De Gerlache Research Articles

Tectonics and Seismicity of the Lunar South Polar Region

The lunar south pole regions are subjected to global stresses that result in contractional deformation and associated seismicity. This deformation is mainly expressed by lobate thrust fault scarps; examples are globally distributed, including polar regions. One small cluster of lobate scarps falls within the de Gerlache Rim 2 Artemis III candidate landing region. The formation of the largest de Gerlache scarp, less than 60 km from the pole, may have been the source of one of the strongest shallow moonquakes recorded by the Apollo Passive Seismic Network. The scarp is within a probabilistic space of relocated epicenters for this event determined in a previous study. Modeling suggests that a shallow moonquake with an M w of ∼5.3 may have formed the lobate thrust fault scarp. We modeled the peak ground acceleration generated by such an event and found that strong to moderate ground shaking is predicted at a distance from the source of at least ∼40 km, while moderate to light shaking may extend beyond ∼50 km. Models of the slope stability in the south polar region predict that most of the steep slopes in Shackleton crater are susceptible to regolith landslides. Light seismic shaking may be all that is necessary to trigger regolith landslides, particularly if the regolith has low cohesion (on the order of ∼0.1 kPa). The potential of strong seismic events from active thrust faults should be considered when preparing and locating permanent outposts and pose a possible hazard to future robotic and human exploration of the south polar region.

Character and spatial distribution of mineralogy at the lunar south polar region

The lunar south polar region, encompassing part of the South Pole-Aitken (SPA) basin, stands out as one of the most intriguing areas for future lunar exploration endeavors. Using the Moon Mineralogy Mapper (M3) data, we conducted a comprehensive investigation into the characteristics and distribution of minerals within the lunar south polar region, spanning from 80°S to the south pole. The cartographic outputs from this study, capable of delineating the composition and abundance of various minerals, have enabled the partitioning of the lunar south polar region into two distinct zones. The region situated within the inner ring of the SPA basin is characterized by an elevated abundance of low-Ca pyroxene, whereas the Feldspathic Highlands (FH) in the lunar south polar region and the outer ring of the SPA basin predominantly comprise feldspathic materials, albeit with localized pyroxene-rich areas. The dominant mafic component across the lunar south polar region is low-Ca pyroxene, with no evidence of olivine-rich materials being detected. The mineralogy of some candidate landing sites was illustrated and the hematite-bearing materials were observed at the rim of Shackleton and de Gerlache. Furthermore, we also identified an abundance plagioclase on the western rim of Shackleton. These findings underscore the significance of the lunar south polar region, not only as a promising locale for in situ resource utilization (ISRU) in forthcoming lunar missions but also as a key site for advancing our understanding of the Moon's geological evolution.

Simulation of the temperatures in the permanently shadowed region of the Moon's south pole and data validation

The permanently shadowed regions (PSRs) at the lunar poles without direct solar illumination maintain low temperatures throughout the year, making them optimal environments for the preservation of water ice. This paper investigates the diurnal and seasonal temperature variations of the PSRs within craters at the lunar south pole. The craters de Gerlache, Shoemaker, Amundsen, and Wiechert E are selected to explore how latitudes and shapes impact PSR temperature. Using the ray tracing approach, the shadow effect of terrain on the scattered sunlight and thermal radiation is calculated. PSR temperatures are simulated with the one-dimensional heat conduction equation. The thermal emissivity of the lunar surface is studied. Simulations with anisotropic emissivity are closer to the Diviner data in PSRs than the simulations with isotropic emissivity. In addition, by comparing the simulations to the Diviner data, it is found that the thermal conductivity at the extremely low temperatures in PSRs might be lower than that at high temperatures outside the PSRs. Simulations of the selected craters are used to study the influence of polar day phenomena occurring at high-latitude craters during the summer and the effect of direct solar illumination at the floors of low-latitude craters on the temperature distribution of PSRs. The influence of crater shape is analyzed as well by investigating the temperature distributions within PSRs of flat-floored and bowl-shaped craters. With the analysis of the heat flux propagation distances, emission angles, and incident angles, this study quantitatively elucidates the spatial and temporal variations in PSR temperatures. To explain why the Diviner data are lower than the simulation results at the solar-illuminated crater walls, an undulating rough surface is generated. The locations of the Sun and the observer on opposite sides of the rough surface may decrease the observed infrared brightness temperature according to the simulations. The PSR peak temperatures simulated with the anisotropic emissivity and thermal conductivity for PSRs are used to search for low-temperature areas suitable for preserving water ice within de Gerlache and Shoemaker.

