pu‘u Pua‘i, tion of interpretations made from satellite data sets cannot be and cross sections of the scoria deposit are exposed in a series of overemphasized as a learning experience! collapse pits. These pits have developed within the tephra deposit as tephra has fallen into preexisting fractures. Thus, they provide 7. K lauea Iki and Pu‘u Pua‘i good examples of circular depressions developed by collapse of a surface layer into a linear fi ssure, much like (except for their size Here, there are many hours worth of excellent volcanic difference) the pit chains that have been observed at many volcanic features and planetary analogs all within a short walk or drive. locations on Mars (Fig. 10). The 1959 K lauea eruption partially fi lled a preexisting pit crater (K lauea Iki; little K lauea) with lava, and some of the highest Objectives lava fountains on record in Hawai‘i built a substantial scoria cone The purpose here is to walk across the frozen lava lake (Pu‘u Pua‘i; gushing hill) and downwind tephra deposit (Fig. 9; and observe the tephra deposits from Pu‘u Pua‘i. This provides Macdonald, 1962; Richter et al., 1970). A hiking trail leads down the opportunity to discuss the smooth (and therefore radar-dark) one side of K lauea Iki crater, across the solidifi ed surface of the surface of the lava lake, and its meaning for the interpretation lava lake, and up the other side. Along the way, one can stop to peer of plains materials on Venus (Fig. 11; Campbell et al., 1993; A Hwy. 11 - Pahala Ke‘amoku- flow (Mauna Loa) 13 Figure 11. Synthetic aperture radar (SAR) data for K lauea and Sif Mons, Mauna Iki Kilauea- Venus. (A) A 3-wavelength composite Halema‘uma‘u Caldera of P band (68 cm), L band (24 cm), and C band (5.6 cm) wavelengths in red, green, and blue, respectively. This is a mosaic of Jet Propulsion Laboratory 9B AIRSAR images kd1 and kc4, collected Hilo in August 1990 (Glaze et al., 1992). 16 K lauea caldera, K lauea Iki, and Hale- Pu‘u 9A ma‘uma‘u are all radar-dark because Pua‘i December Kilauea- they are mostly smooth ponded lava 1974 flow Iki fl ows. Note that much of the area SW of the caldera is also radar-dark, and this is due to extensive coverage by Keanak ko‘i ash. Radar properties of the 100 km December 1974 fl ow were studied, with B Venus analogs in mind, by Gaddis et al. (1989, 1990). Numbered arrows indi- cate locations from where Figures 9 and 13 were taken, and dashed ellipse shows area of Figure 17. (B) Numerous, complex lava fl ows, some of which have been constrained by preexisting frac- tures, on the north fl ank of Sif Mons, Venus (Magellan image no. PIA00471). Downloaded from specialpapers.gsapubs.org on March 5, 2012 spe483-01 page 412 412 Rowland et al. Campbell and Rogers, 1994; Campbell and Shepard, 1996; (Clague et al., 1999; Swanson, 2008) and produced extensive tube-fed Carter et al., 2006). Inspection of the tephra deposits leads into p hoehoe fl ows that extend to the coast ~40 km away. The eruption a discussion of explosive volcanism on the planets, and, in par- immediately preceded ~300 yr of explosive activity at K lauea, and it ticular, pyroclastic deposits such the dark halo craters within may be recorded in part of the epic Hawaiian story of Pele, Hi‘iaka, Alphonsus crater on the Moon (Fig. 12). and Lohi‘au (Swanson, 2008). 8. N Huku (Thurston Lava Tube) Objectives N Huku provides another opportunity (in addition to N Huku (the protuberances) is a large lava tube that leads out Ka mana cave) to talk about long-duration basaltic eruptions, of the summit crater of the ‘Ai L ‘au (forest eater) satellitic shield lava-tube development, thermal erosion, and sinuous rilles on (Fig. 13). The ‘Ai L ‘au eruption lasted from ca. 1410 to 1470 A.D. the Moon. A B main 1959 vent 1959 lava lake DH DH N Pu‘u Pua‘i collapse pits Devastation trail Byron N Ledge trail 500 m500 m Figure 12. Tephra deposits. (A) Part of a panchromatic IKONOS image (no. 2000112520362450000011603357, collected 25 November 2000), showing the thickest part of the downwind tephra deposit from the 1959 K lauea Iki eruption. The dashed ellipse shows the region of collapse pits (Fig. 10). (B) An oblique view looking west, showing dark halo deposits (DH) within the lunar Alphonsus Crater, which is ~100 km across. Apollo-16 image number AS16-M-2478. - Pu‘u ‘O‘o- plume - R O F I L E O F P ‘A I L A ‘A U S H I E L D Byron Ledge Pu‘u Pua‘i 1974 lavas ponded against E caldera wall Figure 13. Profi le of the ‘Ai L ‘au shield (the skyline; highest elev. = 1200 m), viewed to the east from the Hawaiian Volcano Observatory (5.3 km away; see Fig. 11 for view direction). The fl oor of K lauea caldera is in the near and middle ground. Byron Ledge (3.2 km away; elev. ~1130 m) separates the caldera from K lauea Iki crater. Downloaded from specialpapers.gsapubs.org on March 5, 2012 spe483-01 page 413 NASA volcanology fi eld workshops on Hawai‘i: Part 1 413 9. K lauea Caldera, the Hawaiian Volcano Observatory (HVO) A K lauea caldera probably developed shortly before the ‘Ai L ‘au eruption (Swanson, 2008; Fiske et al., 2009), but it is just one in a series of many calderas that have formed, infi lled, and fault then reformed during the life of K lauea volcano (e.g., Holcomb, blocks 1987; Decker, 1987). The structure of the caldera is visible from a number of vantage points, and it clearly illustrates the com- July plex nature of a large caldera, including collapse blocks (Fig. 14), Dr. multiple faults, and nested collapse structures. HVO is run by r Rim 1974 ate the U.S. Geological Survey (USGS) and is one of the oldest and Cr lava most advanced volcano observatories in the world. The Jaggar Museum, constructed out of an older part of HVO, houses many modern displays about volcanoes and volcano monitoring, and it Keanakako‘i- has probably the best vantage point in the whole summit region. crater Objectives This location allows us to gain an appreciation for the scale - and complexity of caldera features, and the ways in which these Keanakako‘i ash large-scale structures affect the morphology and distribution of lava fl ows, to learn more about the morphology of basaltic shields, to learn how their activity is monitored, and to under- stand how they evolve over time. Views of the caldera are par- ticularly valuable for discussions of planetary calderas such as B those found in the Tharsis region of Mars and on shields on Venus (Crumpler et al., 1996; Mouginis-Mark and Rowland, 2001; Mouginis-Mark et al., 2007). On a clear day, participants can not only gaze into K lauea caldera, but also turn around and look westward for a spectacular profi le view of Mauna Loa, the largest shield volcano on Earth. 10. Devil’s Throat Pit Crater Not quite 100 m NE of Chain of Craters Road is Devil’s Throat pit crater. It was described by Jaggar (1912 [1988]) as being ~75 m deep with an overhanging rim. Since then, perhaps as recently as the 1960s (Blevins, 1981), the last vestiges of over- hangs fell in to produce essentially vertical walls (Fig. 15). The idea of the surface layers being the last to fall in led Blevins (1981) and Walker (1988) to propose stoping as the mechanism for pit crater formation. Modeling by Blevins (1981) suggested that the cavity into which material is falling is at a depth of 50–100 m below the surface, and may therefore be immediately beneath the present crater fl oor. Okubo and Martel (1998) proposed an alter- native based on the propagation of fractures upward from the top edge of a dike. The angle between these two fractures is constant, Figure 14. Failure of caldera walls as coherent blocks. (A) Oblique air photo northward across K lauea caldera. The length of the contact between the lowest fault blocks and the caldera fl oor is ~1100 m. (B) Mosaic of Thermal Emission Imaging System (THEMIS) images of the NE portion of Ascraeus Mons caldera, Mars. Illumination is from the left. Mosaic of 2 km images V01464013 and V01826008. Downloaded from specialpapers.gsapubs.org on March 5, 2012 spe483-01 page 414 414 Rowland et al. Objectives A The objective here is to observe a structure formed in relatively horizontal lava fl ows purely by collapse and discuss the relationship between fractures and open pits. The newly discovered pits on the Moon and Mars (Fig. 3D; analog site no. 2) resemble Devil’s Throat in both morphology and size, and C a discussion of whether they might be skylights or pit craters, as well as the differences between skylights and pit craters, is appropriate here. Chain o Rd. 11. K lauea SW Rift Zone Fractures f Craters N ~40 m At a pullout along Crater Rim Drive, much of the stra- tigraphy of the explosive Keanakko‘i (the adze cave) ash deposit is exposed in a series of fi ssures that opened dur- B ing the huge 1868 earthquake (Fig. 16). These fi ssures are the proximal end of K lauea’s SW rift zone. The pyroclastic material exposed in the fi ssures ranges from fi ne-grained ash fall to lithic-rich pyroclastic density current deposits. All of these deposits were fi rst interpreted as