Europlanet Science Congress 2020
Virtual meeting
21 September – 9 October 2020
Europlanet Science Congress 2020
Virtual meeting
21 September – 9 October 2020

Oral presentations and abstracts

TP12

The EPSC symposium "Open Lunar Science & Innovation” will address:
- Celebrating the legacy of Apollo and Luna programmes after 50 years
- Recent lunar results: geochemistry, geophysics in the context of open planetary science and exploration
- Synthesis of results from Clementine, Prospector, SMART-1, Kaguya, Chang’e 1, 2 and 3, Chandrayaan-1, LCROSS, LADEE, Lunar Reconnaissance Orbiter, Artemis and GRAIL
- First results from Chang'E 4, Chandrayaan2,
- Goals and Status of missions under preparation: orbiters, Luna25-27, SLIM, , Commercial landers, Chang'E 5 and Lunar sample return missions, Future cargo landers,
- Precursor missions, instruments and investigations for landers, rovers, sample return, and human cis-lunar activities and human lunar surface sorties (Artemis and others)
- Preparation for International Lunar Decade: databases, instruments, missions, terrestrial field campaigns, support studies
- ILEWG and Global Exploration roadmaps towards a global robotic/human Moon village
- Strategic Knowledge Gaps, and key science Goals relevant to Lunar Global Exploration
- The Moon Village with the goal of a sustainable human and robotic presence on the lunar surface as an ensemble where multiple users can carry out multiple activities.
- The Moon for planetary science, life sciences, astronomy, fundamental research, resources utilisation, human spaceflight, peaceful cooperation, economical development, inspiration, training and capacity building.
- How a laboratory on the Moon should be equipped to be useful for a variety of disciplines, including geology, biology, and chemistry
- How can the Moon Village serve as a stepping stone for exploration of Mars and planetary bodies even further away?
- Historical, societal, humanistic aspects of lunar exploration

Lunar science and exploration are developing further with new and exciting missions being developed by China, the US, Japan, India, Russia, Korea and Europe, and with new stakeholders.

Co-organized by MITM
Convener: Bernard Foing | Co-convener: Joana S. Oliveira

Session assets

Session summary

Chairperson: Bernard Foing, Joana Oliveira
EPSC2020-210
Erik Kuulkers and Anniek Gloudemans

The Apollo 15 & 16 missions were the first to explore the Lunar surface chemistry by investigating about 10 percent of the Lunar surface using a remote sensing X-ray fluorescence spectrometer experiment. The data obtained has been extensively used to study Lunar formation history and geological evolution. In this work a re-evaluation of the Apollo 15 & 16 X-ray fluorescence experiment is conducted with the aim to obtain up-to-date empirical values for aluminum (Al) and magnesium (Mg) concentrations relative to silicon (Si) of the upper Lunar surface. An up-to-date orbit reconstruction, updated instrument response, and improved intensity ratio calculations are used to obtain new intensity ratio maps.

How to cite: Kuulkers, E. and Gloudemans, A.: Re-evaluation of Lunar X-ray observations by Apollo 15 & 16, Europlanet Science Congress 2020, online, 21 Sep–9 Oct 2020, EPSC2020-210, https://doi.org/10.5194/epsc2020-210, 2020.

EPSC2020-271
Alessandro Maturilli, Joern Helbert, Harald Hiesinger, Giulia Alemanno, Sabrina Schwinger, and Mario D'Amore

The Mercury Radiometer and Thermal Infrared Spectrometer (MERTIS) is part of the ESA BepiColombo Mercury Planetary Orbiter (MPO) payload and consists of a push-broom IR-spectrometer (-TIS) and a radiometer (-TIR) [1].

During the long cruise to Mercury, and before its arrival on December 5th 2025, BepiColombo will perform 9 flybys: among them, the Earth/Moon flyby on April 10th 2020. Due to the flight configuration, not all the instruments onboard BepiColombo are able to operate during cruise and flybys. Among the instruments that can operate is MERTIS, providing the first hyperspectral observation of the Moon in the thermal infrared (TIR) wavelength range from space.

At the Planetary Spectroscopy Laboratory (PSL) of DLR in Berlin, a spectral library for lunar analog rocks in the TIR spectral range, measured under simulated Moon surface conditions, has been built to help the interpretation of MERTIS’ Moon spectra.