Characterization of the Moon’s South polar craters using optical, microwave and thermal remote sensing

The peculiar illumination and insolation conditions at the poles of the Moon lead to the formation of Permanently Shadowed Regions (PSR) that act as cold traps for volatiles and are important for In Situ Resource Utilization (ISRU). However, since these regions lie in shadows of surrounding topographic highs, the ability of optical remote sensing in imaging these regions for photo reconnaissance is limited and using other modes of remote sensing becomes imperative. In this work, reflectance from optical data, backscatter from active microwave data and temperature from thermal data from the surfaces of three craters – de Gerlache, Haworth and Shoemaker – on the South Pole of the Moon, in close proximity to the Artemis III candidate landing sites, has been studied. Images from Clementine UVVIS, LRO WAC and LRO NAC have been compared with fully polarimetric data from the L-bands sensor of Chandrayaan-2 DFSAR. Further, the temperatures at the surface of the craters have been studied using data from LRO DIVINER. Since large parts of the craters under study lie in permanent shadows, Clementine UVVIS and LRO WAC could image only some parts of the rims. LRO NAC, with its longer exposure times, could image some parts within the crater however the walls of the crater and the floor near the walls remained in shadow. DFSAR was found to be useful in viewing the permanently shadowed regions of the craters. Overall, the backscatter in HH and VV (co-pol) channels was higher than the backscatter in HV and VH (cross-pol) channels. The elevated rims of the craters were clearly visible in co-pol channels and the rough texture of the ejecta of the craters had a distinct high backscatter in cross-pol channels. This fully polarimetric data can be used to map the interiors of the craters where optical data has low albedo. Analysis of the thermal data revealed that within the craters, in the regions that were in perpetual shadows, the maximum summer temperatures were less than 150 K making these regions cold traps for volatiles and possible locations of surface water–ice. The parts of craters lying in the shadows of surrounding higher features had lower maximum temperatures in summer and the parts facing them had higher maximum temperatures due to reflected insolation. Seleno Referenced Image (SRI) product from Chandrayaan-2 DFSAR was found to be a viable alternative to optical data for viewing the PSRs and for their geologic mapping.

An Analysis of the Requirements for a Sustainable Lunar Transportation System to Enable Initial DIANA Infrastructure

The Dedicated Infrastructure and Architecture for Near-Earth Astronautics (DIANA) is a design concept for a self-sustainable lunar village near the de Gerlache crater, on the lunar South Pole, comprising tourists and astronauts alike. The village will be permanently inhabited and will exploit future technologies to achieve independence from a majority of Earth resupply missions. Execution of the initial construction phase of the DIANA infrastructure depends primarily on the persistent supply of in-situ construction material, regolith. Lunar raw materials also primarily contribute to the life support systems (LSS) and the radiation protection for the inhabited modules. To enable ISRU, resources need to be transported using diverse locomotion systems on the unexplored lunar terrain. A self-sustainable lunar base requires to be built on an ecosystem that facilitates continuous transportation of materials, humans (astronauts and tourists) and robotic systems. This paper focuses on a detailed comprehension of the design, feasibility, and economic requirements of a transportation ecosystem concept explicitly dedicated to the establishment and development of the DIANA lunar village. The mission objectives and top level requirements pertaining to the individual transportation systems will be derived from the detected necessities that are defined for alternative transportation technologies that efficiently provide large amounts of lunar raw material for the construction of lunar infrastructure as well as water ice from the de Gerlache Crater, which shall primarily contribute to the LSS and the production of rocket fuel. While transporting humans, factors such as time, comfort, and risk mitigation play a major role, and are therefore, discussed thoroughly within the framework of this study. Using this study as the principal foundation, a phase 0/A design study illustrating a novel transportation infrastructure concept based on magnetic levitation technology would be developed for efficient transportation of resources and people across the lunar surface. This transportation concept shall be sustainably manufactured using the abundant lunar resources to minimize costs and resupply missions in the long term to pave the way for an independent lunar village.