having been emplaced over hundreds of years (e.g., Powers, 1948), but they were later reinterpreted to have been emplaced in perhaps as little as a month (Decker and Christiansen, 1984; McPhie et al., 1990). Based on 14C dating, the interpretation has come full circle, and the Keanak ko‘i ash is now known to have been deposited over an ~300-yr-long period, specifi cally between ca. 1500 and 1790 A.D. (Swanson, 2008; Fiske et al., 2009). These are some of the best exposures of basaltic pyroclastic features on K lauea. Unfortunately, as of this writing (June C 2011), this part of Hawai‘i Volcanoes National Park, as well as the features described in locality 12, are closed due to high SO2 levels associated with the vapor plume emanating from Halema‘uma‘u (house of the ama‘u fern) crater. Visitors should inquire at Park Headquarters regarding these locations and never attempt to enter closed areas. Objectives The goal is to provide close-up views of explosive depos- its of many kinds and stimulate a discussion of the causes of explosive eruptions on basaltic volcanoes (Dvorak, 1992; Mas- tin, 1997). Figure 15. Devil’s Throat pit crater. (A) IKONOS panchromatic (1 m 12. Keanak ko‘i Ash, Gullies, Sandwash SW of K lauea spatial resolution) image. Arrow indicates location from which C was Caldera, December 1974 Lava Flow taken. (B) Oblique air photo taken toward the SW. Dashed lines are fracture zones mapped by Blevins (1981) and Okubo and Martel (1998); The region SW of K lauea caldera is blanketed by the note that they form a “waist” at Devil’s throat. (C) Photo to the east across Devil’s Throat, showing the numerous lava-fl ow layers exposed Keanak ko‘i ash (Malin et al., 1983; Fiske et al., 2009), which in the near-vertical walls. Note person (circled) for scale. is currently being gullied whenever heavy rains occur (Fig. 17). This region therefore provides good examples of both the surface (e.g., dunes) and subsurface (e.g., cross-beds) meaning that as the top of the dike nears the surface, the fractures characteristics of a basaltic pyroclastic deposit. South of the approach one another. When they reach a critical distance, the sandwash area are the vents of the December 1974 lava fl ow strength of the rock between them can no longer remain coher- (Lockwood et al., 1999). This fl ow has been the focus of ent, and it collapses into the top of the dike. numerous radar roughness and topography-interaction studies Downloaded from specialpapers.gsapubs.org on March 5, 2012 spe483-01 page 415 NASA volcanology fi eld workshops on Hawai‘i: Part 1 415 (e.g., Gaddis et al., 1989; Campbell et al., 1993; Carter et al., Halema‘uma‘u 2006). The transition from smooth p hoehoe to rough ‘a‘ A is particularly well displayed, as are interesting controls by the north-facing Koa‘e (tropic bird) fault zone (Fig. 11). Mouginis-Mark et al. (2011, Chapter 26, this volume) discuss these radar studies in more detail (see references therein and B their Figs. 9–12). Keanakako‘i- Objectives ash 1971 The purpose here is to discuss explosive basaltic activity, spatter windblown deposits, gully formation, lava surface transitions, and lava and fault scarps. Many of the pyroclastic surfaces have devel- oped a duricrust by precipitation of silicic material between grains (Malin et al., 1983). The deposits are mostly very smooth in SAR data (Fig. 11) and provide a good impetus to B start a discussion of what constitutes “smooth” and “rough” on planetary surfaces (e.g., Campbell et al., 1993; Campbell 1971 and Rogers, 1994; Campbell and Shepard, 1996; Carter et al., block spatter sag 2006). This, of course, is also an excellent place to discuss gully formation and whether or not the obvious surface-water cutting of these gullies can be scaled upward to explain the huge gullies observed on Mars, or if some other mechanism Keanakako‘i- is required (e.g., Kochel and Piper, 1986; Kochel and Baker, ash 1990; Malin and Edgett, 2000; Gulick, 2001; Lamb et al., 2007). The 1974 vents are fi ne examples of en echelon spat- ter ramparts, and the exposures of fl ow surface transitions are second to none. The Koa‘e fault scarps, formed as the south fl ank of K lauea pulls away from the caldera (Duffi eld, 1975), provide not only volcano-structural discussion points, but also C excellent exposures of lava fl ows in cross section and of the interaction between windblown basaltic sands and preexisting topography. 13. Mauna Iki Mauna Iki (Fig. 18) is a satellitic shield and associated fl ow fi eld, erupted during the fi rst 9 mo of 1920. The eruption occurred near the end of at least 100 yr of constant lava lake activity at Halema‘uma‘u, and Rowland and Munro (1993) found evidence that during parts of the Mauna Iki eruption, there was direct drainage of lava from the summit down the ~4 cm SW rift to this eruption site. Objectives Figure 16. Keanak ko‘i ash exposed in fractures. (A) View NE of the Except in 2008, when it was closed to the public due to high uppermost part of K lauea’s SW rift zone, marked here by a series of fractures. The arrow indicates the location from which photo B was concentrations of SO2 and H2SO4, this has been our full-day taken. The road is 2 lanes wide, and Halema‘uma‘u (middle distance) mapping site. Participants are provided with image data in the is 990 m wide, rim to rim. (B) Participants in our fi rst workshop ex- weeks leading up to the workshop, and from these, they are amining a large block that produced a sag structure in the underlying expected to produce a geologic map. Mauna Iki is probably the air-fall ash layers. (C) An image taken by the panoramic camera on the Spirit Mars exploration rover (MER) at the “Home Plate” site, best location on K lauea for this exercise because it presents a which shows a ~4-cm-wide sag structure in layers (National Aero- wide variety of geological surfaces, structures, and ages, and nautics and Space Administration [NASA] MER press release image because it is essentially unvegetated and easily accessed from a 20070503a). trailhead on Hwy 11. Downloaded from specialpapers.gsapubs.org on March 5, 2012 spe483-01 page 416 416 Rowland et al. A D caldera rim B E pre-Keanakako‘i- pahoehoe- C F Figure 17. Surfaces and outcrops SW of K lauea caldera. (A) Surface of Keanak ko‘i ash, which is very radar-dark in Synthetic aperture radar (SAR) data (see Fig. 11 for location). (B) A small rain-cut gully, exposing pre-Keanak ko‘i p hoehoe, outlined by the dotted line. (C) Water-reworked pyroclastics in the wall of a small rain-cut gully. (D) Workshop participants at a location where a narrow arm of September 1982 lava fl owed down a preexisting gully. (E) A tumulus at the crest of a Koa‘e fault scarp (down- dropped to the left). The tumulus was split open by the faulting, and windblown sand has infi lled the fracture. (F) A southward view across part of the 1974 fl ow. In E and F, the global positioning system (GPS) receiver (circled) is 15 cm × 7 cm in size. 14. N nole Hills The N nole (bending) Hills (Fig. 19) are enigmatic, high- standing hills with sloping upper surfaces that are mostly, but not entirely, coplanar. These hills have been interpreted in a number of ways, including that they represent a very early stage of Mauna Loa or perhaps a separate, pre–Mauna Loa volcano (Stearns and Clark, 1930; Macdonald et al., 1983). A pre-Mauna Loa volcano in this location would be Figure 18. Photo of Mauna Iki satellitic shield, viewed from the inconsistent with the increase in ages of Hawaiian volcanoes NW. Note the gentle slopes, similar to those of the ‘Ai L ‘au shield to the NW; however, the rocks that comprise the hills are (Fig. 13). The skyline, which roughly parallels the SW rift zone, is ~2 km indeed old. Ages of 100,000–200,000 yr have been determined away in this view, and the arrows are ~2 km apart. Downloaded from specialpapers.gsapubs.org on March 5, 2012 spe483-01 page 417 NASA volcanology fi eld workshops on Hawai‘i: Part 1 417 10 km N i Wood Volcano Figure 19. Shaded relief image (illumi- e Valley n nated from the NW and 45° above the o horizon, created from a U.S. Geological Hilina Pal z Survey 10 m digital elevation model; http://hawaii.gov/dbedt/gis/hill.htm) t of the SE portion of Hawai‘i, showing Pahala- f the N nole Hills, downslope of what i appears to be a large, mostly buried r Ninole- collapse scarp (hachured line). Inset: These same hills as viewed to the NNW Hills 1 W Y1 from Honu‘apo. K, P, M, and E indi- E cate Kaiholena (referring to a type of S K HW banana), Pkua (back wall or enclosure), P M Makanau (surly eyes) Hills, and Enuhe K P (caterpillar) Ridge, respectively. The M E distance from the summit of Kaiholena to the top of Makanau is 5.7 km. Kailu - a Wai‘ohinu Honu‘apo Na‘alehu-- (Lipman et al., 1990), although there is considerable uncer- both the east and west fl anks of Tharsis Tholus (Fig. 20; Ples- tainty due to the weathered nature of the rocks and their low cia, 2003b). K content. The interpretation of Lipman et al. (1990) is that the N nole