Baseline Terrestrial Experiments

The data in Table VI are currently taken as the strongest evidence for the existence of neutrino oscillations. Despite having been observed in two independent atmospheric neutrino experiments—K-II and SuperK—a need 

A linear array of the original Kamiokande-style detectors, arranged on a long baseline (50-100 km), might also track the sinusoidal dependence on distance of the flavor content of a v beam. This disappearance experiment would bypass the difficult problem of devising a Vj detector for the Fermilab and CERN experiments and would still serve the equivalent purpose of demonstrating neutrino oscillations conclusively. 

The observations of extraterrestrial neutrinos from the sun by different experimental methods have confirmed the details of the nuclear processes in the core of the sun and have verified its internal structure and method of energy generation. Moreover, the neutrinos from the earth s atmosphere and from the sun appear to exhibit the phenomenon of neutrino oscillations which, if fully verified, will conclusively demonstrate that at least one of the neutrinos in the current model of elementary leptons has nonzero mass and that at least two of them can spontaneously exchange flavor. 

Neutrinos observed from the supernova SN1987A, approximately 55 kiloparsecs from earth, have quantitatively confirmed the current description of type II supernovae and the particle physics and astrophysics principles on which the description is based. 

Together, these detailed observations have established experimental neutrino astronomy, or, perhaps more appropriately, neutrino astrophysies, as a source of fundamental information relating to the internal structure and behavior of stars. As more powerfiil neutrino detectors become available and permit observation of other neutrino radiation from the sky, we expect that neutrino astronomy wiU be an increasingly valuable adjunct of the older astronomy employing electromagnetic radiation as its means of observation. 

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Tucker et al demonstrated the applicability of LIBS to bulk elemental analysis of igneous rock powders. The LIBS spectra were modelled using PLS to predict major element compositions. Multiple calibration sets relevant to different rock types were preferred over a single all-encompassing calibration set. Baseline removal and transforming spectral data by their first derivative did not improve predictions and may even have negative effects. These results are directly applicable to spectra that will be acquired by the ChemCam experiment on Mars Science Laboratory, but also to terrestrial LIBS applications. 

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