Measuring Elemental Abundances in Metal-Poor Stars
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Date
2020-12
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Publisher
The Ohio State University
Abstract
By analyzing the elemental abundance profile of a star, insight can be gained into the composition of its initial dust cloud. Using this insight, it is possible to determine the likelihood that the star was able to form planets based on the amount of metal material available. We present an analysis of 16 dwarf stars in the galactic halo, a relatively metal-poor region when compared to the thin disk, where most currently known exoplanets reside. We calculated detailed elemental abundance profiles for each of these stars and found their metallicities to be in the range expected for halo stars (-2.0 < [Fe/H] < -0.5). In this process, we also determined the values of the effective temperature and surface gravity for each star.
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Keywords
Stars, Spectroscopy, Galactic Halo, Exoplanets