Hills are in-place remnants of Mauna Loa’s east 15. Thermally Eroded Lava Tube at Honu‘apo fl ank, which was isolated from resurfacing lavas because of the presence of a west-facing collapse scar, which lowered In a low ocean cliff at Honu‘apo (caught turtle), there is the axis of the SW rift zone such that lavas only fl owed west. an example of a partially drained lava tube that eroded into Only after the rift zone had rebuilt itself above the head of its substrate (Coombs and Rowland, 1994). The idea of ther- the scar were lavas able to begin resurfacing the east fl anks, mal (or thermomechanical) erosion by fl owing lava was pro- in the process partially burying valleys and ridges (i.e., the posed and studied mostly by planetary geologists for many N nole Hills). A recent interpretation (Morgan et al., 2010) years as a possible mechanism for forming sinuous rilles on is that the N nole Hills are remnants of an old and abandoned the Moon (Hulme, 1973, 1982; Carr, 1974; Williams et al., Mauna Loa rift zone. 2000). Although observations consistent with thermal ero- Examination of digital topography (Fig. 19) shows that sion were made during the Mauna Ulu eruption (Peterson the hills are downslope of a somewhat subdued, concave- and Swanson, 1974; Peterson et al., 1994), only somewhat downslope scarp, that probably is the headwall of a collapse that recently have most terrestrial volcanologists taken much produced the Punalu‘u (spring that is dived for, i.e., submarine interest in the topic. This changed more recently with the spring) avalanche deposit offshore (e.g., Mark and Moore, 1987; publication of a catalog of thermal erosion examples (Gree- Moore et al., 1989; Moore and Mark, 1992). Another interpre- ley et al., 1998), evidence of erosion observed in active tubes tation, therefore, is that the N nole Hills are toreva blocks that during the current K lauea eruption (Kauahikaua et al., 1998, only moved a short distance from a large-scale collapse scar. 2003), and serious consideration of the physical processes It is probably safest to say that the N nole Hills are not fully involved (Fagents and Greeley, 2001; Kerr, 2001). The understood. example at Honu‘apo is associated with a p hoehoe fl ow that underlies ~26,000-yr-old P hala ash, and it has cut through Objectives an ‘a‘ fl ow, a layer of scoria, another ‘a‘ fl ow, and partially With views of the N nole Hills in the distance, the vari- into a p hoehoe fl ow (Fig. 21). ous formation mechanisms that would produce these peculiar structures can be discussed and compared to ideas about vol- Objectives cano collapse in general. Several analogous Martian volcano The main planetary topic is a discussion of the thermo- collapses have been proposed, including formation of the mechanical erosion of substrates, including the heat-transfer basal escarpment of Olympus Mons, and arcuate collapses on concepts and ways in which erosion is accomplished. The Downloaded from specialpapers.gsapubs.org on March 5, 2012 spe483-01 page 418 418 Rowland et al. AB500 m C 500 m C B 20 km Figure 20. Tharsis Tholus, Mars, located at 13.2°N, –90.725°E. (A) Viking Orbiter image mosaic, showing the entire volcano, with higher-resolution subscenes B and C outlined. (B–C) High-Resolution Science Experiment (HiRISE) images ESP_012612_1940 and PSP_002169_1940, respectively, showing details of the caldera walls. In C, the height of the caldera wall is ~4 km. Hawaiian Ranchos subdivision, within the ~2500-yr-old P0hue - ‘a‘a (gourd) Bay lava fl ow (Fig. 22; Jurado-Chichay and Rowland, 1995). The tube diameter is ~8 m, which is not particularly - ‘a‘a large. However, in places, the roof of the channel is ~20 m thick (Fig. 23). Along much of its exposed course, the tube has pahoehoe- collapsed completely, to produce a structure that topographi- cally resembles a channel. At the coast, the P hue Bay fl ow hosts a collection of littoral cones, some of which are circular in ‘a‘a- ~1 m planform (Jurado-Chichay et al., 1996a), and resemble recently scoria ‘a‘a- described features on Mars (Lanagan et al., 2001; Fagents et al., scoria 2002; Hamilton et al., 2010). pahoehoe- Objectives If access is granted, this series of skylights and collapses Figure 21. Photograph of the thermally eroded lava tube at Honu‘apo. provides hours of topics to examine and discuss. Examples The top and bottom of the p hoehoe fl ow that hosts the lava tube are include the complex interplay between effusion rate and lava outlined with solid lines; other fl ow boundaries are dashed. surface texture, the limitations of simple numerical models if not applied carefully, and the complexity of fl ow behavior particular planetary examples to reference are lunar sinuous (e.g., a younger fl ow apparently invaded and utilized the tube- rilles and the canali on Venus. Also noteworthy is the prox- channel complex; Jurado-Chichay et al., 1996b). Additionally, imity of this site to the undersea volcano L ‘ihi, and a fi ber- the more circular skylights resemble the newly discovered pits optic data and power cable from the short-lived Hawai‘i on the Moon (Fig. 3D), and whether the lunar pits are skylights Undersea Geo-Observatory (HUGO) on L ‘ihi’s summit that or pit craters (e.g., analog site no. 10) is a good discussion came ashore here. topic here. 16. Large Lava Channels and Tubes in the P hue Bay 17. Upper Part of the Hawaiian Ocean View Estates Flow, SW Flank of Mauna Loa (HOVE) Subdivision One of the most spectacular lava tube and channel systems Upslope from Hwy 11 are the Hawaiian Ocean View in Hawai‘i is located just downslope of the SE corner of the Estates (HOVE), a civil defense nightmare. Some 45 streets Downloaded from specialpapers.gsapubs.org on March 5, 2012 spe483-01 page 419 NASA volcanology fi eld workshops on Hawai‘i: Part 1 419 Figure 22. Large channel/tube systems. (A) Air photo of the P hue Bay tube/channel system (American Soil Conserva- tion Service photo no. EKL-9CC-189; see Fig. 24 for location and note that this photo was taken before the Hawaiian Ranchos subdivision was built). Note the dark-toned ‘a‘ breakout from one of the skylights. Jurado-Chichay et al. (1996b) suggested that this breakout may have been unrelated to that which formed the original tube system. Arrows indicate locations from which Figures 23A and 23B were taken. (B) Image of Hadley Rille, on the Moon. Illumination is from the right (Apollo-15 frame AS15-M-0414). AB Figure 23. The P hue Bay fl ow chan- nel and tube system. (A) View up-fl ow b along a channel-like section of the sys- tem. Note workshop participants at right for scale. Two cross-channel profi les are shown by dashed lines. Note the narrow, partially collapsed bridge (b), which separates this channel section from the next one up-fl ow. (B) View across a large skylight in the tubed section of the system. Note workshop participants (in oval) for scale. Arrows indicate upper- most level of lava veneer produced by the last lava to fl ow through this region of the channel-tube system (see Fig. 22 for location). extend diagonally upslope from the highway, almost to SW rift zone eruption were to break out upslope from HOVE, Mauna Loa’s SW rift zone (Fig. 24). The 1887 lava fl ow and people in the upper reaches of the subdivision would have only both arms of the 1907 lava fl ow (Zimbelman et al., 2008) minutes to evacuate. Nevertheless, the views from this loca- cut through the area, where the average slope is ~10°. If a tion are stunning, and the lots are cheap, so it is diffi cult for Downloaded from specialpapers.gsapubs.org on March 5, 2012 spe483-01 page 420 420 Rowland et al. 18. N Pu‘u a Pele Littoral Cones These cones are hosted in 750–1500-yr-old Mauna Loa lava fl ows (Wolfe and Morris, 1996). At least fi ve cones and cone remnants are visible in high-spatial-resolution imagery (Fig. 25). Cross sections of the cones are well exposed in a low coastal cliff. Objectives Because of the many cones, cone morphologies, and out- crops in this area, it is well worth spending a full day. Topics to dis- cuss include the nature of fuel-coolant (lava-water) interactions, the methods used to differentiate between secondary and primary pyroclastic features and deposits in images and out- crops, and issues relating to water availability on Mars, where fi elds of small circular cones have been mapped and interpreted as having a rootless origin (e.g., Fagents et al., 2002; Hamilton et al., 2010). 