Abstract
Low noise, high resolution spectral scans have been obtained for the resonance lines of silver λ3280.7 and λ3382.9, observed at the centre of the solar disk. A double pass-monochromator is used in conjunction with the Snow telescope at Mount Wilson; the transparency of the sky is monitored during the observations in order to achieve required accuracy. The data are analyzed by the method of spectral synthesis wherein we employ a model atmosphere resembling Elste's (1968) model and checked by limb-darkening observations. The present kinematical model adopts a macroturbulent velocity of 2.2 km s−1 and no microturbulence. With this model line profiles can be reproduced without invoking implausibly large collisional damping constants.
The silver abundance turns out to be {Ag}=log[N(Ag)/N(H)]+12;=0.85, a factor of four under the value found from the Type I carbonaceous chondrites.
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Ross, J.E., Aller, L.H. The solar abundance of silver. Sol Phys 25, 30–43 (1972). https://doi.org/10.1007/BF00155742
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DOI: https://doi.org/10.1007/BF00155742