Hot Gas Lines in T Tauri Stars
David R. Ardila (1), Gregory J. Herczeg (2), Scott G. Gregory (3,4),, Laura Ingleby (5), Kevin France (6), Alexander Brown (6), Suzan Edwards (7),, Christopher Johns-Krull (8), Jeffrey L. Linsky (9), Hao Yang (10), Jeff A., Valenti (11), Herv\'e Abgrall (12)

TL;DR
This study analyzes high-resolution ultraviolet spectra of T Tauri stars to understand accretion processes, revealing line profiles, velocities, and correlations that support complex accretion and outflow models.
Contribution
It provides a comprehensive dataset and detailed line profile analysis of UV resonance lines in T Tauri stars, highlighting multiple accretion columns and outflow signatures.
Findings
C IV lines often show a narrow component with a redshifted broad component.
Velocity measurements support accretion shock models in some stars.
Detection of wind signatures in the C IV line for specific stars.
Abstract
For Classical T Tauri Stars (CTTSs), the resonance lines of N V, Si IV, and C IV, as well as the He II 1640 A line, act as diagnostics of the accretion process. Here we assemble a large high-resolution dataset of these lines in CTTSs and Weak T Tauri Stars (WTTSs). We present data for 35 stars: one Herbig Ae star, 28 CTTSs, and 6 WTTSs. We decompose the C IV and He II lines into broad and narrow Gaussian components (BC & NC). The most common (50 %) C IV line morphology in CTTSs is that of a low-velocity NC together with a redshifted BC. The velocity centroids of the BCs and NCs are such that V_BC > 4 * V_NC, consistent with the predictions of the accretion shock model, in at most 12 out of 22 CTTSs. We do not find evidence of the post-shock becoming buried in the stellar photosphere due to the pressure of the accretion flow. The He II CTTSs lines are generally symmetric and narrow, less…
Peer Reviews
No public reviews on file for this paper yet. If you reviewed it on a platform where reviews are public (OpenReview, ICLR, NeurIPS, ICML), you can paste yours below so the community can read it here.
Videos
No videos yet. Explain this paper in a talk, walkthrough, or lecture? Add one.
