Deflection of the vertical and refraction in three-dimensional adjustment of terrestrial networks

Summary In this paper statistical tests are exploited in order to verify the hypotheses about the refraction and the deflection of the vertical pertaining to a geometrical model for the three-dimensional adjustment of terrestrial networks. The deflections of the vertical and the refraction coefficients can be assumed either as unknowns or fixed input data, at some or all the points of the network. The geometrical model, reported in the appendix for convenience, assumes as observables the slant distances, zenith and horizontal angles, without any reduction neither to the marks on the ground nor to the surface of reference. Further, the observation equations are derived and linearized in terms of Cartesian coordinates in Geocentric or Topocentric system; direction cosines of the vertical and of the ellipsoidal normal are adopted as the relevant direction parameters. Finally, an application to a network from Hradilek (1984), performed under different assumptions about the unknowns and the corrections of the angular observations due to the deflections of the vertical, shows the effectiveness of the proposed approach.     

Measurements of solar occulation: the error in a naive retrieval if the constituent's concentration changes

The stratospheric concentrations of many minor constituents change rapidly at sunrise or sunset. If this happens, there is an inherent error when retrieving the vertical profiles of the constituents from measurements of their absorption of sunlight. For retrievals of NO at sunset the error can be estimated from in-situ measurements alone, without appeal to a model of stratospheric photochemistry. Below 20 km this error can approach 100% so that the retrieved NO is zero. But at 40 km, and at 25 km when the absorption is strong and Lorentzian, it can be less than 20%. Precise calculations of the error, even if small, require model calculations of the sunset and sunrise changes. With a model, we have calculated the error for NO, NO₂, OH and ClO.     

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Search for Spatial Variability in the Solar Acoustic Spectrum

Motivated by the various examples of spatial variability in the power of the acoustic spectrum, we attempted to look for spatial variability in the peak frequency of the spectrum. However, the determination of this peak frequency on a spatial scale of a single pixel (8 arc sec for the GONG data) is limited by the stochastic variations in the power spectrum presumably caused by the stochastic nature of the excitation process. Averaging over a large number of spectra (100 spectra from a 10 × 10 pixel area) produced stabler spectra. The peak frequencies of 130 such locations were found to be distributed with a FWHM of about 130 Hz. A map of the spatial variation of this peak frequency did not show any strong feature with statistically significant deviation from the mean of the distribution. Likewise, the scatter in the peak frequencies masked the detection of magnetic-field-induced changes in the peak frequency. On a much larger scale, the N latitudes showed a slightly lower value of the peak frequency as compared to the S latitudes, although the difference (25 Hz) is barely larger than the r.m.s. spread (20 Hz).