Moon spectrum

The reflection spectrum of the atmosphere is a measure of the albedo of the planet (Figure 10.4) and, despite the strong methane absorption in the red, Titan s disc looks orange principally due to scatter from the surface of dense methane-hydrocarbon clouds. Scatter from aerosol particles within the thick clouds obscures the surface of the moon although the radar analysis reveals considerable Chapman layer structure within the atmosphere and some interesting surface features. 

Purchase some rainbow" glasses from a nature, toy, or hobby store. The lenses of these glasses are diffraction gratings. Looking through them, you will see lig ht separated into its color components. Certain light sources, such as the moon or a car s headlights, are separated into a continuous spectrum—in other words, all the colors of the rainbow appear in a continuous sequence from red to violet. 

The ultimate objective of remote reflectance spectral measurements is to obtain quantitative estimates of the modal mineralogy of unexplored surfaces of the Moon and, indeed, other terrestrial planets. This necessitates difficult and elaborate spectrum-curve fitting procedures, which has been the focus of detailed research (e.g., Roush and Singer, 1986 Clouds et al., 1986 Mustard... 

The contrasting temperature-induced shifts of the pyroxene 1 and 2 pm bands could lead to erroneous estimates of the composition and, to a lesser extent, structure-type of a pyroxene-bearing mineral assemblage deduced from the remote-sensed reflectance spectrum of a hot or cold planetary surface if room-temperature determinative curves, such as that shown in fig. 10.5, are used uncritically. For example, remote-sensed spectra of planets with hot surfaces, such as Mercury and the Moon, would lead to overestimates of Fe2+ contents of the orthopyroxenes and underestimated Fe2+ contents of the clinopyroxenes (Singer and Roush, 1985). Planets with cold surfaces, such as Mars and the asteroids, could produce opposite results. On the other hand, the room-temperature data underlying the pyroxene determinative curve shown in fig. 10.5 may impose constraints on the compositions of pyroxenes deduced from telescopic spectra of a planet with very high surface temperatures, such as Mercury. 

Yoon D, Moon H, Cheong H, Choi JS, Choi JA, Park BH (2009) Variations in the Raman spectrum as a function of the number of graphene layers. J Korean Phys Soc 55 1299-1303... 

It may be mentioned here that this decade probably will see the soft lunar landing of an atomic absorption spectroscope (M8) intended to analyze surface material of the moon and relay signals back to earth. The system makes use of a solar furnace for sample vaporization and depends on the sun s spectrum as a light source. 

In 1896 he made the first quantitative link between changes in carbon dioxide concentration and climate. He calculated the absorption coefficients of carbon dioxide and water based on the emission spectrum of the moon, and he also calculated the amount of total heat absorption and corresponding temperature change in the atmosphere for various concentrations of carbon dioxide. His prediction of a doubling of carbon dioxide from a temperate rise of 5-6°C is close to modern pre-... 

The original CLEAN algorithm was invented to deconvolve effectively the Fourier spectrum from the PSF. In radio astronomy it was either impossible or impractical to arrange detectors on a regularly spaced grid due to malfunctioning of the part of equipment, occultations caused by the Moon, or if telescopes were operating over a... 

An interesting example of the use of ESCA is the nondestructive identification of elements on the lunar surface. The Surveyor was an unmanned probe that landed on the surface of the moon. The lunar soil was exposed to magnesium K radiation and the ESCA spectrum collected. The elemental components of the soil can be clearly identified... 

The only way scientists know that the Sun is mostly hydrogen is from experiments performed here on Earth. Each element in the periodic table has a distinct signature, called its spectrum. Electrons do not stick to the nuclei in atoms, but surround the core in a fashion that scientists have modeled variously as orbits, clouds, and probability densities. More detail will unfold later in this chapter, but for the moment, the model of an atom to be pictured is that of an electron orbiting the nucleus like the Moon orbits Earth. 

Tidal forces exerted by the attraction of the moon and the sun (and to a minor extent by the planets) on the earth s body produce a wide spectrum of geodynamic phenomena, from primary luni-solar attractional effects to secondary induced effects like solid earth and ocean tides, and third order ocean loading effects. Since these phenomena affect precise geodetic observations and make them time-dependent it is necessary to reduce time-variable geodetic observables and derived quantities in order to correspond to a quasinstationary, time—invariant state. 

Fig. 18.27 The Ar/ Af dates of small particles of impact-melt glass in lunar meteorites collected in Antarctica and in the Saheua Desert of Libya indicate the frequency of explosive impctcts of meteoroids or asteroids on the Moon. The results derived from these samples yield a spectrum of dates ranging from >1.8 to <4.2 billion years. The low abundances of dates older than 3.4 billion years implies that some glass particles older than about 3.4 billion years were destroyed by more recent impacts on the Moon. The Ar/ Ar dates shown here were measured by Cohen et al. (2005)...

---