19. Guided Mapping Exercise on Mauna Loa’s NE Flank Along a stretch of the access road to the Mauna Loa Solar Observatory, there is a series of completely unvegetated lava fl ows that provide a variety of surface types, structures, and ages. Importantly, some high-spatial-resolution (~8 m per pixel) thermal infrared images are available for this site, which can be processed into a principal component (PC) image (Fig. 26). This is a classic area for studying the character of basaltic lava fl ows in thermal infrared data (Kahle et al., Figure 24. Shaded relief image (illuminated from the NW and 45° above 1988; Abrams et al., 1991). We have found that it is extremely the horizon, created from a U.S. Geological Survey 10 m digital ele- instructive for workshop participants to walk along the road vation model; http://hawaii.gov/dbedt/gis/hill.htm). Solid white lines and “navigate” by means of the PC image as well as 1 m spatial- are roads (from http://hawaii.gov/dbedt/gis/haw_street_centerlines. resolution IKONOS images. htm), which highlight the locations of the Hawaiian Ocean View Es- tates and Hawaiian Ranchos subdivisions, immediately downslope from Mauna Loa’s SW rift zone. Black areas (with white stippling) are Objectives post–1800 A.D. lava fl ows, with ages indicated (Trusdell et al., 2005). The objective here is to gain an understanding of the Also shown are Pu‘u Hou (new hill), Pu‘u K (Ti plant hill), and subtle yet detectable differences on basaltic surfaces that N Pu‘u a Pele (the hills of Pele) littoral cones. arise from different fl ow textures and exposures to weather- ing. The very different characteristics of the fl ows that are apparent in thermal infrared wavelengths are important con- people to resist settling here. Some of the 1887 vents are only cepts for participants who will be using THEMIS (Thermal a 20 min walk from the uppermost streets, and during our third Emission Imaging System) infrared data in Martian volcanic workshop, we spent most of a day wandering among the cones regions. and shelly p hoehoe, discussing these structures. In the NE quadrant of HOVE itself, there is a large scoria cone that is 20. Saddle between Mauna Loa and Mauna Kea, Mauna being quarried, offering excellent exposures of the interior of Kea Scoria Cones the structure. The summit of Pu‘u Huluhulu (bristly hill) offers, on Objectives a clear day, excellent views of both Mauna Kea and Mauna This is a good place to discuss rift zone activity, including Loa. The profi les of the two volcanoes can be compared, and rift volcanism on Beta Regio (Venus) and the rift that extends their differences discussed (Fig. 27). Mauna Loa, being in from Ascraeus Mons through Pavonis Mons, and then across its active tholeiite shield stage, erupts with fountains a few Arsia Mons, on Mars. tens to hundreds of meters high, resulting in small scoria/ Downloaded from specialpapers.gsapubs.org on March 5, 2012 spe483-01 page 421 NASA volcanology fi eld workshops on Hawai‘i: Part 1 421 A Pu‘u Ki- B - Na Pu‘u a Pele 1887 flow D Pu‘u Kahakahakea 500 m C - Pu‘u Waimanalo 1868 500 m flow D Pu‘u Kaimu‘uala ~3 m Pu‘u Hou 500 m E F 1 km Figure 25. Littoral cones. (A–C) Portions of American Soil Conservation Service photo nos. EKL- 1CC-70, EKL-13CC-4, and EKL-14CC-16, respectively, showing three clusters of littoral cones on Mauna Loa’s SW coastline (see Fig. 24 for locations). Associated fl ow ages (Wolfe and Morris, 1996) are as follows: Na Pu‘u a Pele, 1500–750 yr B.P.; Pu‘u K , 1500–750 yr B.P.; Pu‘u Kahaka- hakea (maybe “white-lined hill”), 10,000–3000 yr B.P.; Pu‘u Kaimu‘ula (maybe “the red oven hill”), 10,000–3000 yr B.P.; Pu‘u Waimnalo (potable water hill), 10,000–3000 yr B.P.; and Pu‘u Hou, 1868 A.D. fl ow. (D) A typical outcrop in one of the Pu‘u K cones (see arrow in B for location), showing coarse and fi ne particles, as well as a prominent unconformity. (E) The long road that members of our 2005 workshop trudged to N Pu‘u a Pele. (F) Probable rootless cones sitting on the surface of a platy-ridged lava fl ow in southern Elysium Planitia, Mars (Mars Global Surveyor Mass Orbital Camera [MGS MOC] release no. MOC2-186). spatter cones and voluminous, long lava fl ows. From a dis- of Mauna Loa (Figs. 27A–27C). Mauna Kea was glaciated tance, the cones along the rift zone profi le are barely discern- at least three times, and this has complicated its topographic ible. Mauna Kea, however, in its postshield alkalic stage, profi le (Porter, 1987; Wolfe et al., 1997; Moore and Mark, erupts cooler, gas-rich lava, resulting in large scoria cones 1992; Rowland and Garbeil, 2000). Pu‘u Huluhulu itself is a and shorter, more stubby lava fl ows. The result is a volcano Mauna Kea scoria cone that has been surrounded by Mauna profi le that is considerably more bumpy and steep than that Loa lavas, most recently by infl ated tube-fed p hoehoe of the Downloaded from specialpapers.gsapubs.org on March 5, 2012 spe483-01 page 422 422 Rowland et al. E C . d R e l d d d d a a S S C B - - - - 1855–56 pahoehoen - o i Pris - lan 1935–36 pahoehoe u 1880–81 pahoehoe K ‘a‘a A 1899 ‘a‘a 1899 G D N M.L. Observatory F 1 km Figure 26. Principal component (PC) image of thermal infrared mapping spectrometer (TIMS) data for a portion of the NE fl ank of Mauna Loa (portion of fl ight line 24, collected April 1985; Karas et al., 1994). Note that young p hoehoe fl ows produce vivid colors in this stretch, whereas young ‘a‘ fl ows are a relatively featureless green. Our typical plan is to walk from A to B, which is slightly downhill (photo inset C), comparing the fl ows in the fi eld to both the TIMS PC and 1 m panchromatic IKONOS images. In 2003, we extended this exercise to C and then D, which was probably a mistake. From C to D is all uphill, and most of that walk was completed in rain and fog (photo inset E). Insets F and G are examples of the IKONOS data. 1935–1936 eruption. There are excellent examples of infl a- cones on Mars, and possibly the formation of the dark halo tion features in this 1935–1936 fl ow, including lava rise pits deposits on the Moon. that expose the underlying surface (Fig. 27D; Walker, 1991, 2009), and an old cattle wall, the top of which is now lower 21. Mauna Kea Scoria Cones than the infl ated lava surface (Fig. 27E). Walking around the west side of the cone into the partially quarried crater, there From the summit of Pu‘ukalepeamoa (comb of the chicken are views of complex scoria-lava contacts within the cone. hill), a small, spindle-bomb–rich scoria and spatter cone near the Ellison Onizuka Center for International Astronomy, there Objectives are fi ne views downslope to lower- elevation Mauna Kea This is a good location to observe and discuss infl a- cones (Fig. 28). These cones exhibit a variety of morphologies tion of lava fl ows and the complex interior structure of a depending on their erosional modifi cation (e.g., Wood, 1980a, scoria cone, and to discuss the time-variable nature of 1980b), relative amounts of spatter versus scoria, and degree of high-fountaining eruptions as they may relate to volcanic interaction with associated lava fl ows. Downloaded from specialpapers.gsapubs.org on March 5, 2012 spe483-01 page 423 NASA volcanology fi eld workshops on Hawai‘i: Part 1 423 KAILUA, WAIMEA Mauna Kea Observatories D A MK Pu‘ukalepeamoa Ellison Onizuka Figure 27. The Mauna Kea–Mauna Loa Center saddle. (A) Shaded relief image of the saddle, showing Mauna Kea (MK) and SaddleSad d le Mauna Loa (ML; illuminated from the RRd. d. NW and 45° above the horizon, created HILO from a U.S. Geological Survey 10 m Pu‘u Huluhulu digital elevation model; http://hawaii .gov/dbedt/gis/hill.htm). (B) Mauna Kea viewed from the north fl ank of Mauna Loa. Examples of deeply gullied mo- Area of E Mauna Loa Fig. 25 raines (m) and large scoria cones (s) are Solar and Weather indicated. (C) Mauna Loa viewed from Observatory ~2 m near the summit of Mauna Kea. Spatter/ scoria cones (s) and Moku‘weoweo zone (‘ weoweo [a red fi sh] section) cal- NE rift Moku‘aweoweo- dera (c) are indicated. In A–C, note the very different morphologies of these ML two shield volcanoes, with Mauna Kea 10 km possessing numerous very large scoria N cones and steeper gullied slopes. In contrast, the scoria cones along Mauna B s Loa’s NE rift zone are barely visible. m (D) Photo showing a participant in our 2010 workshop studying a lava-rise pit within the 1935–1936 Mauna Loa p hoehoe fl ow, just NE of Pu‘u Huluhu- lu. The older surface in this instance is rough, spalled p hoehoe, outlined by a dotted line for clarity, around which the 1935–1936 lava has infl ated by ~1 m. (E) Photo from the top of Pu‘u Hu- luhulu of the top of an old cattle wall c (dashed line) near the west base of the C s cone. The 1935–1936 lava approached the wall from the west (i.e., toward the viewer) and infl ated by as much as 2 m in places before overtopping it. A B Figure 28. Views downslope (A) and upslope (B) from Pu‘ukalepeamoa. In A, note the various stages of erosional rounding of the scoria cone crater rims and fl anks. The rim of the crater of the nearest cone is ~400 m across. In B, the prominent unit with downslope-parallel dark and light streaks is a lava fl ow that postdates the most recent glacial deposits (Wolfe et al., 1997). The dark streaks are outcrops of blocky ‘a‘ lava, and the light streaks are talus. The buildings in the lower right corner are the Hale P haku astronomy facility. Downloaded from specialpapers.gsapubs.org on March 5, 2012 spe483-01 page 424 424 Rowland et al. A B e - Pu‘u Anahulu Kiholo aikoloa Bay Kawaiha W D Hwy. 19 Kailua Pu‘u