Polar regions of the moon as a potential repository of solar-wind-implanted gases

Starukhina, L. V.

doi:10.1016/j.asr.2005.04.033

Cited by 67 publications

(72 citation statements)

References 19 publications

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“…We will examine this particular implantation scenario. Starukhina (2001Starukhina ( , 2006Starukhina ( , 2012 examined solar wind proton implantation even prior to the discovery of the extended OH veneer in 2009; this for explaining the possible build up of H in cold trap regions of craters and on cold asteroids. As described in these foundation-level works, 1 keV solar wind protons will undergo charge exchange with the surface neutrals (see also Hodges (2011)) and implant as H in the first 100 nm of regolith material.…”

Section: Implantation Of Protons Into Oxygen-rich Regolithmentioning

confidence: 99%

“…As described in these foundation-level works, 1 keV solar wind protons will undergo charge exchange with the surface neutrals (see also Hodges (2011)) and implant as H in the first 100 nm of regolith material. However, their diffusion time, s D , back out into free space is a strong function of surface temperature and number of 'trapping' defects (i.e., crystal lattice vacancies) (Starukhina, 2006(Starukhina, , 2012Dyar et al, 2010). The ability of a region in a crystal to locally trap a free hydrogen is represented by the activation energy, U, with large values of U (>1 eV) representative of locations where the H is locally trapped and would have difficulty migrating away.…”

Section: Implantation Of Protons Into Oxygen-rich Regolithmentioning

confidence: 99%

“…In this paper, we will perform an investigation of the solar wind implantation process, expanding the fundamental work on the subject originally presented by Starukhina (2001Starukhina ( , 2006Starukhina ( , 2012 This is an open access article under the CC BY-NC-ND license (http://creativecommons.org/licenses/by-nc-nd/3.0/). These past works considered the possibility that implantation, Htrapping at defect sites, and OH formation was possibly occurring in cold lunar polar craters and on cool asteroids.…”

Section: Introductionmentioning

confidence: 99%

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Solar wind implantation into lunar regolith: Hydrogen retention in a surface with defects

Farrell

Crider

Zimmerman

2015

Icarus

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a b s t r a c t Solar wind protons are implanted directly into the top 100 nm of the lunar near-surface region, but can either quickly diffuse out of the surface or be retained, depending upon surface temperature and the activation energy, U, associated with the implantation site. In this work, we explore the distribution of activation energies upon implantation and the associated hydrogen-retention times; this for comparison with recent observation of OH on the lunar surface. We apply a Monte Carlo approach: for simulated solar wind protons at a given local time, we assume a distribution of U values with a central peak, U c and width, U w , and derive the fraction retained for long periods in the near-surface. We find that surfaces characterized by a distribution with predominantly large values of U (>1 eV) like that expected at defect sites will retain implanted H (to likely form OH). Surfaces with the distribution predominantly at small values of U (<0.2 eV) will quickly diffuse away implanted H. However, surfaces with a large portion of activation energies between 0.3 eV < U < 0.9 eV will tend to be H-retentive in cool conditions but transform into H-emissive surfaces when warmed (as when the surface rotates into local noon). These mid-range activation energies give rise to a diurnal effect with diffusive loss of H at noontime. Published by Elsevier Inc. This is an open access article under the CC BY-NC-ND license (http://creativecommons.org/licenses/by-nc-nd/3.0/).

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Section: Implantation Of Protons Into Oxygen-rich Regolithmentioning

confidence: 99%

Section: Implantation Of Protons Into Oxygen-rich Regolithmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Solar wind implantation into lunar regolith: Hydrogen retention in a surface with defects

Farrell

Crider

Zimmerman

2015

Icarus

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“…Compared with the copious 3 He fed by solar wind, the 3 He saturation limit for lunar regolith is easier to be met though some areas are less effective on 3 He trapping under the influences of lunar longitude and latitude, the Earth's magnetic field and lunar rotation. Starukhina [35] has confirmed that lunar regolith can fast reach its saturation limit of solar wind volatiles. At low latitudes, the saturation time is very short, 100 years or so.…”

Section: Effects Of Solar Wind Flux On Lunar Regolith 3 He Abundancementioning

confidence: 55%

Lunar 3He estimations and related parameters analyses

Liu

Zhang

et al. 2010

Sci. China Earth Sci.

