Unveiling extremely veiled T Tauri stars
G. F. Gahm, F. M. Walter, H. C. Stempels, P. P. Petrov, G. J. Herczeg

TL;DR
This study investigates the nature of veiling in classical T Tauri stars, revealing that it is often caused by line emission filling in photospheric lines rather than continuous excess emission, challenging its use as an accretion rate indicator.
Contribution
The paper demonstrates that veiling in certain T Tauri stars is primarily due to line emission filling photospheric lines, not just excess continuum emission, providing new insights into accretion processes.
Findings
Veiling varies strongly and can be extremely large.
Veiling correlates weakly with stellar brightness.
Line emission filling photospheric lines causes large veiling factors.
Abstract
Photospheric absorption lines in classical T Tauri stars (CTTS) are weak compared to normal stars. This so-called veiling is normally identified with an excess continuous emission formed in shock-heated gas at the stellar surface below the accretion streams. We have selected four stars (RW Aur A, RU Lup, S CrA NW and S CrA SE) with unusually strong veiling to make a detailed investigation of veiling versus stellar brightness and emission line strengths for comparisons to standard accretion models. We have monitored the stars photometrically and spectroscopically at several epochs. In standard accretion models a variable accretion rate will lead to a variable excess emission. Consequently, the stellar brightness should vary accordingly. We find that the veiling of absorption lines in these stars is strongly variable and usually so large that it would require the release of several…
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