Shortly after launch, MERTIS underwent a Near-Earth Commissioning Phase on Nov. 13-14 2018 during which the instrument was turned on for the first time in space. MERTIS was found to be fully operational [4], and the radiometer showed an excellent correspondence of the 2013 preflight sensitivity measurements and the 2018 in-flight measurements.

Although most instruments on the BepiColombo MPO are blocked by the Mercury Transfer Module (MTM) during cruise and flyby operations, MERTIS is able to acquire data through its space baffle. We adapted the MERTIS operations software to allow for this unique opportunity. Especially the Earth/Moon fly-by is of interest, as the surface composition of the Moon and Mercury have been frequently compared in the literature [5-10]. Observing the Apollo and Luna landing sites with MERTIS, in combination with laboratory studies, provides extremely valuable ground truth for our MERTIS measurements.

The time allocated for MERTIS pointing to the Moon was 4 hours and started 1 day before closest approach. During this slot the Moon was in the FoV of MERTIS. The 4 hours visibility slot was divided in 4 segments of 1 hour approximately connected by short slews. The attitude in each segment was quasi inertial (no tracking, keeping the Sun within illumination constraints) with the Moon slowly drifting in the FoV such that it is aligned with the boresight right in the middle of the segment. Within the 4 hours allocated for observations the Moon was nearly fully illuminated.

In the last decades orbital spectroscopic observations of the lunar surface have greatly advanced our understanding of the global distribution of different rock types and their chemical compositions. This vast dataset is complemented by the first in situ reflectance spectra from the lunar surface obtained by the recent Chang’E 3 and current Chang’E 4 missions, which provide more detailed information about the mineralogy of local surface materials and the geological context of the landing sites [11].

A reliable quantification of mineral modal abundances from measured reflectance spectra requires the availability of laboratory spectra of comparable samples. Current spectral databases primarily contain spectra measured on powder samples, lacking spectra of coarse grained rock samples. Reflectance spectra are sensitive to grain size and surface roughness [12], the available powder spectra might not be sufficient for a quantitative interpretation of measured rock spectra.

Rock samples obtained during the Apollo missions indicate that lunar anorthosites are typically coarse grained and can reach grain sizes of more than 1 cm. Hence, the global abundance of anorthosite as the dominant rock type of the lunar surface suggests that such coarse grained rocks are ubiquitous.

Therefore the extension of the current spectral databases by new spectral data of whole rock samples is crucial for the interpretation of current remote and in-situ measurements.

The Planetary Spectroscopy Laboratory (PSL) of DLR in Berlin is a spectroscopy facility providing spectral measurements of planetary analogues from the visible to the far-infrared range for comparison with remote sensing spacecraft/telescopic measurements of extraterrestrial surfaces [13-17]. External simulation chambers are attached to the FTIR spectrometer to measure the emissivity of solid samples.

The samples selected for this work includes: - slabs and stone chunks of plagioclases bearing rocks such as anorthosite, diorite, monzodiorite, gabbro and diabas; several basalts, rhyolite, olivine, granite, andesite, labradorite, obsidian.

Samples are heated in vacuum slowly and gradually up to 400° C. Measurements were taken at 100° C, 200° C, 300° C and 400° C in the MIR and FIR spectral ranges.

Thermally processed samples are measured in hemispherical and bi-directional reflectance in the full spectral range from UV to FIR.

A sample of graphite measured in emissivity at increasing T, adopting the same configuration and procedure used for the samples was used as blackbody for emissivity calibration.

MERTIS on ESA BepiColombo will be the first instrument to obtain hyperspectral measurements of the Moon in the TIR spectral range from space. Here we present the first results combined with a spectral library of emissivity for lunar analog rocks measured under simulated Moon conditions.

How to cite: Maturilli, A., Helbert, J., Hiesinger, H., Alemanno, G., Schwinger, S., and D'Amore, M.: MERTIS seeing the Moon in the TIR: results from the first Bepicolombo flyby, Europlanet Science Congress 2020, online, 21 Sep–9 Oct 2020, EPSC2020-271, https://doi.org/10.5194/epsc2020-271, 2020.