Selection of Lunar South Pole Landing Site Based on Constructing and Analyzing Fuzzy Cognitive Maps

The Permanently Shadowed Regions (PSRs) of the lunar south pole have never been directly sampled. To explore and discover lunar resources, the Chinese lunar south pole exploration mission is scheduled to land in direct sunlight near the PSR, where sampling and analysis will be carried out. The selection of sites for lunar landing sampling sites is one of the key steps of the mission. The main factors affecting the site selection are the distribution of PSRs, lunar surface slopes, rock distribution, light intensity, and maximum temperature. In this paper, the main factors affecting site selection are analyzed based on lunar multi-source remote sensing data. Combined with previous engineering constraints, we then propose a comprehensive multi-factor fuzzy cognition and selection model for the lunar south site selection. An analytical model based on a fuzzy cognitive map algorithm is also established. Furthermore, to make a preliminary landing area selection, we determine the evaluation index for the candidate landing areas using fuzzy reasoning. Using the proposed model and combined scoring index, we also verify and analyze the prominent impact craters at the lunar south pole. The scores of de Gerlache (88.48°S 88.34°W), Shackleton (89.67°S 129.78°E), and Amundsen (84.5°S, 82.8°E) craters are determined using fuzzy interference as 0.816, 0.814, and 0.784, respectively. Moreover, using our proposed approach, we identify feasible landing sites around the de Gerlache crater close to the PSR to facilitate discovery of water ice exposures in future missions. The proposed method is capable of evaluating alternative landing zones subject to multiple engineering constraints on the Moon or Mars based on the existing data.

Characteristics of de Gerlache crater, site of girlands and slope exposed ice in a lunar polar depression

The 31 km diameter and 7.5 km deep de Gerlache crater, located 30 km from the southern pole of the Moon was surveyed. At its bottom a 15 km diameter younger crater can be also found beside many smaller overprinting craters. At moderately sloping terrains a few m high, 100–200 m wide, curving quasi-parallel, km long set of ridges could be identified, which seem to be widespread on the surface, and might cover the half or even more of the crater. We named these “girland like features” in this work, which seem to be produced by mass movements on slopes (however differ from most of the already identified slope features, which show downslope elongated lineaments or fallen/redeposited debris on the Moon). At all locations they are superposed by recently formed 10–50 m diameter craters, thus might be older than the equilibrium crater population shown age of about 100 Ma old. This is the first identification of these features at the polar terrains, where they might contribute both in the shielding or exposing of subsurface ice. In de Gerlache crater ice occurrences have previously been located on moderately steep slopes, indicating they might be exposed by mass movement processes, where active movements might have happened in the last some 10 Ma using crater statistics based age of the shallow regolith layer. Only half of them were located at areas with modelled surface temperatures below 110 K, where temperature might be not enough to keep most of the deposited H2O there on Ga time scale. However the real values are probably more diverse because of the limited spatial resolution of available temperature data. Target areas are indicated for possible future missions, where periodic solar illumination, and subsurface ice at 0.5 m depth could be also present.

Resource potential of lunar permanently shadowed regions

The lunar polar regions contain permanently shadowed regions (PSRs) or local topographic depressions that never receive direct sunlight. These environments (<110 K) have the potential to cold-trap volatile materials in the form of ice, which are essential resources for exploration and industrialization of cislunar space and the Solar System. Orbital observations and those from the LCROSS impactor experiment provide evidence of the existence of water ice and other cold-trapped volatiles in PSRs; however, constraints on volatile abundance and distribution remain ambiguous as individual observations are not always in concord. Here we compile observations indicating the presence of volatiles from ten remotely sensed datasets in 65 PSRs to estimate the locations and mass of water ice deposits. Faustini, Cabeus, de Gerlache, Shoemaker, Haworth, Sverdrup, Slater, and Amundsen are likely the most resource-rich PSRs. Based on co-locations of observations indicative of surface frost and subsurface hydrogen abundance, we find that the craters with the highest potential mass in metric tons (t) of water ice include Cabeus (~11 × 106 t), Shoemaker (~5 × 106 t), Faustini (~4 × 106 t), de Gerlache (~3 × 106 t), and Haworth (~3 × 106 t). Future prospecting of lunar volatiles and water ice is contingent on filling knowledge gaps in resource potential, notably accurate measurements of grade and depth of volatiles. Our proposed ranking and estimates for resource tonnage are a tool to guide future orbital and landed missions that could accurately determine the resource potential of PSR deposits.

