Measuring the Spot Variability of T Tauri Stars Using Near-IR Atomic Fe and Molecular OH Lines

Abstract

As part of the Young Exoplanets Spectroscopic Survey (YESS), this study explores the spot variability of 13 T Tauri Stars (TTSs) in the near-infrared $H$ band, using spectra from the Immersion GRating INfrared Spectrometer (IGRINS). By analyzing effective temperature ($T_{\rm eff}$) sensitive lines of atomic FeI at ~1.56259 um and ~1.56362 um, and molecular OH at ~1.56310 um and ~1.56317 um, we develop an empirical equivalent width ratio (EWR) relationship for $T_{\rm eff}$ in the range of 3400-5000 K. This relationship allows for precise relative $T_{\rm eff}$ estimates to within tens of Kelvin and demonstrates compatibility with solar metallicity target models. However, discrepancies between observational data and model predictions limit the extension of the $T_{\rm eff}$-EWR relationship to a broader parameter space. Our study reveals that both classical and weak-line TTSs can exhibit $T_{\rm eff}$ variations exceeding 150 K over a span of two years. The detection of a quarter-phase delay between the EWR and radial velocity phase curves in TTSs indicates spot-driven signals. A phase delay of 0.06 $\pm$ 0.13 for CI Tau, however, suggests additional dynamics, potentially caused by planetary interaction, inferred from a posited 1:1 commensurability between the rotation period and orbital period. Moreover, a positive correlation between $T_{\rm eff}$ variation amplitude and stellar inclination angle support the existence of high-latitude spots on TTSs, further enriching our understanding of stellar surface activity in young stars.