[astro-ph.SR] There are exceedingly few chemical abundance measurements available in the literature for K dwarf stars, especially for those with Teff< 4700 K due to an incompatibility of traditional analyses […]
![Plots of the observed, high signal-to-noise H (top panel) band IGRINS spectra used in this abundance analysis. Oxygen abundances are determined from OH lines located in the H band (1.45–1.80 microns) while carbon, 12C/ 13C, and 16O/ 18O abundances are derived from various CO isotopologue lines located in the 2.3-2.45 micron region of the K band (1.95–2.45 microns). -- [astro-ph.SR]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/11/Expanding.png?resize=1200%2C721&ssl=1)
[astro-ph.SR] There are exceedingly few chemical abundance measurements available in the literature for K dwarf stars, especially for those with Teff< 4700 K due to an incompatibility of traditional analyses […]