Experiment 6 The Surface Roughness of the Moon. Reflection and Scattering from a Planetary Surface: Part I. Surface Materials

2012 ◽  
pp. 105-128
Author(s):  
Leslie M. Golden
Keyword(s):  
Surface Roughness ◽  
Planetary Surface ◽  
The Moon ◽  
Surface Part ◽  
Surface Materials

Thermophysical model of the Moon from 3.7 to 15 μm

2020 ◽  
Author(s):  
Thomas G. Müller ◽  
Martin J. Burgdorf ◽  
Stefan A. Buehler ◽  
Marc Prange
Keyword(s):  
Surface Roughness ◽  
Wavelength Range ◽  
Thermal Flux ◽  
Field Of View ◽  
Spectral Energy ◽  
The Moon ◽  
Mid Infrared ◽  
Thermophysical Model ◽  
Wide Range ◽  
Model Fits

<p>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°.<br />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.</p> <p>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.</p> <p>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.</p> <p>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).</p> <p><br />References:<br />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.</p> <p> </p>

The influence of surface roughness on volatile transport on the Moon

Icarus ◽  
2018 ◽  
Vol 299 ◽  
pp. 31-45 ◽  
Author(s):  
P. Prem ◽  
D.B. Goldstein ◽  
P.L. Varghese ◽  
L.M. Trafton
Keyword(s):  
Surface Roughness ◽  
The Moon ◽  
Volatile Transport

Experimental system for the study of planetary surface materials' BRDF

2000 ◽  
Vol 19 (1-4) ◽  
pp. 59-74 ◽  
Author(s):  
Nicolas Bonnefoy ◽  
Olivier Brissaud ◽  
Bernard Schmitt ◽  
Sylvain Douté ◽  
Michel Fily ◽  
...  
Keyword(s):  
Experimental System ◽  
Planetary Surface ◽  
Surface Materials

scholarly journals Sintering and Microstructures of SUS 316L Powder Produced by 3D Printing Process

2017 ◽  
Vol 62 (2) ◽  
pp. 1215-1218 ◽  
Author(s):  
W.J. Kim ◽  
H.-H. Nguyen ◽  
H.Y. Kim ◽  
M.-T. Nguyen ◽  
H.S. Park ◽  
...  
Keyword(s):  
Surface Roughness ◽  
3D Printing ◽  
Selective Laser Sintering ◽  
High Porosity ◽  
Ceramic Powders ◽  
Spherical Type ◽  
Spherical Powder ◽  
Surface Part ◽  
Metal Polymer ◽  
Type Sample

AbstractSelective laser sintering (SLS) is a type of laminating sintering technique, using CO2laser with (metal, polymer, and ceramic) powders. In this result, the flake SUS 316L was used to achieve a high porous product, and compare to spherical type. After SLS, the porosity of flake-type sample with 34% was quite higher than that of the spherical-type one that had only 11%. The surface roughness of the flake SLS sample were also investigated in both inner and surface parts. The results show that the deviation of the roughness of the surface part is about 64.40μm, while that of the internal one was about 117.65μm, which presents the containing of high porosity in the uneven surfaces. With the process using spherical powder, the sample was quite dense, however, some initial particles still remained as a result of less energy received at the beneath of the processing layer.

scholarly journals Penetrometry of granular and moist planetary surface materials: Application to the Huygens landing site on Titan

Icarus ◽  
2010 ◽  
Vol 210 (2) ◽  
pp. 843-851 ◽  
Author(s):  
Karl R. Atkinson ◽  
John C. Zarnecki ◽  
Martin C. Towner ◽  
Timothy J. Ringrose ◽  
Axel Hagermann ◽  
...  
Keyword(s):  
Landing Site ◽  
Planetary Surface ◽  
Surface Materials

A discussion on infared astronomy - Mid-infrared spectroscopic observations of the Moon

1969 ◽  
Vol 264 (1150) ◽  
pp. 109-139 ◽  
Keyword(s):  
Remote Sensing ◽  
Lunar Surface ◽  
Wavelength Region ◽  
Landing Site ◽  
Ground Truth ◽  
Molecular Vibration ◽  
The Moon ◽  
Mid Infrared ◽  
Surface Materials ◽  
Remote Sensing Techniques

Now that space probes have actually landed on the Moon, and man is soon to follow, one might suppose that the need for the development of lunar remote sensing techniques is past. Exactly the opposite is true. It must be remembered that no nation is financially able to support exploration of more than a very small percentage of the total surface area of the moon. Small areas immediately adjacent to a landing site will, of course, be explored in detail. Hopefully, there will be a few traverses made to discover the degree of lateral inhomogeneity of the surface materials. Realistically, however, we must plan on extending this ‘ground truth’ information to cover the entire lunar surface by remote means. In fact, remote sensing techniques will be employed prior to much of the detailed lunar surface exploration in order to define areas of maximum interest. The mid-infrared region of the spectrum is a wavelength region which possesses a high potential usefulness for remote sensing, because the molecular vibration spectra in this region are directly interpretable in terms of molecular composition. It is the purpose of this paper to examine this potential, review the theoretical justification for use of this wavelength region, describe laboratory studies of possible lunar surface materials, and present the data so far obtained from the moon itself.

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