Selection of a Landing Site in the Permanently Shadowed Portion of Lunar Polar Regions Using DEM and Mini-RF Data

Direct sampling has never been performed in the permanently shadowed regions (PSRs) of lunar poles up to now. In the Chinese Chang’e-7 (CE-7) mission, a mini-flyer will fly from the lander in a solar illuminated region at the lunar south polar region to the nearby PSRs to collect samples for analysis. In this letter, four potential craters of the lunar south pole, including Shackleton, Shoemaker, de Gerlache, and Slater are discussed for this proposal. Design principles of the landing site, sampling site, and flight route are presented. The local surface slopes are calculated using a digital elevation model (DEM) to select a flat area as a potential landing site, which should allow ample time for solar illumination to support the rover from the lander and allow the flyer to reach the neighboring PSRs. Mini-RF data are applied for further validation of the flat landing and sampling sites, particularly for some rocky rough surfaces that are not identified in DEM and optical images of PSRs. The craters de Gerlache and Slater are found to be suitable for further analysis when high-resolution synthetic aperture radar (SAR) data are acquired by the new polarimetric SAR carried by CE-7.

Carbon Dioxide Cold Traps on the Moon

AbstractWater ice is expected to be trapped in permanently cold regions near the lunar poles. Other ices (“super‐volatiles”) are trapped at lower temperatures, close to the lowest temperatures measured within the lunar permanently shadowed regions (PSRs). Here, the thermal stability of solid carbon dioxide in the south polar region is determined by analysis of 11 years of temperature measurements by Diviner, a radiometer onboard the Lunar Reconnaissance Orbiter. Sublimation rates averaged over a draconic year are far lower than peak sublimation rates. Small spatially contiguous pockets of CO2 ice stability are found in the craters Amundsen, Haworth, de Gerlache, and others, over a cumulative area of roughly 200 km2. The LCROSS probe impacted one of those pockets and released CO2, serving as validation of the thermal stability calculations. Future surface missions can utilize this highly localized resource for the production of fuel, steel, and biological materials.

The Black Sea in Romanian Oceanographic Research

Romania, as a maritime state, after being separated from the Black Sea coast for 400 years, until the War of Independence in 1877, has a tradition in the marine sciences for over 100 years. The illustrious ancestors of Romanian oceanography, especially biological oceanography, are Emil Racoviță, Grigore Antipa and Ioan Borcea. From an oceanographic point of view, E. Racovitza distinguished himself as a biologist of the famous Antarctic multinational expedition, under the command of Captain Adrien de Gerlache, from Belgium, aboard the vessel Belgica, between 1997 and 1998. G. Antipa is the founder of the Bio-Oceanographic Institute in Constanța (1932) and of the Biological Research Station in Caliacra (currently in Bugaria) and in this context he held the positions of organizer, general administrator and director general of the State Fisheries, as the second national delegate of Romania at the International Commission for the Scientific Exploration of the Mediterranean Sea (CIESM), and as rapporteur for the Black Sea, Marmara and the Eastern Mediterranean, as well as organizer of the first Congress and General Assembly of CIESM in Romania in Bucharest in 1935. I. Borcea's main scientific achievement is the creation of the Marine Zoological Station in Agigea, in 1926, which bears his name to this day, with the maintenance of close collaborative relations in the field of marine biology, especially with France and Italy. The main marine research institutions, namely the Marine Zoological Station “Professor Ioan Borcea”, the Bio-Oceanographic Institute, which later became the Fisheries Research Station “Dr. Grigore Antipa”, the Marine Biology Sector from Constanța of the “Traian Săvulescu” Institute of Biology from Bucharest, the Oceanographic Research Station from Constanța and Sulina and the Marine Sedimentology Laboratory, affiliated to the Geological Institute of Romania, merged into the Romanian Marine Research Institute (RMRI) from Constanța on March 1, 1970. The succesor of RMRI since 1990 is the National Institute for Marine Research and Development “Grigore Antipa”, in the same headquarters (Bd. Mamaia No. 300, RO-900581 Constanța). A definite confirmation of the value of the results of the Romanian marine research, over time, is, among others, the close professional relationships with CIESM, continued to the present. Thus, Romania has further promoted and supports marine research at national, regional and international level.