Figure 29. Trachyte on Hual lai. C (A) Simulated true-color Landsat image (a portion of a cloud-free mosaic avail- Anahul able online at http://hawaiiview.higp .hawaii.edu/mosaics.htm.) Note the light color of weathered trachyte at the distal (north) end of Pu‘u Anahulu. (B) Shaded u relief image (illuminated from the NW and 45° above the horizon, created from a U.S. Geological Survey 10 m 4 km Pu‘u digital elevation model; http://hawaii Wa‘awa‘a .gov/dbedt/gis/hill.htm); dashed box indi- C cates area of A, and arrows indicate loca- tions and directions from which photos C C and D were taken. C was taken look- Hwy. 190 ing upslope from just off Hwy 190, and D was taken from the coastline at K holo (fi shhook) Bay. (E) Magellan radar im- age of lava domes on the eastern fl ank of Alpha Regio, Venus (Magellan press release image P-37125). N Pu‘u 4 km Wa‘awa‘a D E ~200 m ~25 km Objectives upper surface. These have an amplitude of a few tens of meters View a variety of pyroclastic constructs in varying states of and wavelengths of 100–200 m. All of Pu‘u Wa‘awa‘a and most of erosion, and discuss volcano-ice interactions. Pu‘u Anahulu are contained in the Pu‘u Wa‘awa‘a ahupua‘a (land division), which recently reverted to state of Hawai‘i management 22. Trachyte Pumice Cone and Lava Flow on North Flank after many decades of cattle grazing. The ahupua‘a is home to of Hual lai many rare and endangered plants and birds, and, unfortunately, a huge number of invasive species as well; efforts are being made to The ~105,000-yr-old trachyte pumice cone (Pu‘u Wa‘awa‘a— restore the ecosystem (Giffen, 2009). An old pumice quarry near furrowed hill) and lava fl ow (Pu‘u Anahulu—ten-day hill; Fig. 29) the NE base of Pu‘u Wa‘awa‘a offers the opportunity to see both comprise the largest single erupted volume on any Hawaiian pumice and obsidian. volcano (e.g., Moore et al., 1987). Pu‘u Wa‘awa‘a is purely pyro- clastic, with radial gullies cut into its fl anks. The Pu‘u Anahulu Objectives lava fl ow is ~9 km long, and, in places, it is 200 m thick. From the This is a good location to talk about evolved magmas on air, prominent convex-downslope pressure ridges are visible on its basaltic shield volcanoes, and the viscosity of their lava fl ows, Downloaded from specialpapers.gsapubs.org on March 5, 2012 spe483-01 page 425 NASA volcanology fi eld workshops on Hawai‘i: Part 1 425 to initiate a discussion of pancake domes on Venus and the Gru- (e.g., Gulick, 2001; Gulick and Baker, 1990) or may not (Lamb ithuisen dome and the Marius Hills on the Moon, and to explore et al., 2007) have developed via sapping. the idea that evolved magmas may have erupted on these bodies too. We point out that although the planimetric shape of Pu‘u RECOMMENDATIONS FOR PLANNING FIELD Wa‘awa‘a is similar to that of a lava dome (such as those that WORKSHOPS have been interpreted to be lava domes on Alpha Regio, Venus), it is actually Pu‘u Anahulu that is lava. After running ten successful workshops, we have devel- oped some valuable insights into what does or does not work for these projects. The following suggestions are our best advice 23. Waipi‘o Valley Overlook, Kohala for other investigators who are considering similar workshops: Waipi‘o (curved water) Valley is a prominent amphithe- 1. Start all logistical planning early. Even before the funding is ater-headed valley that has cut far into the fl anks of Kohala in hand, make tentative reservations for lodging and arrange- volcano (Fig. 30). The valley cuts southwestward from a high ments for food. You should also submit any permits and/or cliffed coastline and, ~6 km inland, makes an almost 90° turn permission letters that may be required to access otherwise to the northwest. This bend is the result of erosion having closed areas (e.g., the active fl ow fi eld) or private lands. Pre- preferentially exploited faults (Stearns and Macdonald, pare your workshop announcement fl yer so that it can be 1946). The head of the valley is not visible from the overlook distributed the moment you know that you will be funded. (and is almost always shrouded in clouds anyway), but it is a 2. Once notifi ed that your workshop will be funded, do your classic example of a Hawaiian amphitheater-headed valley. best to get the money from the funding source early, or at least on time. We once had to postpone a workshop for a Objectives year because by the time we received both notifi cation of This is a good location to discuss the cutting of large funding and the actual funds, there was insuffi cient time valleys into basalt volcanoes and the possibility that they may for adequate planning. A -- B Hawi - - Pololu Honokane Figure 30. Large valleys on Kohala Waipi‘o and Mars. (A) Shuttle Imaging Radar- imanu C (SIR-C; data taken 122.20, 16 April Wa aipi‘o 1994, 22:42:18 GMT) image overlain faults W faults on a shaded relief image (illuminated from the NW and 45° above the horizon, created from a U.S. Geological Survey 10 m digital elevation model; http:// hawaii.gov/dbedt/gis/hill.htm). Waipi‘o, Kawaihae Waimea Waimanu (bird water), Honok ne (K ne’s bay), and Polol< (long spear) 5 km are indicated, as are a few of many nor- C 2 km mal faults, downdropped to the SW, Hadriaca Patera which are controlling the orientations of D Waipi‘o and Honok ne. The dotted box indicates the location of B. (B) Shaded relief image of Waipi‘o and Waimanu valleys. (C) Mars Global Surveyor im- age no. MGS-M-MOC-NA/WA-2-DS- DP-L0-V1.0 (red visible light), show- ing Dao and Niger Valles on the south Dao Vallis fl ank of Hadriaca Patera, Mars. The dotted box indicates the location of D. (D) Portion of Thermal Emission Im- aging System (THEMIS) visible image V25970005, showing the headwall of allis rV Dao Vallis, Mars. Nige 100 km 2 km Downloaded from specialpapers.gsapubs.org on March 5, 2012 spe483-01 page 426 426 Rowland et al. 3. Advertise early, and give applicants detailed instructions discussions wander where they may. This is much more about required elements in their applications. Make sure productive than giving long preplanned speeches. they are aware of the physical demands involved in fi eld 10. Provide some down time. Do not plan formal talks in the work. This is particularly the case if the weather turns bad evening when everybody is exhausted from the day’s efforts. or the active lava fl ows are a long hike away from the trans- 11. Give some thought to your overall schedule so that partici- portation; warning potential participants multiple times that pants do not face long hikes or long drives on successive this is not a driving fi eld trip is key! Most of our participants days. have been perfectly happy out in the fi eld, but on a few occa- 12. Learning is plenty—do not feel the need for a “product” sions, there have been participants who were not physically such as a group paper. or mentally prepared for the effort that is required. 13. Have the participants actively participate, and not merely 4. Once applicants are selected, send information early about listen or discuss. The mapping project is one example, as what to bring, what to read, what to expect, etc., and again are outcrop interpretations, isopach derivations, etc. warn about physical effort. Encourage them to break in 14. Provide a detailed schedule that lists where each day’s new boots, and discourage them from expecting to sus- activities will be, what they will entail (driving, hiking, tain electronic contact with the rest of the world during the etc.), which images in their handout, pages in the fi eld workshop; fi eld trips work on their own schedule and do guide, and references are pertinent, etc. The better the par- not wait for checking e-mail, running telecoms, or taking ticipants know what to expect, the better prepared they will breaks for Mauna Kea observations. be for the activities of the day, and the better they will deal 5. Make reading materials available online. It is great if the with changes in the plan that may be necessary. participants read everything, but they will be busy people, 15. Pick your leader team with regard to scientifi c background so list papers in order of priority. and compatibility. These team leaders may also be expected 6. Include a mapping project. The supporting image data to drive long distances, so they should have a “tour leader must be sent out early (at least 4 wk before the start of the mentality” (i.e., willing to discuss geology, plants, culture, workshop), with explanations of the data sets and the meth- science, lousy radio stations, etc.) to make these journeys ods used to process them (for those participants who may tolerable. be unfamiliar with certain remote-sensing technologies). 