Abstract

Among different stellar types, low-mass dwarfs, in particular late-K and M dwarf, are the most abundant stars in our Galaxy, and can be used to probe the structure and chemodynamical evolution of the Milky Way. In addition, due to the slow fusion process in their interiors, the main-sequence lifetime of these cool dwarfs is much longer than the current age of the Universe. As a result, their atmospheric abundances are pristine indicators of the chemical properties of the progenitor molecular clouds. Moreover, cool dwarfs have increasingly become attractive targets as planet host candidates, because widely used methods in detecting exoplanets are more sensitive to planets orbiting low-mass stars. In this talk, I will present some studies of Galactic chemical properties using spectroscopic analysis of cool dwarfs and the related challenges. Some Galactic chemical evolution models are also shown to compare with observations. I will further discuss the chemical link between planets and their host stars, which could provide crucial insight into planet formation. Recently, JWST has started measuring exoplanet chemical abundances with high precision. The accurate abundance measurement of JWST cool host stars has therefore been my main goal to search for planet-star connections.