The Solar Hot Water Supply System for an Inhabited Base Located at the Moon Poles

The use of the environmentally friendly solar thermal energy runs into some problems during practical realization of the power systems due to the difficulties of accumulating and storing the produced thermal energy during the lunar night. The paper deals with a solar hot water supply system for a life support system of the lunar bases located at the peaks of eternal light of the North and South Poles of the Moon and able to maintain hot water temperature during a lunar year taking into account the solar eclipses at the Moon. Solar hot water supply system includes a solar collector in the form of an annular cylinder with an axis perpendicular to the surface of the Moon with hydrogen coolant and seasonal storage heater located in lunar soil filled with crushed regolith to maintain hot water temperature during the periods without sun illumination. Design parameters as well as the system efficiency have been evaluated on the basis of the developed mathematical model and computer simulation of dynamic conditions for the system located at the ridge of Peary crater at the North Pole and the ridges of Shackleton and De Gerlache craters and Malapert Mountain at the South Pole of the Moon. It is shown that for the North Pole the water temperature at the lunar base reaches the required level at the end of the first lunation and practically does not change during the solar eclipse due to the presence of heat in the solar system. When the solar system is located in any peak of eternal light at the South Pole, the time it takes for the system to reach the required thermal regime does not exceed 4 lunations, while the required level of hot water is provided throughout the year. It is noted that due to the presence of dark intervals in the southern peaks of eternal light, significantly larger areas of the mid-solar collector and twice the size of the heat accumulator are required compared to the North Pole.

The Strike‐Slip West Wishbone Ridge and the Eastern Margin of the Hikurangi Plateau

AbstractThe West Wishbone Ridge (WWR), east of New Zealand, has previously been interpreted as a Cretaceous plate boundary, although both the nature and timing of motion along this feature have been disputed. Here, using recently acquired seismic reflection data from the region of the intersection of the WWR with the Chatham Rise, we show that the WWR was primarily a dextral strike‐slip fault during the Late Cretaceous. The WWR first propagated along the eastern margin of the Hikurangi Plateau after the collision of the Hikurangi Plateau with the Chatham Rise, in response to the slowing of spreading at the Osbourn Trough while spreading continued unabated east of the East Wishbone Ridge, from ca. 105 Ma. Reorientation of spreading at the Osbourn Trough at this time resulted in short‐lived, oblique subduction beneath the southern extent of the WWR. Motion along the WWR likely ceased with the cessation of Osbourn Trough spreading. Using our seismic reflection data and gravity modeling across those same profiles, we locate, for the first time, the eastern boundary of the Hikurangi Plateau between 42–43°S. We also find anomalously thick oceanic crust (∼12 km thick) north of the Hikurangi Plateau. Matching tectonic fabric and fracture zone links between the East Wishbone Ridge and the De Gerlache Gravity Anomaly near Ellsworth Land on the West Antarctic margin indicates that these features were linked or parallel during the Late Cretaceous, and fed strike‐slip motion southward into the Gondwana interior, contributing to the onset of Gondwana rifting ca. 85 Ma.

On the long-ignored scientific achievements of the Belgica expedition 1897–1899

ABSTRACTThe Belgica expedition, which left Belgium in August 1897, was the first to spend 13 months continuously in Antarctic waters, before returning in late 1899. This was not only an exploratory venture, as new lands and oceans were charted, but more importantly it was an exceptional and successful scientific voyage. After the return of the expedition, a vast array of scientific data was processed and eventually 92 publications in some nine volumes funded by the Belgica Commission appeared over 40 years as a series called Resultats du voyage de la Belgica en 1897–99 sous le commandement de A. de Gerlache de Gomery – rapports scientifiques. Disappointingly, those significant results have been mostly ignored in the scientific literature and the paper here aims to inform scientists of the achievements of the Belgica expedition and where to obtain the information. Many of the climatological and oceanographic data obtained by the expeditioners ought to be examined in line with the changes that are occurring...

