The focus is set on high-resolution spectroscopy of cool giant stars. We aim to compare the results of deriving stellar parameters using different atmosphere models and different analysis strategies. Various model codes and strategies for the analysis of stellar spectra are available today.Īims. Our ability to extract information from the spectra of stars depends on reliable models of stellar atmospheres and appropriate techniques for spectral synthesis. SIfA, School of Physics, University of Sydney,Ĭontext. Institute of Astronomy, The University of Tokyo,Ĭentro de Astrobiología (INTA-CSIC), LAEFF Campus, European SpaceĪstronomy Department, Ohio State University,Īustralian Astronomical Observatory, PO Box 296, Epping, NSW Zentrum für Astronomie der Universität Heidelberg (ZAH), Institutįür Theoretische Astrophysik, Albert Ueberle-Str. Indian Institute of Astrophysics, Koramangala, Bangalore, Indiaĭepartment of Physics, Catholic University of INAF – OAPD, Vicolo dell’Osservatorio 5, 35122 Goddard Space Flight Center, NASA, Greenbelt Laboratoire Univers et Particules de Montpellier, Universitéĭepartment of Astronomy & Physics, Saint Mary’s Université de Nice Sophia Antipolis, CNRS (UMR 6202), ObservatoireĪstrophysical Advances/UCOLick, 607 Marion Pl, Palo Alto, CA Física Teórica y del Cosmos, Universidad deĭepartment of Physics and Astronomy, MacquarieĪrgelander Institute for Astronomy, University of University of Vienna, Türkenschanzstrasse 17, 1180Į-mail: of Physics and Astronomy, Uppsalaĭepto. Astronomical objects: linking to databases.Including author names using non-Roman alphabets.Suggested resources for more tips on language editing in the sciences Punctuation and style concerns regarding equations, figures, tables, and footnotes
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