Thermal Characteristics of Apollo 16 Lunar Fines

Cremers, C. J.; Hsia, H. S.; Birkebak, R. C.

doi:10.1615/ihtc5.1240

Cited by 18 publications

(17 citation statements)

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“…Figure 3), so it is reasonable to assume that variations in bulk density and composition do not (Robie et al, 1970) from Apollo missions fit to the Diviner model (which uses Ledlow et al, 1992) and to the best third-order polynomial fits. (b) Thermal conductivity measurements of regolith (Cremers & Hsia, 1974) fit to Watson's equation (Vasavada et al, 1999;Watson, 1964).…”

Section: Lunar Regolith Simulantsmentioning

confidence: 99%

“…Due to the entanglement of the effects of physical properties of regolith (petrologic modes, particle heterogeneity, particle size and shape, etc.) on thermal conductivity, fitting lunar data to equation ( 30) is nontrivial (e.g., Cremers et al, 1971aCremers et al, , 1971bCremers, 1975;Cremers & Hsia, 1973, 1974. Driven by a motivation to understand the effect of bulk density on thermal conductivity, we develop a model based on a well-tested lunar simulant, namely particulate basalt.…”

Section: With Valuesmentioning

confidence: 99%

“…The thermal properties of the fine, particulate components of lunar regolith are well understood for temperatures within the range of ~150-400 K. Extensive laboratory tests, in particular, temperature-dependent thermal conductivity and specific heat measurements, have been performed on lunar samples collected from the Apollo and Luna missions (e.g., Cremers et al, 1971aCremers et al, , 1971bCremers, 1975;Cremers & Hsia, 1973, 1974Hemingway et al, 1973;Horai & Fujii, 1972;Horai et al, 1970). Additionally, due to the limited availability of lunar samples, simulant materials have been studied in-depth to better understand thermal transport and characteristics of the lunar regolith (e.g., Fountain & West, 1970).…”

Section: Introductionmentioning

confidence: 99%

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A Model for the Thermophysical Properties of Lunar Regolith at Low Temperatures

2019

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The thermophysical properties of lunar regolith have been thoroughly investigated for temperatures higher than 100 K. For the near‐equatorial thermal measurements of the Apollo era, this temperature range was sufficient to generate appropriate models. However, recent measurements from the Lunar Reconnaissance Orbiter Diviner Lunar Radiometer Experiment have revealed polar temperatures as low as 20 K, with apparently lower thermal inertia than explainable by existing theory. In the absence of comprehensive laboratory measurements of regolith thermal properties at low temperatures (<100 K), we investigate solid state theory and fits to lunar simulant materials to derive a semiempirical model of specific heat and thermal conductivity in lunar regolith in the full range 20–400 K. The primary distinctions between these previous models are (1) the temperature dependence of the solid conduction component of thermal conductivity at low temperatures, (2) the focus on regolith bulk density as the primary variable, and (3) the concept that the composition and modal petrology of grains could significantly influence thermal properties of the bulk regolith. This model predicts that at low temperatures, thermal conductivity is as much as an order of magnitude lower and specific heat is likely higher than expected from current models. The thermal conductivity at low temperature should vary depending on the constituent grain materials, their crystallinity, contributions from phonon scattering modes, bulk porosity, and density. To demonstrate the impact of our finding, we extrapolate the effects of our conductivity model on temperature variations in permanently shadowed regions on the Moon. This work motivates experimental confirmation of thermophysical properties of lunar regolith at low temperature.

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Section: Lunar Regolith Simulantsmentioning

confidence: 99%

Section: With Valuesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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A Model for the Thermophysical Properties of Lunar Regolith at Low Temperatures

2019

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“…The model was used to fit the measured surface temperatures as a function of the density, specific heat, and thermal conductivity, assumed similar to those of a lunar regolith (9)(10)(11). A self-heating parameter (12) accounts for the contribution of unresolved topography and microroughness.…”

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confidence: 99%

The Surface Composition and Temperature of Asteroid 21 Lutetia As Observed by Rosetta/VIRTIS

Coradini¹,

Capaccioni²,

Erard³

et al. 2011

Science

116

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The Visible, InfraRed, and Thermal Imaging Spectrometer (VIRTIS) on Rosetta obtained hyperspectral images, spectral reflectance maps, and temperature maps of the asteroid 21 Lutetia. No absorption features, of either silicates or hydrated minerals, have been detected across the observed area in the spectral range from 0.4 to 3.5 micrometers. The surface temperature reaches a maximum value of 245 kelvin and correlates well with topographic features. The thermal inertia is in the range from 20 to 30 joules meter(-2) kelvin(-1) second(-0.5), comparable to a lunarlike powdery regolith. Spectral signatures of surface alteration, resulting from space weathering, seem to be missing. Lutetia is likely a remnant of the primordial planetesimal population, unaltered by differentiation processes and composed of chondritic materials of enstatitic or carbonaceous origin, dominated by iron-poor minerals that have not suffered aqueous alteration.

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“…Thermal conductivity of ice‐free, porous materials are reviewed by Schotte [1960], Dul ' nev and Sigalova [1967], Wechsler et al [1972], Jakosky [1986], Tsotsas and Martin [1987], Presley and Christensen [1997a], and Carson et al [2005]. Measurements of dry particulate thermal conductivity have been conducted for industrial applications [e.g., Smoluchowski , 1910], and in association with the Apollo lunar program [e.g., Wechsler and Glaser , 1965; Fountain and West , 1970; Cremers , 1971; Cremers and Hsia , 1974]. More recent experiments have been carried out in a CO 2 atmosphere in the Martian atmospheric pressure regime [ Presley and Christensen , 1997b; Presley and Craddock , 2006; Presley and Christensen , 2010].…”

Section: Introductionmentioning

confidence: 99%

Measurements of thermal properties of icy Mars regolith analogs

et al. 2012

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[1] In a series of laboratory experiments, we measure thermal diffusivity, thermal conductivity, and heat capacity of icy regolith created by vapor deposition of water below its triple point and in a low pressure atmosphere. We find that an ice-regolith mixture prepared in this manner, which may be common on Mars, and potentially also present on the Moon, Mercury, comets and other bodies, has a thermal conductivity that increases approximately linearly with ice content. This trend differs substantially from thermal property models based of preferential formation of ice at grain contacts previously applied to both terrestrial and non-terrestrial subsurface ice. We describe the observed microphysical structure of ice responsible for these thermal properties, which displaces interstitial gases, traps bubbles, exhibits anisotropic growth, and bridges non-neighboring grains. We also consider the applicability of these measurements to subsurface ice on Mars and other solar system bodies.

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Thermal Characteristics of Apollo 16 Lunar Fines

Cited by 18 publications

References 0 publications

A Model for the Thermophysical Properties of Lunar Regolith at Low Temperatures

A Model for the Thermophysical Properties of Lunar Regolith at Low Temperatures

The Surface Composition and Temperature of Asteroid 21 Lutetia As Observed by Rosetta/VIRTIS

Measurements of thermal properties of icy Mars regolith analogs

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