Illumination conditions at the lunar poles: Implications for future exploration

We produced 400 × 400 km Digital Terrain Models (DTMs) of the lunar poles from Lunar Orbiter Laser Altimeter (LOLA) ranging measurements. To achieve consistent, high-resolution DTMs of 20 m/pixel the individual ranging profiles were adjusted to remove small track-to-track offsets. We used these LOLA-DTMs to simulate illumination conditions at surface level for 50 × 50 km regions centered on the poles. Illumination was derived in one-hour increments from 01 January, 2017 to 01 January, 2037 to cover the lunar precessional cycle of 18.6 years and to determine illumination conditions over several future mission cycles. We identified three regions receiving high levels of illumination at each pole, e.g. the equator-facing crater rims of Hinshelwood, Peary and Whipple for the north pole and the rim of Shackleton crater, and two locations on a ridge between Shackleton and de Gerlache crater for the south pole. Their average illumination levels range from 69.5% to 82.9%, with the highest illumination levels found at the north pole on the rim of Whipple crater. A more detailed study was carried out for these sites as targets for a lander and/or rover equipped with solar arrays. For this purpose we assumed a lander with a structural height of two meters above the ground (height of the solar panels). Here average illumination levels range from 77.1% to 88.0%, with the maximum found at the ridge between Shackleton and de Gerlache crater on the south pole. Distances, sizes and slopes of nearby Permanently Shadowed Regions (PSRs) as a prime science target were also assessed in this case.

Illumination conditions at the lunar south pole using high resolution Digital Terrain Models from LOLA

The illumination conditions of the lunar south pole are investigated using a geometrically adjusted, 20m/pixel Digital Terrain Model (DTM) from laser tracks of the Lunar Orbiter Laser Altimeter (LOLA). Several comparisons with Narrow Angle Camera (NAC) images have been made to cross-validate the results. Illumination conditions were first evaluated over a region of 20×20km over a one-year period (October 22, 2018 – October 22, 2019) at surface level and 2m above ground. Three potential landing sites are investigated in more detail. A 19-year study covering the lunar precessional cycle was carried out at surface level, 2 and 10m above ground for a site found at “Connecting Ridge”, the ridge connecting the Shackleton and de Gerlache crater. This area was found to be an ideal site for future landing missions with respect to illumination conditions. We identified locations receiving sunlight for 92.27% of the time at 2m above ground and 95.65% of the time at 10m above ground. At these locations the longest continuous periods in darkness are typically only 3–5days.

Seamounts off the West Antarctic margin: A case for non-hotspot driven intraplate volcanism

New radiometric age and geochemical data of volcanic rocks from the guyot-type Marie Byrd Seamounts (MBS) and the De Gerlache Seamounts and Peter I Island (Amundsen Sea) are presented. 40Ar/39Ar ages of the shield phase of three MBS are Early Cenozoic (65 to 56Ma) and indicate formation well after creation of the Pacific–Antarctic Ridge. A Pliocene age (3.0Ma) documents a younger phase of volcanism at one MBS and a Pleistocene age (1.8Ma) for the submarine base of Peter I Island. Together with published data, the new age data imply that Cenozoic intraplate magmatism occurred at distinct time intervals in spatially confined areas of the Amundsen Sea, excluding an origin through a fixed mantle plume. Peter I Island appears strongly influenced by an EMII type mantle component that may reflect shallow mantle recycling of a continental raft during the final breakup of Gondwana. By contrast the Sr–Nd–Pb–Hf isotopic compositions of the MBS display a strong affinity to a HIMU-type mantle source. On a regional scale the isotopic signatures overlap with those from volcanics related to the West Antarctic Rift System, and Cretaceous intraplate volcanics in and off New Zealand. We propose reactivation of the HIMU material, initially accreted to the base of continental lithosphere during the pre-rifting stage of Marie Byrd Land/Zealandia to explain intraplate volcanism in the Amundsen Sea in the absence of a long-lived hotspot. We propose continental insulation flow as the most plausible mechanism to transfer the sub-continental accreted plume material into the shallow oceanic mantle. Crustal extension at the southern boundary of the Bellingshausen Plate from about 74 to 62Ma may have triggered adiabatic rise of the HIMU material from the base of Marie Byrd Land to form the MBS. The De Gerlache Seamounts are most likely related to a preserved zone of lithospheric weakness underneath the De Gerlache Gravity Anomaly.