EPSC2020-586
Thomas G. Müller, Martin J. Burgdorf, Stefan A. Buehler, and Marc Prange

We present a thermophysical model (TPM) of the Moon which matches the observed, global, disk-integrated thermal flux densities of the Moon in the mid-infrared wavelength range for a phase angle range from -90° to +90°.
The model was tested and verified against serendipitous multi-channel HIRS measurements of the Moon obtained by different meteorological satellites (NOAA-11, NOAA-14, NOAA-15, NOAA-17, NOAA-18, NOAA-19, MetOp-A, MetOp-B). The sporadic intrusions of the Moon in the deep space view of these instruments have been extracted in cases where the entire Moon was within the instruments' field of view. The HIRS long-wavelengths channels 1-12 cover the range from 6.5 to 15 μm, the short-wavelengths channels 13-19 are in the 3.7 to 4.6 μm range.

The model is based on an asteroid TPM concept (Lagerros 1996, 1997, 1998; Müller & Lagerros 1998, 2002), using the known global properties of the Moon (like size, shape, spin properties, geometric albedo, thermal inertia, surface roughness, see Keihm 1984; Racca 1995; Rozitis & Green 2011; Hayne et al. 2017), combined with a model for the spectral hemispherical emissivity which varies between 0.6 and 1.0 in the HIRS wavelength range (Shaw 1998; ECOSTRESS data base: https://ecostress.jpl.nasa.gov/). The spectral emissivity as well as characteristics of the surface roughness are crucial to explain the well-calibrated measurements.

Our Moon model fits the flux densities for the currently available 22 epochs (each time up to 19 channels) with an absolute accuracy of 5-10%. The phase curves at the different wavelengths are well explained. The spectral energy distributions are very sensitive to emissivity and roughness properties. Here, we see minor variations in the model fits, depending on the origin (phase and aspect angle related) of the thermal emission. We also investigated the influence of reflected sunlight at short wavelengths.

Our TPM of the Moon has a wide range of applications: (i) for Earth-observing weather satellites in the context of field of view and photometric calibration (e.g., Burgdorf et al. 2020); (ii) for interplanetary space missions (e.g., Hayabusa2, OSIRIS-REx or BepiColombo) with infrared instruments on board for an in-space characterization of instrument properites (e.g., Okada et al. 2018); (iii) to shed light on the thermal mid-infrared properties of the lunar surface on a global scale; and, (iv) to benchmark thermophysical model techniques for asteroids in the regime below 10 μm (e.g., observed by WISE in the W1 and W2 bands at 3.4 and 4.6 μm, by Spitzer-IRAC at 3.55 and 4.49 μm or from ground in M band at around 5 μm).


References:
Burgdorf M., et al. 2020, Remote Sens. 12, 1488; Hayne, P. et al. 2017, JGRE 122, 237; Keihm, S.J. 1984, Icarus 60, 568; Lagerros 1996,  A&A 310, 1011; Lagerros 1997, A&A 325, 1226; Lagerros 1998, A&A 332, 1123; Müller & Lagerros 1998, A&A 338, 340; Müller & Lagerros 2002, A&A 381, 324; Okada T. et al. 2018, P&SS 158, 46; Racca G. 1995, P&SS 43, 835; Rozitis & Green 2011, MNRAS 415, 2042.

 

How to cite: Müller, T. G., Burgdorf, M. J., Buehler, S. A., and Prange, M.: Thermophysical model of the Moon from 3.7 to 15 μm, Europlanet Science Congress 2020, online, 21 Sep–9 Oct 2020, EPSC2020-586, https://doi.org/10.5194/epsc2020-586, 2020.

EPSC2020-561ECP
| MI
Nicolas Bott, Jessica Flahaut, Mélissa Martinot, and Gen Ito

1. Introduction

One of the Moon’s most surprising characteristics is its crustal asymmetry; the farside hemisphere, dominated by ancient highlands and covered with a few mare deposits, has a different volcanic history than the (sampled) nearside [1]. Surface dating of the lunar mare basalts revealed that the volcanism on the Moon lasted between ~3.9-4.0 and ~1.2 Ga, with a peak in the volcanic activity ~3.6-3.8 Ga ago [2]. A recent study further demonstrated that the mineralogy of the nearside mare basalts reveals a late stage volcanism with high titanium and olivine contents [3]. More recent spectroscopic analyses focused on the farside’s crustal rocks composition (e.g. [4] for South Pole-Aitken [SPA] basin), but no comprehensive study of the farside mare compositions has been conducted up to now.

