Abstract
Abstract Magnetic fields are a critical component of interior and atmospheric models of low-mass stars. Additionally, stellar activity associated with magnetic fields may make exoplanets around K and M stars uninhabitable. Here we describe the measurement of the magnetic fields of K and M dwarfs from high-resolution spectra, and discuss the impact of projected rotational velocity (v sin i) on these measurements. We determine the magnetic fields by measuring the Zeeman effect on Na, Ti, and Ca spectral lines. Observed spectra in our analysis come from the Immersion GRating INfrared Spectrometer (IGRINS), while synthetic spectra were created using the MoogStokes software along with MARCS atmosphere models. We found that measuring Zeeman splitting in R ∼ 45,000 spectra is limited primarily by the projected rotational velocity of the star, but also by spectral resolution, line strength, and spectral signal-to-noise.
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