16. Keep all participants involved and pay attention to folks 7. Do not plan too much activity. This includes not who appear to be consistently left out of discussions. packing every day with dawn to dusk driving stops and 17. Utilize participant evaluations, particularly when planning hikes. The best learning during a workshop takes place your next workshop. These evaluations are valuable met- during discussions at outcrops and overviews, and it is rics for assessing the success of the workshop, and they counterproductive to feel that these need to be hurried in provide supplemental information for future workshop order to stay on a tight schedule. proposals and for tenure or promotion applications. 8. Have contingency sites and activities in case of bad 18. Learn something new yourself and have fun! Include at weather, bad roads, active lava fl ows, lack of active lava least one site that you have visited only rarely or a topic fl ows, or other access problems. that is new to you—somebody will know something about 9. Do not script your fi eld presentations. The beauty of fi eld it. A happy organizer makes the whole workshop experi- workshops is, after brief introductions to a site, to let ence that much more enjoyable for the participants. Downloaded from specialpapers.gsapubs.org on March 5, 2012 spe483-01 page 427 NASA volcanology fi eld workshops on Hawai‘i: Part 1 427 APPENDIX 1. LOGISTICS FOR EACH FIELD SITE noitacoL erehtgnitteG ropmetdnalaitapS al scale Comments and considerations 1. Kapoho From Hilo, head SW (toward Volcano) on Hwy 11. Depending on the time available, The dirt road to the lighthouse is passable Turn left at the Kea‘au bypass. Go through or minutes to hours can be spent at in a regular car. Toothpaste lava is very around P hoa (dagger), and turn left at Hwy 132. Kapoho. The best toothpaste sharp and abrasive, and proper footwear The intersection of State Hwy 132 and 137 is lava examples are near the is essential. The eruptive vents are NW within the 1960 Kapoho flow field and prior to lighthouse, but some can be of the highway intersection, but are January 1960 was the center of town. A dirt road found near the highway being quarried away for decorative extends east from this intersection to the Kapoho intersection. scoria. The vents are on private land lighthouse, which was surrounded on two sides by and should not be trespassed. excellent examples of toothpaste lava. 2. Ka 428 Rowland et al. APPENDIX 1. LOGISTICS FOR EACH FIELD SITE (Continued) noitacoL erehtgnitteG elacslaropmetdnalaitapS snoitaredisnocdnastnemmoC 7. K lauea Iki, Access to Pu‘u Pua‘i and the K lauea Iki overlook is The K lauea Iki crater hike should Make sure participants carry sufficient Pu‘u Pua‘i via a short road that cuts off from Crater Rim Dr., be given 3–4 h in order to see all water. Although the hike may start out in ~4 km clockwise from the national park entrance. the features along the way. If a drizzle, chances are it will become A 10 min hike from the Pu‘u Pua‘i parking lot along only the overlooks are visited, sunny later, and the hike out of K lauea the Devastation Trail takes you through the then the combination of them Iki is strenuous. proximal part of the 1959 scoria deposit. You can plus the Devastation Trail hike shuttle your cars to the Devastation Trail parking can take as little as half an hour. lot to meet the hikers. From the Devastation Trail parking lot, a 5 min walk NW toward the caldera will bring you to the collapse pits, just before a low rise. The hike across K lauea Iki crater starts at the N Huku parking lot, switchbacks into K lauea Iki, then across the crater floor, and up out the other side. 8. N Huku N Huku is located ~3 km clockwise along Crater The lighted portion of the lava The first ~100 m of N Huku is lighted and Rim Dr. from the park entrance. The parking lot is tube takes as little as 15 min to heavily traveled, so many small-scale usually quite full between the hours of 10 a.m. and hike through. Continuing on tube features have been worn away. 2 p.m., so you should try to avoid those times. requires an additional 30 min. However, an additional, more interesting ~200 m is available for exploration with a flashlight, but sturdy shoes and gloves are recommended here. 9. K lauea The Hawaiian Volcano Observatory (HVO) and the A thorough view and discussion The museum has a bookstore with a good caldera and Jaggar Museum are located ~5 km of the caldera from the Jaggar selection of popular and scientific titles, Hawaiian counterclockwise around Crater Rim Dr. from the Museum requires 10–20 min, but plus a variety of posters, patches, Volcano park entrance. you should give participants T-shirts, and other national park Observatory plenty of time to admire the view. paraphernalia. The museum itself requires an additional 20–30 min. 10. Devil’s Devil’s Throat is ~80 m NE of the intersection of From the intersection of the two The National Park Service discourages Throat pit Chain of Craters Rd. and Hilina Pali Rd. roads, it is a 5 min walk to Devil’s visits to the crater because it is very crater Throat, but be extremely careful hazardous, and extreme care should be when approaching the edge, and taken near the edges. There are do not linger. It is instructive to numerous crater-parallel fractures, examine the fractures that lead indicating that large blocks are poorly from the south wall of Devil’s supported and liable to fall in. Throat SW to Chain of Craters Additionally, invasive ground-nesting Rd. and beyond. wasps live in the area. They are aggressive and their stings are quite painful for a long time. 11. K lauea SW The SW rift zone fractures are ~3 km beyond HVO Examination of the fractures, from The floors of the fractures are somewhat rift zone along Crater Rim Dr. They extend perpendicular to their edge and from their floor uneven, so good footwear is fractures the road in both directions. takes 10–40 min. recommended. Note that this part of the park has been closed since March 2008 due to high levels of SO2. 12. Keanakko‘i The easiest access to this region is by walking SW Examination of the caldera- Some of the Keanakko‘i ash areas are ash, sandwash, from Crater Rim Dr. across the September 1982 proximal parts of the somewhat featureless, and can become upper SW rift lava flow, which ponded in the southernmost part Keanakko‘i deposit requires at disorienting. There is shelly phoehoe zone of the caldera. The easiest access to the Koa‘e least an hour. The hike to the near the 1974 vents, so boots, long fault zone and the middle part of the 1974 flow is 1974 vents and back adds pants, and gloves should be worn. Carry via the Mauna Iki trail, off Hilina Pali Rd. another 2 h. sufficient water if you plan to hike that far or farther. Note that this part of the park has been closed since March 2008 due to high levels of SO2. 13. Mauna Iki Mauna Iki is accessible via the Ka‘< Desert A full day is required to see all of Participants navigating by themselves trailhead, which is along Hwy 11, ~17 km SW of the surficial and structural should be equipped with GPS receivers the national park entrance (entry to the park is not features of Mauna Iki, especially and two-way radios, and should know necessary). if participants have produced how to use them. There is ‘a‘ and their own maps that they want to shelly phoehoe in the mapping area, so ground-truth. long pants, boots, and gloves are necessary. This trail and the Mauna Iki area were closed by the National Park Service from 2008 to 2009 due to high levels of SO2; inquire at park headquarters to be sure the trail is open. 14. N nole Hills Access to the N nole Hills themselves is difficult, The discussion of volcano Be careful of fast highway traffic. and involves permission from private landowners. instability, recovery, and It is much more useful to view them from the resurfacing can take 10–30 min, intersection of Hwy 11 and the road to Punalu‘u, depending on the interests and ~6 km southwest of P hala (cultivation by burning backgrounds of the participants. mulch). (Continued) Downloaded from specialpapers.gsapubs.org on March 5, 2012 spe483-01 page 429 NASA volcanology fi eld workshops on Hawai‘i: Part 1 429 APPENDIX 1. LOGISTICS FOR EACH FIELD SITE (Continued) noitacoL erehtgnitteG ropmetdnalaitapS al scale Comments and considerations 15. Lava tube at Honu‘apo, also known as Whittington Beach Park, The discussion of thermal erosion Do not leave valuables in your vehicle. Honu‘apo is just off Hwy 11, ~10 km south of Phala. The and L0‘ihi can take 20–40 min, outcrop is visible from the south end of the park, depending on the interests and near the ruins of an old pier. backgrounds of the participants. 16. P0hue Bay The tube and channel system is best exposed From the SE corner of the Although there are roads and trails in this flow downslope of the Hawaiian Ranchos subdivision, Hawaiian Ranchos subdivision, area, it is advisable to be prepared to ~15 km west of N ‘ lehu (the volcanic ashes). The the lava tube and channel walk over ‘a‘ lava flows, so boots, area is privately owned, and access is complicated system is 10 min walk over gloves, and long pants are necessities. by conflicts between adjoining landowners. The rough lava and gravel roads. tube and channel system itself is on land managed Following the system another km by Yamanaka Enterprises (808) 935-9766. Access or so is instructive, and will via the Hawaiian Ranchos subdivision can be require 2–3 h round-trip. arranged via the Hawaiian Ranchos Road Maintenance Corp. (808) 989-4140. 