2. Data and methods

In this work, we used spectroscopic data of the Moon Mineralogy Mapper (M3) onboard Chandrayaan-1 to survey the mineralogy of all mare deposits in the VNIR domain (0.4-3 μm). Each mare unit was mosaicked separately and processed using the method of [5]: an IDL routine automatically computes and removes the continuum of each spectrum, and determines its spectral parameters (e.g. band centers, band areas, band depths, spectral slope). To compare with the mineralogy of the nearside [3], we also mosaicked three selected mare regions, each representative of one spectral unit. Finally, we applied statistics on spectral parameters of interest to survey the variation in mineral signatures and compositions of farside maria.

3. Preliminary results

We found that spectra of mare basalts are dominated by pyroxene signatures (Figure 1).

However, some mare units (e.g. Apollo, see Figure 2) showed considerable differences in band characteristics in which cases we computed statistics on each mare subunits.

Major differences were also observed in SPA mare units when they were compared to Mare Australe deposits and other maria outside of the SPA basin (Figure 3).

This suggests different pyroxene compositions within SPA. Moreover, the nearside mare units we defined based on [3] are clearly distinct from all farside mare deposits since they are the richest in clinopyroxenes (Figure 3).

4. Conclusion and perspectives

The results we have so far indicate slightly different mineralogies of mare basalts between the nearside and the farside of the Moon and, if confirmed by looking at the other spectral parameters, could mirror its crustal dichotomy. We plan to investigate possible evidence of olivine and possible correlations with age and location, as well as intra-SPA diversity with our spectral parameters set.

Acknowledgements

The authors want to thank Jan Hendrik Pasckert and Harald Hiesinger for having kindly shared with us their shapefiles of SPA mare deposits [8]. Fundings from the CNRS Momentum, LUE Future Leader and CNES APR are much appreciated.

References

[1] Head III, J. W., and Wilson, L.: Lunar mare volcanism: Stratigraphy, eruption conditions, and the evolution of secondary crusts, Geochimica et Cosmochimica Acta, Vol. 56, 1992.

[2] Hiesinger, H., et al.: Ages of mare basalts on the lunar nearside, Journal of Geophysical Research, Vol. 105, 2000.

[3] Staid, M. I., et al.: The mineralogy of late stage lunar volcanism as observed by the Moon Mineralogy Mapper on Chandrayaan-1, Journal of Geophysical Research, Vol. 116, 2011.

[4] Moriarty, D. P., and Pieters, C. M.: The Character of South Pole-Aitken Basin: Patterns of Surface and Subsurface Composition, Journal of Geophysical Research, Vol. 123, 2018.

[5] Martinot, M., et al.: Mineralogical Diversity and Geology of Humboldt Crater Derived Using Moon Mineralogy Mapper Data, Journal of Geophysical Research, Vol. 123, 2018.

[6] Klima, R. L., et al.: Spectroscopy of synthetic Mg-Fe pyroxenes I: Spin-allowed and spin-forbidden crystal field bands in the visible and near-infrared, Meteoritics & Planetary Science, Vol. 42, 2007.

[7] Adams, J. B.: Visible and near-infrared diffuse reflectance spectra of pyroxenes as applied to remote sensing of solid objects in the solar system, Journal of Geophysical Research, Vol. 79, 1974.

[8] Pasckert, J. H., Hiesinger, H., Van der Bogert, C. H.: Lunar farside volcanism in and around the South Pole-Aitken basin, Icarus, Vol. 299, 2018.

How to cite: Bott, N., Flahaut, J., Martinot, M., and Ito, G.: Unveiling the mineralogical composition of lunar farside mare basalts, Europlanet Science Congress 2020, online, 21 Sep–9 Oct 2020, EPSC2020-561, https://doi.org/10.5194/epsc2020-561, 2020.

EPSC2020-427
Dina Bower, Prabhakar Misra, Marianne Peterson, Madison Howard, Tilak Hewagama, Nicolas Gorius, Steven Li, Shahid Aslam, Timothy Livengood, Amy McAdam, and John Kolasinski

Introduction:  The ability to discriminate between different mineral phases in lunar materials is critical in reconstructing the origin and evolution of the moon and understanding its relationship to Earth.  Resource identification is also critical to develop a viable long-term lunar exploration program enabling a continued human presence. Mineral-bound metals are important resource targets in regolith and mare basalts [1]. Minerals in lunar basalts and regolith such as ilmenite and pyroxene are known hosts of metals like Cr, Ni, Co, and Mn, and ilmenite in particular has been considered for Fe and O2 extraction [2][3].  

