Solar errors

To summarize, Tifft s original claims have been strongly and independently substantiated by the Napier-Guthrie analysis this latter analysis has appeared in the mainstream literature and stands increasingly secure as Hipparchus observations continue to tighten the solar error box. Any serious thought about these two effects soon convinces one that the implications for cosmology are profound—and very difficult to comprehend. 

We present here the results of abundance measurements of iron, calcium and nickel in four open clusters, from UVES spectra of solar type stars. A code developed by one of the authors (Francois) performs line recognization, equivalent width measurements and finally obtains the abundances by means of OSMARCS LTE model atmosphere [4]. Temperature, gravity and microturbulence velocity have to be input to the program. This is made in an automatic way for a grid of values chosen on photometric basis. Those that best reproduce excitation and ionization equilibria are selected and used, namely when no significant trend of the computed abundances is seen, neither versus the excitation potential of the line nor versus its equivalent width, and for which the abundances obtained with lines of different ionization stages of the same specie give equal results within the errors. This check is made with iron lines, we have in fact at least thirty Fe I lines in each star, and six Fell lines. 

Fig. 3.42. Depletion below solar abundances of elements in the H I gas towards f Ophiuchi plotted against atomic mass number in (a) and condensation temperature in (b), based in part on the curve of growth shown in Fig. 3.11. Vertical boxes indicate error bars. The dotted curve in the left panel represents an A-1/2 dependence expected for non-equilibrium accretion of gas on to grains in the ISM. The condensation temperature gives a somewhat better, though not perfect, fit, suggesting condensation under near-equilibrium conditions at a variety of temperatures either in stellar ejecta or in some nebular environment. Note the extreme depletion of Ca ( Calcium in the plane stays mainly in the grain ). After Spitzer and Jenkins (1975). Copyright by Annual Reviews, Inc.

Fig. 6.7. r-process abundances in the Solar System. Filled circles represent r-only nuclides, while open circles with error bars show the result of subtraction of a calculated s-process contribution. After Kappeler, Beer and Wisshak (1989). Copyright by IOP Publishing Ltd. Courtesy Franz Kappeler. 

Fig. 12.14. Metallicity evolution in DLAs. Curves show predicted mean metallic-ity in the interstellar gas relative to solar predicted by chemical evolution models of Pei, Fall and Hauser (1999), Pei and Fall (1995), Malaney and Chaboyer (1996) and Somerville, Primack and Faber (2001) respectively. Data points giving column-density weighted metallicities based on zinc only (filled circles) or other elements (open circles) are plotted in the upper panel taking upper limits as detections and in the lower panel taking upper limits as zeros. Horizontal error bars show the redshift bins adopted. After Kulkarni et al. (2005).

For Solar-System 232Th, 238U, A — (r) = 3.2 Gyr. The error from uncertainties in In K is of order 10 per cent, and that from neglecting the quadratic term in Eq. (10.33) is also of order 10 per cent, but is systematic in the sense that the 3.2 Gyr is an overestimate by about that amount. 

Fig. 8.2. Iron content as a function of the age of stars in the neighbourhood of the Solar System (age-metallicity relation). Age determinations are a dehcate matter and somewhat uncertain. This explains the wide error bars and scatter of the data. Type la supernovas must be included to reproduce the observed iron evolution.

Oxygen isotopic compositions of presolar oxide grains compared with those of red giant stars. Stellar data are shown without error bars, which are large on this scale. Both data sets are characterized by higher 170/160 ratios and lower 180/160 ratios compared to solar oxygen. Stellar data from Smith and Lambert (1990). 

Bais A.F, S. Kazadzis, D.S. Balis, C. S. Zerefos and M. Blumthaler, 0 Correcting global solar UV spectra recorded by a Brewer spectroradiometer for its angular response error, Applied Optics, 37, 6339-6344. 

The variation of solar zenith angle during a spectral measurement may introduce errors in the determination of the calibration factor by altering the shape of the spectrum. This problem can be partly overcome by performing the measurements preferably near the local noon, when the change of solar zenith angle with time is much... 

Bais A. F. (1997) Spectrometers Operational errors and uncertainties, in C. S. Zerefos and A. F. Bais (eds,), Solar Ultraviolet Radiation Modelling, Measurements and Effects, NATO AS1 Series, Series 1 Global Environmental Change, Springer-Verlag, VoL 52, pp. 163-173. 

Figure 2. CIO volume mixing ratio profiles across the vortex edge as measured by the ASUR instrument (solid line) on March 6, 1996, compared to results of the SI.IMCAT 3-D model (dashed line, rectangles) for identical positions at 12 UT. Also indicated are average times, positions, solar zenith angles, and 475 K-PV s for the individual measurements. The thick error bars represent the relevant statistical errors due to measurement noise, the thin dotted error bars include also the error due to the limited altitude resolution (the so-called null-space error). Modelled and measured data are in relatively good agreement inside, at the edge, and outside the Arctic polar vortex.

Subsequent to this initial publication, the satellite Hipparchus has been launched, which has resulted in very refined conventional determinations of the solar vector error box concurrently, Napier has reversed the Napier-Guthrie analysis, assuming the prior existence of the 37.6-km/s effect using it to obtain independent determinations of the solar vector error box. These lie wholly inside the Hipparchus error box determinations. 

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