17. Hawaiian Hawaiian Ocean View Estates is upslope of Hwy 11 Driving from the highway to the The quarry is private property, so you Ocean View from ~15 to ~20 km west of N‘lehu. The roads scoria cone takes 15–20 min, must not leave the shoulder of the road. Estates are in a diagonal pattern, so getting to the top of and another 30 min can be used Additionally, at times there are very the subdivision requires zigzagging up the slope. discussing the pyroclastic steep drop-offs near the road edge. The quarried scoria cone is in the NE (upper-right outcrops and the proximity of as you head uphill) portion of the subdivision houses to the SW rift zone. bounded by Lurline Ln., Mahimahi Dr., Liliana Ln., and Kailua Blvd. 18. N Pu‘u a N Pu‘u a Pele is accessible via a poor-quality four- The drive to the cones from the The road really is bad, so unless you have Pele wheel-drive road (the “Road to the Sea”), which highway is slow because of the a high-clearance four-wheel-drive intersects Hwy 11 ~20 km west of N‘lehu. The road’s poor quality, and it will vehicle, do not attempt to drive beyond cones are within Manuk (blundering) Natural require at least an hour each the first ~4 km., and even this upper Area Reserve. A special use permit must be way. An entire day can easily be portion is barely passable by a regular obtained for groups of 20 or more: spent wandering among the vehicle. http://hawaii.gov/dlnr/dofaw/nars/permit-guidelines. cones. 19. Mauna Loa The road to the Solar Observatory heads south off The walk from a prominent bend The Solar Observatory road is narrow and NE rift zone Saddle Rd. (Hwy 200) ~46 km west of Hilo. The in the road ~15 km from the barely paved, and most rental car mapping turnoff is ~200 m east of Pu‘u Huluhulu, a Saddle Rd. intersection downhill contracts prohibit driving on unimproved exercise prominent scoria cone. to a cinder quarry access road roads. This area is often clouded-in by takes a couple hours if you stop 11 a.m., and the weather can change and discuss most of the flows from warm and sunny to very cold and and flow margins that are rainy in only a few minutes. Be prepared encountered along the way. for both intense sun and cold rain. 20. Mauna Loa, Pu‘u Huluhulu is just south of Saddle Rd. (Hwy A walk around the cone to view Please be sure to close the gate near the Mauna Kea 200), ~46 km west of Hilo, ~200 m west of the inflation features and the scoria parking area so that feral goats don’t get saddle road to the Mauna Loa Solar Observatory, and outcrops in the old quarry will into the Pu‘u Huluhulu reserve. immediately across from the road to the Mauna take 30–40 min. Kea summit. From the parking lot, the inflation features are immediately to the west. A short trail leads through a gate and around the west flank of the cone to the old quarry, and then continues up counterclockwise to the cone’s summit. 21. Mauna Kea The road up Mauna Kea is an obvious right (north) The drive from Hwy 200 to the The road up Mauna Kea is paved as far scoria cones turn off the Saddle Rd. (Hwy 200), immediately Onizuka Center takes ~20 min, as the Onizuka Center, but it is quite across from Pu‘u Huluhulu. The Onizuka Center is and it is worth spending some steep. Cars will be slow, even in low ~10 km up from this intersection. The dirt road to time in the center itself. The hike gear. Low gear is especially important the upslope base of Pu‘ukalepeamoa is ~200 m up the flank of Pu‘ukalepeamoa on the way down because of the downslope from the Onizuka Center parking lot, on takes ~10 min. steepness—do not rely only on your the west side of the road. brakes! The road upslope from the Onizuka Center is unimproved, and a high-clearance vehicle is required. There are plenty of already broken spindle bombs along the trail to the summit of Pu‘ukalepeamoa, and many of them are cored with mafic and ultramafic xenoliths. There is no need to break open any more, so please don’t. 22. Trachyte on Both the pumice cone and lava flow can be viewed Discussion of Huallai at the Access to the pumice quarry must be Huallai easily from a small pullout along M malahoa highway pullout can take 10–30 obtained in advance from the State of (splintered paddle or splintered friendship) Hwy min, depending on the Hawai‘i Department of Land and Natural (Hwy 190), ~100 m west of a prominent bend in participants. The drive to the Resources: (808) 937-2501. the road. There is a locked gate (that leads to the pumice cone and back plus time pumice quarry) and sufficient space for 3–4 to look at the exposures requires vehicles to pull over safely. about an hour. 23. Waipi‘o The Waipi‘o Valley overlook is at the end of Hwy From Honoka‘a, the drive to Do not leave any valuables in your vehicle Valley lookout 240, which branches off of Hwy 19 at the town of Waipi‘o and back takes about an at the Waipi‘o Valley overlook. Honoka‘a (rolling [stones] bay). hour and a half. Downloaded from specialpapers.gsapubs.org on March 5, 2012 spe483-01 page 430 430 Rowland et al. APPENDIX 2. PARTICIPANTS IN THE WORKSHOPS Jennifer Piatek, Jani Radebaugh, Julie Rathbun, Shauna Riedel, James Skinner, Karen Stockstill, Leslie Tamppari, The following lists the 142 participants in our 10 work- Michael Wyatt. shops. Many of the names are familiar as prominent, produc- “For those who’ve stayed on course for Mars and other tive, young (or not-so-young) planetary scientists. It is always planets, I guess the main thing is to remember a little humility... a pleasure to see one or more of these names on author lists, remote sensing can’t teach you everything.” —Bethany Brad- instrument teams, and NASA press releases, and feel that ley, Princeton University maybe some tiny bit of their fi eld experience in Hawai‘i helped 2003. Jacob Bleacher, Joseph Boyce, Joshua Cahill, Tab- get them to where they are today. We have included a few com- batha Cavendish, Andrew Dombard, Melissa Farley, William ments about their fi eld-trip experiences. Garry, Cheryl Goudy, Brian Hynek, Amy Knudson, Will Koep- 1992. Duane Bindschadler, Nathan Bridges, Barbara Bruno, pen, Nicholas Lang, Aisha Morris, Cara Mulcahy, Jim Rice, Bryan Butler, Robert Craddock, David Crown, Annette deCharon, Deanne Rogers, Valerie Slater, Livio Tornabene. Tracy Gregg, Brad Henderson, Lynn Hultgrien, Noam Izenberg, “I would say that the workshop has contributed most to Paul Johnson, Patrick McGovern, Jeffrey Plaut, Mike Ramsey, my skills in the fi eld (identifying geologic features on a map, Trish Rogers, Susan Sakimoto, Michelle Tatsumura, Cynthia etc.). It has also contributed a lot to my ability to teach intro Wilburn. Guests: Bruce Campbell, Vince Realmuto, Jim Garvin. labs—students are very interested in seeing pictures of their “I had been studying planetary volcanology for 2 or 3 years, TA braving things like lava fl ows/tubes/etc., and they seem to and had yet to see a real basalt fl ow! The workshop allowed be more interested in the samples of basalt that I collected me to fi nally put the planetary images in a mental context.” in the fi eld.”—Cara Thompson, University of Tennessee, —Tracy Gregg, associate professor, State University of New Knoxville. York at Buffalo “I work mostly on Mars, but even when working with ter- “As a participant of the fi rst of these workshops, I can restrial data sets, I have a much clearer idea of what might attest to their importance to my own work in planetary science. be happening on the surface. Hands-on (and feet-on) experi- I have also seen their value for my colleagues and students.” ence hiking over the different lava fl ow textures (even the much —David Crown, senior scientist, Planetary Science Institute despised rainy death march on Mauna Loa from our year) 1995. Ben Bussey, Jeffrey Gillis, Diane Hanley, Matt really made a difference in my ability to interpret images.” Peitersen, Louise Prockter, Susan Sakimoto, Selima Siddiqui, —Amy Trueba Knudson, Bellevue College Cathy Weitz, Kevin Williams. “This workshop was one of the best experiences I had in “Also I’ve met lifelong colleagues at your workshop. Louise my training as a planetary scientist. There is not a lot of plan- Prockter—who I’m now on the MESSENGER mission with, Kevin etary fi eld work, especially so for a planetary geodynamicist Williams—who I wrote a successful Lunar Reconnaissance Orbiter like myself (who mainly sits in front of a computer), so getting proposal with, Cathy Weitz who was also studying the Moon at that out to see these things has been incredibly useful.” —Andrew time but I didn’t know and I still chat with her at conferences, and Dombard, Carnegie Institution Susan Sakimoto who I talk to at conferences and might do work 2005. Alice Baldridge, Sarah Black, Devon Burr, Shelby with eventually. I might get one of Susan’s