     Raman spectroscopy non-destructively provides structural information to identify trace compounds and minerals in a matter of seconds. Raman spectroscopy has been used for decades to measure the composition of returned lunar samples and analog materials ([4][5][6] and references therein). Raman measurements can be undertaken with multiple excitation wavelengths, (UV ~244nm, VIS ~532nm, NIR ~785nm, and IR ~1064nm), with advantages to using one excitation wavelength over another. The 532 nm wavelength provides high-energy excitation with good sensitivity and low noise for most materials covering a wide spectral range (~0 – 4000 cm-1). This wide range is essential for the identification of volatiles, in which spectral shift for functional groups like OH occur within ~3000 - 3700 cm-1, and minerals with peak shifts ~100-200 cm-1, such as sulfides, feldspars, and quartz polymorphs. NIR Raman has been shown to exhibit better signal-to-noise, particularly for opaque minerals, like sulfides and oxides, and is the typical wavelength utilized in portable Raman instruments for terrestrial resource prospecting ([7][8]).  The two wavelengths used together ensure near-comprehensive identification and accurate characterization of lunar materials suitable for resource extraction.

Materials and Methods:  This study looks at a suite of lunar analog mineral samples (olivine, plagioclase, pyroxene, ilmenite, apatite) and relevant terrestrial analog rocks using portable and benchtop VIS (532nm) and NIR (780nm) Raman spectroscopy and Fourier transform infrared spectroscopy for comprehensive characterization of composition. Samples were probed either in tact or as powders at room temperature. A subset of powdered samples was heated  (T= 298K, 325K, and 373K) and characterized using NIR Raman to study temperature dependence of Raman spectra.

Initial Results: The mineral samples included in the study were all identifiable using both VIS and NIR Raman spectroscopy, and in some cases the portable instruments performed better than the high-resolution benchtop systems. Basalt and ilmenite samples were better characterized under NIR excitation, while the silicate minerals had a better response under VIS excitation (Fig. 1). FTIR measurements of the silicate minerals were informative, but the opaque nature of ilmenite results in low reflectance under higher wavelengths. For both Raman and FTIR measurements, better results were achieved with the pure minerals in comparison to the rocks composed of multiple minerals. The NIR Raman temperature experiments showed an enhancement of spectral peak intensity for minerals like plagioclase as the temperature increased up to 373K.

Ongoing and Future Work: We have demonstrated that Raman excitation under both VIS and NIR provides useful information to identify lunar minerals of interest to the lunar science community as well as for in situ resource identification, with some advantages for one or the other depending on the target sample. IR (2-16 mm) reflectance spectroscopy is useful for silicates, but opaque minerals like ilmenite require lower wavelengths for identification. Our lab is currently exploring VIS-SWIR reflectance (~0.5 – 2.5 mm as a viable alternative, and further work exploring temperature effects on Raman spectra relevant to the lunar surface is also being done.

Acknowledgements: M. Peterson, M. Howard and P. Misra would like to acknowledge the financial support received from the REU Site in Physics at Howard University (NSF Award # PHY 1659224). D. Bower, S. Li, T. Hewagama, S. Aslam, J. Kolasinski, N. Gorius, T. Livengood, and A. McAdam would like to acknowledge the support of the Internal Research and Development and Fundamental Laboratory Research Programs at Goddard Space Flight Center.

References: [1] Taylor, G. J. and Martel, L. M. V. (2003) Adv. In Sp. Res., 31, 2403-2412. [2] James, O. B. (1973) XX. [3] Papike J., Taylor L., and Simon S. (1991) in Lunar Sourcebook, pg. 121. [4] Wang, A. et al. (2001) American Mineralogist, 86, 790-806. [5] Jolliff, B. et al. (2006) American Mineralogist, 91, 1583-1595. [6] Ling, Z.C. et al. (2011) Icarus, 211,101-113. [7] Jehlicka and Vandenabeele (2015) Journal of Raman Spectroscopy, 46, 927-932. [8] Ando and Garzanti (2014) Geological Society of London Spec. Pub, 386, 395-412.

