Facing the wind of the pre-FUor V1331 Cyg

P. P. Petrov, R. Kurosawa, M. M. Romanova, J. F. Gameiro, M. Fernandez, E. V. Babina, S. A. Artemenko

Resumo
The mass outflows in T Tauri stars (TTS) are thought to be an effective mechanism to remove angular momentum during the pre-main-sequence contraction of a low-mass star. The most powerful winds are observed at the FUor stage of stellar evolution. V1331 Cyg has been considered as a TTS at the pre-FUor stage. We analyse high-resolution spectra of V1331 Cyg collected in 1998–2007 and 20-d series of spectra taken in 2012. For the first time the photospheric spectrum of the star is detected and stellar parameters are derived: spectral type G7–K0 IV, mass 2.8 M⊙, radius 5 R⊙, v sin i < 6 km s−1. The photospheric spectrum is highly veiled, but the amount of veiling is not the same in different spectral lines, being lower in weak transitions and much higher in strong transitions. The Fe ii 5018, Mg i 5183, K i 7699 and some other lines of metals are accompanied by a ‘shell’ absorption at radial velocity of about −240 km s−1. We show that these absorptions form in the post-shock gas in the jet, i.e. the star is seen though its jet. The P Cyg profiles of Hα and Hβ indicate the terminal wind velocity of about 500 km s−1, which vary on time-scales from several days to years. A model of the stellar wind is developed to interpret the observations. The model is based on calculation of hydrogen spectral lines using the radiative transfer code torus. The observed Hα and Hβ line profiles and their variability can be well reproduced with a stellar wind model, where the mass-loss rate and collimation (opening angle) of the wind are variable. The changes of the opening angle may be induced by small variability in magnetization of the inner disc wind. The mass-loss rate is found to vary within (6–11) × 10−8 M⊙ yr−1, with the accretion rate of 2.0 × 10−6 M⊙ yr−1.

Palavras chave
stars: individual: V1331 Cyg, stars: variables: T Tauri, Herbig Ae/Be, stars: winds, outflows

Monthly Notices of the Royal Astronomical Society
Volume 442, Página 3643
agosto 2014

DOI: 10.1093/mnras/stu1131
Código bibliográfico ADS: 2014MNRAS.442.3643P