undergraduates to come Cave, Matt Chojnacki, Frank Chuang, Colin Dundas, Tasha here to grad school.” — Jeffrey Gillis-Davis, assistant researcher, Dunn, Jeffrey Hanna, Jennifer Lougen, Joe Michalski, Melissa University of Hawai‘i Nelson, Nathaniel Putzig, Mike Rampey, Mindi Searls, Sharon 1997. Steve Anderson, Mary Chapman, Vicki Hansen, Wilson, Danielle Wyrick. Guest: Steve Baloga. Catherine Johnson, Pat McGovern, Jeff Plaut, Sue Smrekar, “The necessity of correlating remote sensing data to what Ellen Stofan, Ken Tanaka, Maria Zuber. is actually occurring on the ground is often overlooked in this 1998. Mark Bullock, Sarah Fagents, Rebecca Ghent, fi eld. This workshop goes a long way toward reminding us Amitabha Ghosh, Martha Gilmore, Vicky Hamilton, Jeff John- planetary geologists to look under our feet before we start wav- son, Peter Lanagan, David Lescinsky, Jean-Luc Margot, Dave ing our arms about in space.” —Danielle Wyrick, Southwest Senske, John Stansbury, Aileen Yingst. Research Institute “...this workshop was the fi rst fi eld work I ever did. How “I often think of the things I learned in the workshop, which sad is that?...For someone who wrote an entire thesis chapter I found to be among the best fi eld experiences I’ve ever had... on lunar lava ponds, fi nally seeing an actual potential Earth Additionally, I made several new contacts at the workshop and analog was intensely revealing....” —Aileen Yingst, professor, often run into these same people at conferences and meetings.” University of Wisconsin–Green Bay —Nathaniel Putzig, Southwest Research Institute 1999. Brian Banks, Jeffrey Byrnes, David Finnegan, John “I think the biggest thing I gained was just understanding Grant, Elissa Koenig, Laurent Montesi, Matthew Staid, Eliza- how basaltic volcanism works and seeing the geologic beth Turtle, Duncan Young, Cathy Weitz. structures/materials in the fi eld. I found the last day (I think), 2001. Mary Sue Bell, Ross Beyer, Leslie Bleamaster, where we went out in the fi eld and mapped out units using sat- Beth Bradley, Cari Corrigan, Cathleen Donovan, Amy Sny- ellite images, is a good exercise to how we would map using der Hale, Saswata Majumder, Brian Meyer, Keith Milam, images of Mars.” —Frank Chuang, Planetary Science Institute Downloaded from specialpapers.gsapubs.org on March 5, 2012 spe483-01 page 431 NASA volcanology fi eld workshops on Hawai‘i: Part 1 431 “I have only good things to say about your workshop from Ocean and Earth Science and Technology (SOEST) publica- ages past...learning more about volcanology helps in all types tion 8019 and Hawai‘i Institute of Geophysics and Planetology of planetary research, not only Mars. And getting to go out in (HIGP) contribution 1871. the fi eld is an all-too-infrequent experience for us planetary types.” —Devon Burr, University of Tennessee REFERENCES CITED 2008. Joel Allen, Ryan Anderson, Lynn Carter, Ole Gus- Abrams, M., Abbott, E., and Kahle, A., 1991, Combined use of visible, refl ected tafson, Miguel Pablo Hernández, Debra Hurwitz, Seth Kadish, infrared, and thermal images for mapping Hawaiian lava fl ows: Journal of Laura Kerber, Lucy Lim, Paula Martin, Liz Rampe, Melissa Geophysical Research, v. 96, no. B1, p. 475–484. Baptista, A.R., Mangold, N., Ansan, V., Baratoux, D., Masson, P., Lognonne, Rice, Shawn Wright. Guests: Bruce Houghton, Jim Bell III. P., Williams, D., Bleacher, J.E., and Neukum, G., 2008, A swarm of “The workshop gave me the opportunity to test work I do small shield volcanoes on Syria Planum, Mars: Journal of Geophysical everyday on a distant body, using radar data to map geologic Research, v. 113, E09010, doi:10.1029/2007JE002945. Baratoux, D., Pinet, P., Toplis, M.J., Mangold, N., Greeley, R., and Baptista, units, by premapping an area and verifying those interpreta- A.R., 2009, Shape, rheology and emplacement times of small Martian tions in the fi eld.” —Debra Hurwitz, Brown University shield volcanoes: Journal of Volcanology and Geothermal Research, “You didn’t tell us there might be leaves. And grass!” v. 185, p. 47–68, doi:10.1016/j.jvolgeores.2009.05.003. Barnard, W.M., 1990, Mauna Loa—A source book: Historical Eruptions and —Seth Kadish, Brown University Exploration, Volume 1, From 1778–1907: Fredonia, New York, privately 2010. Andrew Beck, Dan Berman, Christopher Edwards, published by W.M. Barnard, xv + 353 p. 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Bleacher, J.E., Glaze, L.S., Greeley, R., Hauber, E., Baloga, S.M., Sakimoto, S.E.H., Williams, D.A., and Glotch, T.D., 2009, Spatial alignment analyses “The workshop really got us to think about processes, for a fi eld of small volcanic vents south of Pavonis Mons and implications and not only about the objects once they are dead.” —Sylvain for the Tharsis Province, Mars: Journal of Volcanology and Geothermal Piqueux, University of California, Irvine Research, v. 185, p. 96–102, doi:10.1016/j.jvolgeores.2009.04.008. Blevins, J.Y.K., 1981, Subsidence Mechanics of Kilauean Pit Craters [M.S. thesis]: “I’m planning on collaborating with someone I’ve met at Honolulu, University of Hawaii, 108 p. this workshop who is working on Apollinaris Patera as well.” Brigham, W.T., 1909, The volcanoes of Kilauea and Mauna Loa: Memoirs of —Alexandra Farrell, Mercyhurst College the Bernice Pauahi Bishop Museum of Polynesian Ethnology and Natural History, v. 2, no. 4, 222 p. Bruno, B.C., Taylor, G.J., Rowland, S.K., and Baloga, S.M., 1994, Quantifying ACKNOWLEDGMENTS the effect of rheology on lava-fl ow margins using fractal geometry: Bul- letin of Volcanology, v. 56, p. 193–206, doi:10.1007/BF00279604. Byrnes, J.M., and Crown, D.A., 2001, Relationships between pahoehoe Our fi rst workshop (and thus all of them) benefi ted from the surface units, topography, and lava tubes at Mauna Ulu, Kilauea vol- foresight of Planetary Geology and Geophysics (PG&G) cano, Hawaii: Journal of Geophysical Research, v. 106, p. 2139–2151, program managers Steve Baloga and, subsequently, Trish doi:10.1029/2000JB900369. Byrnes, J.M., and Crown, D.A., 2002, Morphology, stratigraphy, and surface Rogers. We thank them both for this vision. Most regrettably, roughness properties of Venusian lava fl ow fi elds: Journal of Geophysical Trish is no longer with us, so we would like to dedicate our Research, v. 107, no. E10, 5079, doi:10.1029/2001JE001828. efforts to her memory. Our thanks also go to Harold Garbeil, Byrnes, J.M., Ramsey, M.S., and Crown, D.A., 2004, Surface unit characteriza- tion of the Mauna Ulu fl ow fi eld, Kilauea volcano, Hawai‘i, using integrated who processed almost every planetary and terrestrial image fi eld and remote sensing analyses: Journal of Volcanology and Geothermal we’ve used, and to Ronnie Torres and Mary Mackay, who Research, v. 135, p. 169–193, doi:10.1016/j.jvolgeores.2003.12.016. helped run workshops two through seven. Gordon, Joann, and Campbell, B., and Rogers, P., 1994, Bell Regio, Venus: Integration of remote sensing data and terrestrial analogs for geologic analysis: Ki‘i Morse from “My Island” Bed and Breakfast in Volcano Journal of Geophysical Research, v. 99, no. E10, p. 21,153–21,171, Village played an important role as hosts for the fi rst eight doi:10.1029/94JE01862. workshops; their hospitality and great cooking helped fos- Campbell, B.A., and Shepard, M.K., 1996, Lava fl ow surface roughness and depolarized radar scattering: Journal of Geophysical Research, v. 101, ter a strong feeling of camaraderie among all the workshop p. 18,941–18,951, doi:10.1029/95JE01804. participants. Pineapple Park hostel and especially Marshall, Campbell, B.A., Arvidson, R.E., and Shepard, M.K., 1993, Radar polariza- Virgie, and Maggie Freitas fi lled the Morses’ big shoes very tion properties of volcanic and playa surfaces: Applications to terrestrial remote sensing and Venus data interpretation: Journal of Geophysical well for the ninth and tenth workshops. Guest volcanologists Research, v. 98, p. 17,099–17,113, doi:10.1029/93JE01541. Bruce Campbell, Vince Realmuto, Jim Garvin, Steve Baloga, Carr, M.H., 1974, The role of lava erosion in the formation of lunar rilles and Mar- and Bruce Houghton, and guest Martian Jim Bell III provided tian channels: Icarus, v. 22, p. 1–23, doi:10.1016/0019-1035(74)90162-6. Carr, M.H., and Greeley, R., 1980, Volcanic Features of Hawaii: A Basis for valuable insight and knowledge. Finally, we would like to Comparison with Mars: National Aeronautics and Space Administration thank all the participants (see Appendix 2), who have made (NASA) Special Publication SP-403, 211 p. every workshop a memorable, enjoyable experience! Mahalo Carter, L.M., Campbell, D.B., and Campbell, B.A., 2006, Volcanic deposits in shield fi elds and highland regions on Venus: Surface properties from to D. Crown and J. Bleacher for helpful reviews of this paper. radar polarimetry: Journal of Geophysical Research, v. 111, E06005, These workshops were sponsored by grants NAG5-4127, doi:10.1029/2005JE002519. 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