How to cite: Bower, D., Misra, P., Peterson, M., Howard, M., Hewagama, T., Gorius, N., Li, S., Aslam, S., Livengood, T., McAdam, A., and Kolasinski, J.: Comparative VIS and NIR Raman and FTIR Spectroscopy of Lunar Analog Samples, Europlanet Science Congress 2020, online, 21 Sep–9 Oct 2020, EPSC2020-427, https://doi.org/10.5194/epsc2020-427, 2020.

EPSC2020-530
Philipp Gläser, Anton Sanin, Jean-Pierre Williams, Igor Mitrofanov, and Jürgen Oberst

Abstract

We modeled (sub-)surface temperatures for the upper two-meter regolith layer near the lunar poles. The temperature maps are compared to the observed hydrogen signal from the Lunar Enhanced Neutron Detector (LEND). We focused our study on six Neutron Suppression Regions (NSRs).

Introduction

The lunar poles offer a thermal environment with surface temperatures allowing for water ice to accumulate, especially in Permanently Shadowed Regions (PSRs) commonly found at crater floors [1]. Extensive remote sensing and modeling techniques were applied from a series of missions to detect and quantify potential deposits (e.g. [2][3]). Although plausible evidence was found from orbiting spacecrafts, alternative explanations are still possible, e.g. roughness, fresh surface material, hydroxyl (OH) bearing minerals etc. However, the Lunar Crater Observation and Sensing Satellite (LCROSS) found direct evidence of water through impacting within the PSR of Cabeus crater. LEND [4] observations revealed several NSRs [5], i.e. hydrogen-rich areas which are typically found within PSRs. However, some NSRs are occasionally in sunlight creating surface temperatures at which water ice cannot be stable. At specific thermal conditions, i.e. maximum and average temperatures are 120 K and 105 K respectively, an ice pumping mechanism into the sub-surface is activated [6].

We investigate to which extent temperatures correlate with LEND’s hydrogen signal and whether or not ice pumping can explain the existence of some of the NSRs.

Data and Method

Our study is based on polar 650x650 km Lunar Orbiter Laser Altimeter (LOLA) Digital Terrain Models (DTMs) [7][8].

Lunar (sub-)surface temperatures are modeled by solving the 1D heat equation [9]. We treat the Sun as an extended source considering the limb-darkening effect. Heat conduction is modeled within the upper two meters of regolith and temperatures are derived for 30 layers. Multiple scattering and re-radiation of VIS and IR is evaluated at each pixel from a 50x50 km window. Earth-shine (VIS and IR) and a constant radiogenic heat source of 0.016 W/m² are also incorporated in the model.

The DTMs were synthetically illuminated [10] in 12-h time steps for a 19-year period, 01-01-1991 to 01-01-2010. Since similar illumination conditions occur at the start and end time we could iterate the process until temperatures converged. After 5 iterations (i.e. 95 years) we found an equilibrated solution from which we derived results presented in this study.

Our investigated NSRs are: areas near Whipple, Fibiger and Peary at the north pole and areas inside Shoemaker, Haworth and Cabeus crater at the south pole. For each NSR we derived minimum, average and maximum temperature maps. Additionally, maps of suppression parameter ξ were prepared. The suppression parameter represents the ratio between the average neutron counting within LEND’s field-of-view to the average neutron counting of a hydrogen-poor reference area [5].

3. Results

To determine whether or not temperature and suppression parameter maps correlate we needed to set thresholds. For instance, the threshold for temperature below which we assume water ice to be stable is 110 K [11]. The threshold for the suppression parameter ξ was set to 0.83. We found this threshold by evaluating the observed ξ around the LCROSS impact site for which we know that water ice is present.

At each depth layer we compared the overlap of the two emerging areas of potential water ice, one determined by temperature and the other determined by ξ (see Fig. 1). We also derived growth rates (%/cm) indicating whether significant increase in overlap (%) is achieved by comparing ξ to temperature layers in greater depth (cm). For the south polar NSRs we find that both areas overlap > 95% and ice appears to be present within the upper 19 cm of regolith. The north polar NSRs show an overlap of ~50-70% and ice seems to be buried to greater depths, e.g. 65 cm. In fact, we found that maximum and average temperatures create ideal conditions for ice pumping into the sub-surface.

