• 천문학회보
• /
• 제40권1호
• /
• pp.62.1-62.1
• /
• 2015

Polarization of the light reflected off the Moon provides information on the size and composition of the particles in the lunar regolith. The mean particle size of the regolith can be estimated from the combination of the albedo and degree of polarization, while the color ratio of the parallel-component polarization (CP) has been suggested to be related to the amount of nanophase metallic iron (npFe^0) inside the regolith particles. Both the mean size and npFe^0 abundance of the particles have been used as maturity indicators of the regolith since sustained impacts of high energy particles and micro-meteoroids cause comminution of particles and production of npFe^0. Based on our multispectral polarimetric observations of the whole near side of the Moon in the U, B, V, R, and I bands, we compare the maps of the mean particle size, CP, and the optical maturity (OM). We find that the mean particle size map is sensitive to the most immature (~0.1 Gyr) soil, the OP map to the intermediate immaturity (a few 0.1 Gyr) soil, and the CP map to the least immature (~1 Gyr) soil.

• Advances in Computational Design
• /
• 제4권2호
• /
• pp.141-153
• /
• 2019

This research is comprised of virtually simulating behavior while experiencing low gravity effects in advance of real world testing in low gravity aboard Zero Gravity Corporation's (Zero-G) research aircraft (727-200F). The experiment simulated a drill rig penetrating a regolith simulant. Regolith is a layer of loose, heterogeneous superficial deposits covering solid rock on surfaces of the Earth' moon, asteroids and Mars. The behavior and propagation of space debris when drilled in low gravity was tested through simulations and visualization in a leading dynamic simulation software as well as discrete element modeling software and in preparation for comparing to real world results from flying the experiment aboard Zero-G. The study of outer space regolith could lead to deeper scientific knowledge of extra-terrestrial surfaces, which could lead us to breakthroughs with respect to space mining or in-situ resource utilization (ISRU). These studies aimed to test and evaluate the drilling process in low to zero gravity environments and to determine static stress analysis on the drill when tested in low gravity environments. These tests and simulations were conducted by a team from Texas A&M University's Department of Construction Science, the United States Air Force Academy's Department of Astronautical Engineering, and Crow Industries

• Journal of Astronomy and Space Sciences
• /
• 제41권2호
• /
• pp.79-85
• /
• 2024

Nowadays, the trend in lunar exploration missions is shifting from prospecting lunar surface to utilizing in-situ resources and establishing sustainable bridgehead. In the past, experiments were mainly focused on rover maneuvers and equipment operations. But the current shift in trend requires more complex experiments that includes preparations for resource extraction, space construction and even space agriculture. To achieve that, the experiment requires a sophisticated simulation of the lunar environment, but we are not yet prepared for this. Particularly, in the case of lunar regolith simulants, precise physical and chemical composition with a rapid development speed rate that allows different terrains to be simulated is required. However, existing lunar regolith simulants, designed for 20th-century exploration paradigms, are not sufficient to meet the requirements of modern space exploration. In order to prepare for the latest trends in space exploration, it is necessary to innovate the methodology for producing simulants. In this study, the basic framework for lunar regolith simulant development was established to realize this goal. The framework not only has a sample database and a database of potential simulation target compositions, but also has a built-in function to automatically calculate the optimal material mixing ratio through the particle swarm optimization algorithm to reproduce the target simulation, enabling fast and accurate simulant development. Using this framework, we anticipate a more agile response to the evolving needs toward simulants for space exploration.

• 한국지형학회지
• /
• 제18권1호
• /
• pp.57-71
• /
• 2011

남해안의 고성에 위치하는 월치고개 단면은 10m 두께의 화강암 풍화층으로써, 10YR 4/4에 가까운 적색을 띠고 있어서 고온다습했던 고기후의 산물로 판단되기 쉬운 단면이다. 그러나 단면관찰과 박편분석, XRD 동정과 지화학적 분석을 통해 살펴본 결과, 열수변성의 대표광물인 할로이사이트가 단면 전체에서 보편적으로 나타나고 있으며, 한반도의 일반적 화강암 풍화층의 화학적 풍화율인 60~70%보다 훨씬 높은 97%에 달하였다. 이는 기후지형학적 풍화에 의해 형성된 적색풍화층이 아니라, 지열수에 의한 열수변성 가능성이 매우 높게 단면으로 판단된다.

• 한국지반공학회논문집
• /
• 제31권7호
• /
• pp.53-63
• /
• 2015

최근 우주개발의 중요성이 다시 부각되면서 주요 우주개발국들은 달 토양과 물리적 화학적 특성이 유사한 인공월면토(lunar simulant)를 개발하여 각종 연구에 활용하고 있다. 달 토양은 지구 토양과 생성 매커니즘과 지반공학적 거동이 다르기 때문에 완벽하게 모사하는 것이 어렵고 제작비용이 많이 소모된다. 기존 인공월면토 중 국제적으로 가장 널리 사용되고 있는 재료는 미국항공우주국(NASA)에서 제작한 JSC-1A이며, 우리나라는 아직 국제적으로 공인된 인공월면토가 없는 실정이다. 따라서 본 연구에서는 국내 지반재료를 이용한 한국형 인공월면토 개발을 위한 기초연구를 수행하여 그 시제품으로 KLS-1(Korea lunar simulant - type 1)을 제시하였다. KLS-1은 기존 국외 인공월면토들과 비교하여 유사성과 경제성이 우수하여 향후 국내 우주개발 사업뿐만 아니라 각종 국제연구에 폭 넓게 활용될 수 있을 것으로 기대된다.

