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SEARCH FOR METEORITES AT MARTIN HILLS AND PIRRIT HILLS, ANTARCTICA. P. Lee1, W. A. Cassidy2, D. Apostolopoulos3, D. Bassi4, L. Bravo5, H. Cifuentes5, M. Deans3, A. Foessel3, S. Moorehead3, M. Parris3, C. Puebla5, L. Pedersen3, M. Sibenac3, F. Valdés6, N. Vandapel7, and W. L. Whittaker3. 1NASA Ames Research Center, MS 245-3, Moffett Field, CA 94035-1000, USA, 2Dept. of Geology and Planetary Science, Univ. of Pittsburgh, Pittsburgh, PA 15260, USA, 3The Robotics Institute, Carnegie Mellon Univ., Pittsburgh, PA 15213, USA, 4Universidad de Santiago, Santiago, Chile, 5Fuerza Aerea de Chile, Chile, 6Empresa Nacional Aeronaútica (ENAER), Chile, 7Laboratoire d’Analyses et d’Architectures des Systèmes, France.
Introduction: Between 4 and 8 Nov.,
1998, a foot search for meteorites was conducted at Martin Hills (82°00’S,
88°00'W) and Pirrit Hills (81°09’S, 85°05’W), Antarctica. This
search was made in the context of a test site survey for the NASA-funded
Robotic Antarctic Meteorite Search (RAMS) Program of the Robotics Institute
of Carnegie Mellon University, Pittsburgh, PA, USA. The goal of the RAMS
Program is to develop a robotic vehicle capable of searching for meteorites
in Antarctica autonomously. The Martin Hills and Pirrit Hills areas were
chosen mainly because of their proximity to Patriot Hills (80°20'S,
81°20'W), a site where logistical support is readily available and
where the 1998-1999 field season tests of the Nomad rover, the present
robotic testbed, would be conducted. No meteorites are found at Patriot
Hills, possibly because of the site’s low altitude (800 - 1000 m) which
results in relatively warm summer peak temperatures and hence significant
surficial ice melting . Both Martin Hills and Pirrit Hills are at higher
elevations, ~1700 m and ~1400 m respectively, and are associated with blue
ice fields, as evident in aerial photographs. We report here on our search
for meteorites at Martin Hills and Pirrit Hills, the first meteorite searches
conducted at these sites.
|Flying to Pirrit Hills|
Martin Hills: On 4 Nov., 1998, a 7-person
search was conducted on foot at Martin Hills during a brief 2-hour stop
at the site’s northern blue ice field. Both the eastern and western strips
of this ice field were walked. The total distance traversed was approximately
10 person-kilometers, covering an estimated 1% of the total blue ice area
available (Fig. 1). One meteorite was found, on blue ice near the western
end of the eastern ice strip, at 82°03.1’S, 87°59.5’W. The meteorite,
~ 3.5 x 1.5 x 1.5 cm in size and 70% fusion-crusted, was assessed upon
collection as probably an ordinary chondrite. Numerous terrestrial rock
debris fragments in a variety of sizes were also present on the ice, mostly
fragments of dark basalt evidently derived from the Martin Hills. A few
regelation portholes (windows of clear refrozen ice through which sunken
rocks or finer sediments can be seen) were noted on the ice, but not nearly
as abundantly as at Patriot Hills .
|The chondrite meteorite found at Martin Hills|
|A regelation porthole|
Pirrit Hills: Between 4 and 8 Nov., 1998, several foot searches by groups of 2 to 5 persons were conducted across the eastern blue ice fields of the Pirrit Hills. Blue ice areas within a radial distance of ~3 km from a temporary campsite established at 81°08.9’S, 85°05.4’W were searched. Traverses reached as far south as 81°09.9’S, 85°23.0’W, 5.3 km from camp, and as far west as 81°08.2’S, 85°21.1’W, 4.7 km from camp. The total distance walked was approximately 60 person-kilometers (Fig. 2). No meteorite was found. Numerous terrestrial rock debris fragments in a variety of sizes are present on the ice, mostly leucocratic fragments of granitic rocks, but also dark fragments of biotite, hornblende and magnetite. A typical surface density of macroscopic debris encountered on bare blue ice is 25 m-2, while snow cover on the blue ice fields was about 50%. Many regelation portholes were noted, in lesser abundance than at Patriot Hills and perhaps more commonly than at Martin Hills . Many rocks or sediments seen in the regelation portholes at Pirrit Hills are of relatively low visual albedo (e.g., granodiorites).
Discussion and Conclusions: One meteorite was found at Martin Hills, none at Pirrit Hills. Signs of ice melting at both sites, mostly in the form of regelation portholes, are fewer than at Patriot Hills but are nevertheless present. Two explanations for the general dearth of meteorites at Martin Hills and at Pirrit Hills are possible: (a) The ice may experience significant melting due to summer peak temperatures above freezing, especially around rocks of low albedo. A meteorite about to emerge from the ice would tend to remain below the ice surface by radiatively melting its surroundings, or if somehow exposed at the surface, would likely experience rapid weathering; (b) The history and sources of ice in the Martin Hills and Pirrit Hills areas are unknown and might have been inadequate for concentrating meteorites. The blue ice fields traversed might have been exposed as potential meteorite stranding surfaces only recently, or the upstream gathering areas might not be extensive. Although clearly not a stranding site of high yield, the Martin Hills blue ice field may warrant further meteorite search efforts. The Pirrit Hills site appears less promising. The eastern blue ice fields at this site are not productive search areas for meteorites. The slight difference in elevation between Martin Hills and Pirrit Hills, ~1700 m vs ~ 1400 m, might be part of the reason why the former site has yielded a meteorite while the latter has not. Our results support the general observation that only those blue ice fields experiencing very little surficial melting may be productive meteorite stranding surfaces . Combined with our meteorite search experience in the Patriot Hills area , a threshold altitude in the Ellsworth Land region of Antarctica below which meteorite searches are likely to be unproductive appears to be ~1500 m. We do not recommend robotic meteorite searches at either Martin Hills or Pirrit Hills.
References:  Lee, P. et al. (1998). Meteorit. & Planet. Sci. 53, …-….  Lee, P. et al. (1998). J. Glaciol., in prep.  Cassidy, W. A. (1991). In The Geology of Antarctica, Oxford Univ. Press, 652-666.
Acknowledgements: We are grateful to
the National Aeronautics and Space Administration (NASA), the Fuerza Aerea
de Chile (FACH), the Instituto Antartico Chileno (INACH), and the Institut
pour la Recherche et la Technologie Polaires (IFRTP) for their support.
We also thank Ralph P. Harvey of Case Western Reserve University and John
W. Schutt for useful discussions.