2015/09/11 by Thomas E. Harrison, T. E. Harrison, Ryan T. Hamilton · 10 citations
Chemistry · Physics and Astronomy · #Analytical Chemistry (journal) #Astronomy #Astronomy and Astrophysical Research #Astrophysics #Astrophysics and Star Formation Studies #Carbon fibers #Carbon star #Chemistry #Emission spectrum #Environmental chemistry #Materials science #Physics #Resolution (logic) #Spectral line #Stars #Stellar, planetary, and galactic studies #astro-ph.SR
paper · pdf · doi:10.1088/0004-6256/150/5/142
published in The Astronomical Journal 150(5), 142 (Institute of Physics) · Accepted in the Astronomical Journal
arxiv created 2015/09/11 · openalex publication_date 2015/10/08 · arxiv updated 2015/10/14 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/06
We use a modified version of MOOG to generate large grids of synthetic spectra in an attempt to derive quantitative abundances for three CVs (GK Per, RU Peg, and SS Cyg) by comparing the models to moderate resolution ( R ∼ 25,000) K -band spectra obtained with NIRSPEC on Keck. For each of the three systems we find solar, or slightly sub-solar values for [Fe/H], but significant deficits of carbon: for SS Cyg we find [C/Fe] = −0.50, for RU Peg [C/Fe] = −0.75, and for GK Per [C/Fe] = −1.00. We show that it is possible to use lower resolution ( R ∼ 2000) spectra to quantify carbon deficits. We examine realistic veiling scenarios and find that emission from H i or CO cannot reproduce the observations.