Additionally, the 950/560 and 950/730 nm image ratios were used to define the regions of mature mare soil in which the relation is valid. Spectral ratio images (400/560 and 400/730 nm) were used to map the abundance of TiO2 using the empirical relation found by Charlette et al from analysis of returned lunar soils. The effect is more significant as seen from orbiting spacecraft over a range of selenographic latitude. Consistent with previous studies, we find that the moon is 'bluer' at small phase angles, but that the effect on the ratio values for TiO2 abundance for the phase angles of our data is on the order of the measurement uncertainties throughout the range of abundances found in the mare. Groundbased telescopic CCD images of 36 selected locations on the moon were obtained in five 'standard' bandpasses at 12 phase angles ranging from -78 deg to +75 deg to measure phase function effects on the ratio values used to quantify the abundance of TiO2 and qualitatively indicate soil maturity. Lunar phase function effects on spectral ratios used for resource assessment The dominant components in the uncertainty budget are the uncertainty in the absolute TOA lunar irradiance and the uncertainty in the fit to the phase correction from the output of the ROLO model. The uncertainties in the empirically corrected output from the ROLO model are approximately 1 % from 440 nm to 865 nm and increase to almost 3 % at 412 nm. Combined with empirically derived phase and libration corrections to the output of the ROLO Model and uncertainty estimates in those corrections, the measurements enable development of a corrected TOA lunar irradiance model and its uncertainty budget for phase angles between +/-80° and libration angles from 7° to 51°. In this work, two recent absolute, low uncertainty, SI-traceable top-of-the-atmosphere (TOA) lunar irradiances, measured over the spectral range from 380 nm to 1040 nm, at lunar phase angles of 6.6° and 16.9°, are used as tie-points to the output of the ROLO Model.
While extremely successful as a relative exo-atmospheric calibration target, the ROLO Model is not SI-traceable and has estimated uncertainties too large for the Moon to be used as an absolute celestial calibration target. The lunar irradiance can be predicted from the modeled lunar reflectance using a spectrum of the incident solar irradiance. The United States Geological Survey (USGS) has developed an empirical model, known as the Robotic Lunar Observatory (ROLO) Model, that predicts the reflectance of the Moon for any Sun-sensor-Moon configuration over the spectral range from 350 nm to 2500 nm. We will summarize recent results of lunar surface from ground-based polarimetric observations and will briefly introduce the science rationals and operation concept of PolCam.Ībsolute, SI-traceable lunar irradiance tie-points for the USGS Lunar Modelīrown, Steven W.
(2) To obtain the reflectance ratios at 320 nm and 430 nm for the whole lunar surface with a spatial resolution of 80m. The science objectives are (1) To obtain the polarization data of the whole lunar surface at wavelengths of 430nm and 650nm for phase angle range from 0° to 120° with a spatial resolution of 80 m. Wide- Angle Polarimetric Camera (PolCam) is selected as one of the onboard instrument for KPLO. We plan to perform the polarimetry in lunar orbit through Korea Pathfinder Lunar Orbiter (KPLO), which will be launched around 2018/2019 as the first Korean lunar mission. However, a polarimetry toward the Moon in its orbit has not been performed. Wide- Angle Polarimetric Camera for Korea Pathfinder Lunar OrbiterĪ polarimetry data contains valuable information about the lunar surface such as the grain size and porosity of the regolith.
LUNAR CYCLE ESCAPE ROOM ANSWER KEY FULL
Since the solar wind flux decreases substantially when the Moon enters the Earth's magnetotail near full Moon, while the global solar photon flux is undiminished, we suggest that solar wind sputtering is the dominant process for sodium production. However, the sodium emission near full Moon falls below that which would be expected for solar photon-driven processes.
This suggests that the rate of sodium vapor production from the lunar surface is largest at the subsolar point and becomes small near the terminator. The emission intensity decreases from a maximum around first quarter ( phase angle 90 deg) to very small values near full Moon ( phase angle 0 deg). These data show a strong dependence on lunar phase. We report new measurements of the sodium emission intensity seen in a line of sight just above the surface of the Moon. Variation of lunar sodium emission intensity with phase angle
0 kommentar(er)
