BOOK REVIEWS overcoming possible notational barriers. No solutions of specialized technical problems are presented. Instead, the essentials of the theory are developed, beginning with tensor analysis, elements of potential theory, then moving to kinematics, dynamics, and the constitutive relation in linear elasticity, at each stage giving rigorous proofs for a large body of relevant assertions. Then a long chapter in elastostatics and another in elastodynamics complete this work which can serve as an excellent text for applied mathematicians interested in elasticity, and as a solid reference book with an extensive list of references for the practitioners. Linear Thermoelasticity by Donald E. Carlson; pp. 297-345 (reviewed by S.N.-N.). This part follows the style of the previous article, giving fundamentals in thermoelasticity, again avoiding solutions to technical problems. It is less ambitious than Gurtin's article, but scholarly done. While this reviewer finds it a welcome addition to the literature, he feels that the use of the questionable Clausius-Duhem inequality in the unquestionable classical theory of thermoelasticity is unnecessary. Existence Theorems in Elasticity and Boundary-Value Problems of Elasticity With Unilateral Constraints by Gaetano Fichera; pp. 347-424 (reviewed by W.E.O.). These two articles are recommended to those who have a good background in modern mathematical analysis. A substantial portion of the first article is devoted to key theorems on the existence and uniqueness of solutions to linear boundary-value problems involving strongly elliptic operators. Applications of these results are given for some classical problems in linear elasticity with bilateral constraints. The second article extends the analysis of the first article so as to treat problems with unilateral (i.e., inequality) constraints. General results are developed for the abstract unilateral problem in cases of both symmetric and nonsymmetric operators. Applications of these results include the famous Signorini Problem.

Context. Our ability to extract information from the spectra of stars depends on reliable models of stellar atmospheres and appropriate techniques for spectral synthesis. Various model codes and strategies for the analysis of stellar spectra are available today. Aims. We aim to compare the results of deriving stellar parameters using different atmosphere models and different analysis strategies. The focus is set on high-resolution spectroscopy of cool giant stars. Methods. Spectra representing four cool giant stars were made available to various groups and individuals working in the area of spectral synthesis, asking them to derive stellar parameters from the data provided. The results were discussed at a workshop in Vienna in 2010. Most of the major codes currently used in the astronomical community for analyses of stellar spectra were included in this experiment.Results. We present the results from the different groups, as well as an additional experiment comparing the synthetic spectra produced by various codes for a given set of stellar parameters. Similarities and differences of the results are discussed. Conclusions.Several valid approaches to analyze a given spectrum of a star result in quite a wide range of solutions. The main causes for the differences in parameters derived by different groups seem to lie in the physical input data and in the details of the analysis method. This clearly shows how far from a definitive abundance analysis we still are.Key words. stars: atmospheres -stars: late-type -stars: abundances -stars: fundamental parameters Based on observations obtained at the Bernard Lyot Telescope (TBL, Pic du Midi, France) of the Midi-Pyrénées Observatory, which is operated by the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique of France.Tables 6-11 are only available in electronic form at http://www.aanda.orgThe spectra of stars 1 to 4 used in the experiment presented here are only availalbe at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via

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