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As a potential nuclear fuel, 3 He element is significant for both the solution of impending human energy crisis and the conservation of natural environment. Lunar regolith contains abundant and easily extracted 3 He. Based on the analyses of the impact factors of 3 He abundance, here we have compared a few key assessment parameters and approaches used in lunar regolith 3 He reserve estimation and some representative estimation results, and discussed the issues concerned in 3 He abundance variation and 3 He reserve estimation. Our studies suggest that in a range of at least meters deep, 3 He abundance in lunar regolith is homogeneously distributed and generally does not depend on the depth; lunar regolith has long been in a saturation state of 3 He trapped by minerals through chemical bonds, and the temperature fluctuation on the lunar surface exerts little influence on the lattice 3 He abundance. In terms of above conclusions and the newest lunar regolith depth data from the microwave brightness temperature retrieval of the "ChangE-1" Lunar Microwave Sounder, a new 3 He reserve estimation has been presented.The fast population expanding, elevated standards of living, and ever-increasing industrialization of the developing nations make world energy consumption grow rapidly, thus put unprecedented pressures on the Earth's resources and environment. Scientists predict that the Earth's energy supplies will have to increase by a factor 3 to 6 in the 21st century, and the 21st century will be the last century in which fossil fuels play a dominant role [1]. One of the effective solutions of this energy resource crisis is the utilization of nuclear energy released by nuclear fission and fusion. However, nuclear fission usually produces many radioactive wastes potentially threatening the security of human kind. Compared to the "traditional" nuclear fuel reaction process releasing 80% neutrons, the reaction between 3 He and Deuterium only generates a few percent of neutrons, which is characterized by enormous reduction of radioactivity, even without nuclear wastes, greatly lowered radiation damage to reactor, safe operation, very high overall operation efficiency, lower cost of electricity, and shorter time to commercial electrical power plants [2,3]. Especially, the 3 He-3 He reaction does not release neutrons, completely without the radioactive wastes and radioactivity worried by people [1,4], and can provide mankind with environment-friendly and inexhaustible electric energy [5]. 3 He, therefore, is the type of nuclear fusion fuel that can be long used, safe, highly efficient, and controllable, with vast developing potential.The Earth is deficient in 3 He resources. Kulcinski [2] believes that the 3 He available on the Earth is from two sources. One is from underground natural gases, with a total reserve of some 200 kg; the other from decaying tritium in thermonuclear weapons and heavy water CANDU fission plants, about 300 kg. Murali and Jordan [6] hold that the known 3 He in terrestrial natural gas deposits could not e...

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“…At the lunar polar regions, the hydrogen concentration has been confirmed (Feldman et al, 1998(Feldman et al, , 1999(Feldman et al, , 2001Lawrence et al, 2006) although whether hydrogen on the pole regions form water or not, and the origin of the hydrogen has been studied (e.g. Butler, 1997;Starukhina, 2000Starukhina, , 2006Lawrence et al, 2006) but not established.…”

Section: Introductionmentioning

confidence: 99%

Global lunar-surface mapping experiment using the Lunar Imager/Spectrometer on SELENE

et al. 2008

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The Moon is the nearest celestial body to the Earth. Understanding the Moon is the most important issue confronting geosciences and planetary sciences. Japan will launch the lunar polar orbiter SELENE (Kaguya) (Kato et al., 2007) in 2007 as the first mission of the Japanese long-term lunar exploration program and acquire data for scientific knowledge and possible utilization of the Moon. An optical sensing instrument called the Lunar Imager/Spectrometer (LISM) is loaded on SELENE. The LISM requirements for the SELENE project are intended to provide high-resolution digital imagery and spectroscopic data for the entire lunar surface, acquiring these data for scientific knowledge and possible utilization of the Moon. Actually, LISM was designed to include three specialized sub-instruments: a terrain camera (TC), a multi-band imager (MI), and a spectral profiler (SP). The TC is a high-resolution stereo camera with 10-m spatial resolution from a SELENE nominal altitude of 100 km and a stereo angle of 30• to provide stereo pairs from which digital terrain models (DTMs) with a height resolution of 20 m or better will be produced. The MI is a multi-spectral imager with four and five color bands with 20 m and 60 m spatial resolution in visible and near-infrared ranges, which will provide data to be used to distinguish the geological units in detail. The SP is a line spectral profiler with a 400-m-wide footprint and 300 spectral bands with 6-8 nm spectral resolution in the visible to near-infrared ranges. The SP data will be sufficiently powerful to identify the lunar surface's mineral composition. Moreover, LISM will provide data with a spatial resolution, signal-to-noise ratio, and covered spectral range superior to that of past Earth-based and spacecraft-based observations. In addition to the hardware instrumentation, we have studied operation plans for global data acquisition within the limited total data volume allotment per day. Results show that the TC and MI can achieve global observations within the restrictions by sharing the TC and MI observation periods, adopting appropriate data compression, and executing necessary SELENE orbital plane change operations to ensure global coverage by MI. Pre-launch operation planning has resulted in possible global TC high-contrast imagery, TC stereoscopic imagery, and MI 9-band imagery in one nominal mission period. The SP will also acquire spectral line profiling data for nearly the entire lunar surface. The east-west interval of the SP strip data will be 3-4 km at the equator by the end of the mission and shorter at higher latitudes. We have proposed execution of SELENE roll cant operations three times during the nominal mission period to execute calibration site observations, and have reached agreement on this matter with the SELENE project. We present LISM global surface mapping experiments for instrumentation and operation plans. The ground processing systems and the data release plan for LISM data are discussed briefly.

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Polar regions of the moon as a potential repository of solar-wind-implanted gases

Cited by 67 publications

References 19 publications

Solar wind implantation into lunar regolith: Hydrogen retention in a surface with defects

Solar wind implantation into lunar regolith: Hydrogen retention in a surface with defects

Lunar 3He estimations and related parameters analyses

Global lunar-surface mapping experiment using the Lunar Imager/Spectrometer on SELENE

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