4. Discussion

Our south polar NSRs reside in PSRs, i.e. the coldest areas on the Moon. They follow the classical view on how water ice deposits at the poles: water molecules hop over the lunar surface and eventually get trapped and accumulate in PSRs. Our selected north polar NSRs, however, reside in non-PSR areas which are occasionally in sunlight and are generally too warm for water ice to be stable. Ice pumping seems to be the explanation for those locations. We could show that NSRs and modeled temperatures do correlate, either at surface or sub-surface level.

Acknowledgements

P. Gläser was funded by a Grant of the German Research Foundation (GL 865/2-1). We gratefully acknowledge the support of NVIDIA Corporation with the donation of a Quadro P6000 GPU used for this research. Last, we wish to thank the LRO Science Teams for releasing such wonderful data products.

 

References

[1] Watson, K. et al. 1961, Journal of Geophysical Research 66, 1598–1600

[2] Nozette, S. et al. 1996, Science 274, 1495–1498

[3] Paige, D.A. et al. 2010, Science 330, 479

[4] Mitrofanov, I.G. et al. 2010, Science 330, 483

[5] Sanin, A.B. et al. 2017, Icarus 283, 20–30

[6] Schorghofer, N. et al. 2010, The Astrophysical Journal 788, 169

[7] Gläser, P. et al. 2018, Planetary and Space Science 162, 170–178

[8] Gläser, P. et al. 2013, Planetary and Space Science 89, 111–117

[9] Gläser, P. et al. 2019, Astronomy & Astrophysics 627, A129

[10] Gläser, P. et al. 2014, Icarus 243, 78–90

[11] Vasavada, A.R. et al. 1999, Icarus 141, 179–193

How to cite: Gläser, P., Sanin, A., Williams, J.-P., Mitrofanov, I., and Oberst, J.: Comparison of LEND's hydrogen signal with modeled (sub-)surface temperatures in the lunar polar regions, Europlanet Science Congress 2020, online, 21 Sep–9 Oct 2020, EPSC2020-530, https://doi.org/10.5194/epsc2020-530, 2020.

EPSC2020-14
Bernard Foing and the ILEWG EuroMoonMars Core Team 2018-2020

The EuroMoonMars Programme started in 2009 by ILEWG, ESA ESTEC, NASA, VU Amsterdam and supported by various space agencies, universities and academic or industrial partners has to bring together : space science and astronomy, Earth and planetary sciences and biology, technology, field work campaigns in extreme environments, resource utilisation and economy, human factors, international cooperation. Space and society, bridging to Arts and social sciences through the ArtMoonMars initiative.

We shall describe how EuroMoonMars can contribute to European astronomy and space science: public and political engagement education in areas of education, research, innovation, culture, youth and sport policies, and industry, digital single market, space and safety, policies .

The International Lunar Exploration Working Group (ILEWG) is a public forum sponsored by the world's space agencies to support "international cooperation towards a world strategy for the exploration and utilization of the Moon - our natural satellite" (International Lunar Workshop, Beatenberg (CH), June 1994). ILEWG was founded by several space agencies: ASA, ASI, BNSC, CNES, DARA, ESA, ISAS, NASA, NASDA, RSA. ILEWG has been organising since 1994 the ICEUM International Conferences on Exploration & Utilisation of the Moon with published proceedings, and where community declarations have been prepared and endorsed by community participants. ILEWG has co-organised and co-sponsored lunar sessions at EGU, COSPAR, EPSC. Declarations from ICEUM conferences  cover all aspects of science, technology, cooperation, industry, society and inspiration. ICEUM13 took place together with COSPAR in Pasadena in 2018, and ICEUM14 with EPSC-DPS in Geneva in 2019. Next ICEUM15 is to take place with COSPAR B/PEX symposia (co-chairs: C. Pieters, B. Foing, G. Schmidt, C. Heinicke), in Sydney in January 2021.

ILEWG founded in 2009 the EuroMoonMars initiative, which comprises field campaigns in Moon-Mars analogue environments.The EuroMoonMars field campaigns have been organised in specific locations of technical, scientific and exploration interest. The campaigns started with EuroGeoMars2009 (Utah MDRS, 24 Jan-1 Mar 2009) with ILEWG, ESA ESTEC, NASA Ames, VU Amsterdam and GWU and continued yearly at MDRS and other extreme field sites on Earth.

The EuroMoonMars campaigns consist of research activities for data analysis, instruments tests and development, field tests in Moon-Mars analogues, pilot projects, training and hands-on workshops and outreach activities.