Romanian Marine Centennial

This article explores an Antarctic expedition that led to the development of marine sciences in Romania, celebrating their one hundredth anniversary, and the creation of marine stations. Emil Racovitza participated in the Belgica Antarctic Expedition of de Gerlache which seems to have nurtured his interest in the marine sciences. He is credited with launching oceanography in Romania. Other major figures in the development of oceanography and the creation of marine research facilities are Borcea and Antipa, whose careers are retraced in the paper. Recently all research points have been regrouped to form the National Institute for Research and Development. La Roumanie fête le centenaire de son océanographie et l'INRDM (Institut National pour la Recherche et le Dévelopment Marins “Grigore Antipa”) célèbre les 40 années de sa création; de fait il s'agit d'un organisme issu de la coalescence de plusieurs stations océanographiques qui ont jalonné le développement de l'océanographie en Roumanie. Plusieurs noms de personalités proéminentes sont citées dans ce bref aperçu. Racovitza, qui se fit un renom en tant que membre du complément scientifique de l'expédition de la Belgica en Antarctique, y trouva probablement sa vocation marine. Les festivités de l'anniversaire, qui ont un cachet international, se centreront sur un symposium. Istoricul oceanologiei româneşti poate fi rezumat prin evocarea personalităţilor lui E. Racoviţa, G. Antipa, I. Borcea şi a instituţionalizării cercetării marine în staţiunile şi laboratoarele care au general Institutul Român de Cercetări Marine/Institutul Naţional de Cercetare-Dezvoltare Marină “Grigore Antipa” şi Institutul Naţional de Cercetare-Dezvoltare pentru Geologie şi Geoecologie Marină “GeoEcoMar.” Die Geschichte der rumänischen Meereswissenschaften kann zusammen-gefasst werden durch die Berufung der Persönlichkeiten von Emil Racovitza, Grigore Antipa und Ioan Borcea sowie die Institutionalisierung der Meeresforschung in Forschungseinrichtungen, die zur Gründung des Rumänischen Meeresforschungs-institut/Nationalinstitut für Meeresforschung und Entwicklung “Grigore Antipa” und des Nationalinsitut für Forschung und Entwicklung der Meeresgeologie und Ökologie (GeoEcoMar) geführt haben.

Belgica's Antarctic Toponymic Legacy

Abstract It might be argued that this paper does not sensu stricto contribute to “polar science.” It, however, rekindles aspects of its history and of that of both oceanography and cartography. Obviously the interest for the polar regions was keen in the 19th century and elicited financial support. The paper may lift anew the veil that has somewhat dimmed the light that should shine on polar science achievements of Belgian explorers and scientists. Knowledge of the names of geographic features in the Antarctic is probably less widespread, and yet, there are many Belgian names on and near the southernmost continent. Most names were given by the head of the first-ever Antarctic expedition to spend a winter on the southernmost continent. Belgian Royal Navy Lieutenant Adrien de Gerlache de Gomery's expedition in the Antarctic brought back a wealth of scientific information. His trip ended precisely 111 years ago, and has been—literally—carved in stone as the Belgica is indeed one of the 20 oceanographic vesse...

Philatelic Panorama of Some Belgian Antarctic Marine Contributions, 19th–21st Centuries: FromBelgicatoPrincess Elisabeth

Abstract Belgium has been interested in and involved in Antarctic studies for over a century. The name of Adrien de Gerlache is indelibly linked with that of his ship, the Belgica, the first vessel to ever spend a winter trapped in the ice of the southern continent. The former Norwegian sealer-whaler had a multinational crew of scientists and sailors. If it brought back a trove of information, it also did a tale of hardships and fears. The postal administration of Belgium—and to a more modest extent that of Romania and Poland—have illustrated the expedition, its anniversaries, and the further research carried out by Belgians in Antarctica. The Belgica was sunk by the German invasion forces in World War II. Efforts are underway to refloat the vessel and make it into a museum, as was done, e.g., for the Fram.