• 한국철도학회:학술대회논문집
• /
• 한국철도학회 2010년도 춘계학술대회 논문집
• /
• pp.1951-1957
• /
• 2010

Study of Lunar exploration is progressed and manned lunar exploration is planned. In order to explore in Lunar, we need habitat to stay for a long time and system that mine, classify and transport materials. Lunar has dust that is very light-tiny. That is on the air for a long time so there are problems to adject transportation system such as vehicle. However, it can solve the problem to use pipe transportation system. This transportation system help materials move continually and is more effective than other transportation system such as train or vehicle. For those positive points, some experts studied about tube transportation systems. I introduce these system and find out factors that can be used in Lunar regolith transportation system. I suggest Lunar regolith transportation system, using the factors.

• 천문학회보
• /
• 제36권2호
• /
• pp.103.2-103.2
• /
• 2011

We measure the degree of polarization of the lunar regolith to map the distributions of the age and the particle size. We use a 12cm refracting telescope with a 2k-square pixel color CCD (R band) and a polarization filter. The angular resolution obtained is 3.02 km/pixel. Our goal is to obtain a map of the lunar particle size distribution on the lunar regolith and then that of the age distribution. Polarization of the light scattered by lunar surface contains information on their mean particle size. The mean particle size of the lunar surface has been decreased by continued micro-meteoroid impact over a long period. One can estimate the age of the lunar surface if the mean particle size is known. Particle sizes can be measured through observations of polarization because the mean particle size is related to the maximum polarization and albedo. The age and the particle size of the lunar regolith can give vital information for the future lunar exploration.

• 한국항공우주학회지
• /
• 제42권4호
• /
• pp.284-290
• /
• 2014

성공적으로 달 탐사를 수행하기 위해서는 달착륙선의 안전한 착륙이 보장되어야 한다. 그러므로 안전한 착륙을 저해하는 착륙 시 충격하중을 감소시키기 위해서는 효율적인 달착륙선 충격흡수장치를 설계해야 한다. 또한 더욱 현실적인 달착륙선 설계를 위해서는 달 토양의 특성을 고려하는 것이 중요하다. 이에 본 논문에서는 달 토양의 특성을 반영한 달착륙선 착륙 해석 모델을 구축하고, 효율적인 충격력 감소를 위해 달착륙선의 충격흡수장치에 대한 최적설계를 수행하였다. 최적설계는 메타모델 기반의 순차적 근사 최적설계기법을 이용하여 수행하였으며, 최적설계 결과로 부터 본 연구에서 사용된 최적화 방법을 통해 달착륙선에 가해지는 충격력을 효과적으로 저감시킬 수 있음을 확인하였다.

• 천문학회보
• /
• 제40권2호
• /
• pp.45.3-46
• /
• 2015

Space weathering agents such as micrometeoroids and solar wind particles continuously age the uppermost regolith of the lunar surface by comminuting as well as darkening and reddening. Among several maturity indices, we investigate median grain size () and optical maturity (OMAT) of the crater rim walls. Crater rim wall is the most immature place among the impact crater features because the vertical mixing process by mass-movement can enhance the gardening of regolith and the supply of immature materials in the deeper layer to the surface. More than 140 simple and complex craters were considered. Both and OMAT values of the inner rim wall initially increase as the crater size increases until ~10-20 km, then decrease. This transition crater size happens to correspond to the transition diameter from simple to complex craters. For larger craters, i.e., complex craters, it is clear that the inner rim wall of the craters formed in recent eras tend to remain fresh and become mature along with time. For the simple crater case, smaller craters are more mature, which is opposite to the case of complex craters. This is thought to be because smaller craters become flattened more quickly, thus have smaller vertical mixing in the regolith due to mass-movement. We will also discuss on the maturity indices of the crater rim walls at high latitudes as a function of the position angle to see the latitude dependence of the space weathering process.

• 천문학논총
• /
• 제30권2호
• /
• pp.65-67
• /
• 2015

The surfaces of most atmosphereless solar system objects are referred to as regolith, layers of loosely connected fragmentary debris, produced by meteorite impacts. Measurements of light scattered from such surfaces provides information about the composition and structure of the surface. A suitable way to characterize the scattering properties is to consider how the intensity and polarization of scattered light depends on the particle size, composition, porosity, roughness, wavelength of incident light and the geometry of observation. In the present work, the effect of porosity on bidirectional reflectance as a function of phase angle is studied for alumina powder with grain size of $0.3{\mu}m$ and olivine powder with grain size of $49{\mu}m$ at 543.5 nm. The optical constants of the alumina sample for each porosity were calculated with Maxwell Garnett effective medium theory. On using each of the optical constants of alumina sample in Mie theory with the Hapke model the variation of bidirectional reflectance is obtained as a function of phase angle with porosity as a parameter. Experimental reflectance data are in good agreement the model. For the olivine sample the effect of porosity is studied using Hapke (2008).