In 2019 ILEWG contributed to IgLuna first ESA Lab inter-University demonstrator project,  hosted by the Swiss Space Centre (SSC) with the vision to create an analogue habitat inside lunar ice caps. The campaigns were held from 17–30 June 2019 and involved 18 student teams from 9 countries across Europe. The students developed modular demonstrators and tested them during a field test conducted inside the moon-like extreme environment of the Glacier Palace inside the Zermatt Matterhorn glacier.

Currently, ILEWG is collaborating with the International Moonbase Alliance (IMA)] and the Hawaii Space Exploration Analog and Simulation (HI-SEAS) on a series of EuroMoonMars, IMA and HI-SEAS (EMMIHS) campaigns, at the HI-SEAS analogue facilities in Hawaii.

ArtMoonMars, Moon Village & ITACCUS (IAF ITACCUS Committee on Socio Cultural Utilisation of Space) activities were performed, with emphasis on events and workshops. The Moon Village is an open concept proposed with the goal of a sustainable human and robotic presence on the lunar surface as an ensemble where multiple users can carry out multiple activities. We want to involve everybody including Socio cultural and Artistic aspects. Why ArtMoonMars? Artists can convey multiple messages of the community including planetary science, life sciences, astronomy, fundamental research, resources utilisation, human spaceflight, peaceful cooperation, economical development, inspiration, training & capacity building.

References

https://en.wikipedia.org/wiki/International_Lunar_Exploration_Working_Group

How to cite: Foing, B. and the ILEWG EuroMoonMars Core Team 2018-2020: ILEWG EuroMoonMars Highlights 2018-2020, Europlanet Science Congress 2020, online, 21 Sep–9 Oct 2020, EPSC2020-14, https://doi.org/10.5194/epsc2020-14, 2020.

EPSC2020-1020
| MI
Michaela Musilova, Ana Nunes, Sabrina Kerber, Charlotte Pouwels, Ariane Wanske, Joseph D'Angelo, Bernard Foing, and Henk Rogers

Introduction: 

Simulated missions to the Moon and Mars have been taking place at the analog research station HI-SEAS (Hawaii - Space Exploration Analog and Simulation) since 2013. The so-called Martian and lunar habitat, HI-SEAS, is located in Hawaii and its research projects are run by the International Moonbase Alliance (IMA) [1]. Numerous aspects of space missions are simulated in order to make them be as realistic as possible, including time delays in communication, emergency procedures and performing relevant research.

In 2019, the EuroMoonMars campaign was launched at HI-SEAS, bringing together researchers from the European Space Agency (ESA), IMA, the International Lunar Exploration Working Group (ILEWG), VU Amsterdam and many other international organizations [2,3]. The campaign aims to increase awareness about the research and technology testing that can be performed in analog environments, in order to help humans become multi-planetary species. Furthermore, the research and technological experiments conducted at HI-SEAS are going to be used to help build a Moon base in Hawaii, and ultimately to create an actual Moonbase on the Moon, as part of IMA’s primary goals [3,4,5].

 

The EMMIHS II mission research: 

EMMIHS-II was the second campaign organized by the EuroMoonMars group, taking place from December 8th-22nd, 2019. When the crew left the HI-SEAS habitat, they wore analog space-suits and went through full extravehicular activity (EVA) protocols to perform their research in the simulated lunar terrain. The crew was supported by a Mission Control Center (MCC) based in Hawaii and a Remote Support team based at EuroMoonMars ESA/ESTEC in the Netherlands [2,3,4,5]. The main research themes of the EMMIHS-II campaign were as follows:

Engineering research: Crew engineers are responsible for numerous tasks to ensure nominal operations and the maintenance of the EVA and habitat equipment. They prepare a daily Engineering Report for the MCC, which includes the status of the equipment, recommendations for improvements and any requests for support. They are also responsible for supporting other crew members’ research projects if needed.  At least two crewmembers should serve as crew engineers with strong analytical, troubleshooting and hands-on technical skills.

Lava tubes as habitats: Detailed investigations were performed of the lava tubes in the vicinity of the HI-SEAS habitat [Figure 1]. They were subsequently compared to lava tubes on the Moon, with the intension of creating an environmental guideline for the architectural lunar habitat development in lava tubes.