ABSTRACT We present a study of permitted emission lines of Fe I and Fe II in the spectrum of the highÈaccretion rate classical T Tauri star DR Tau. Classical T Tauri stars (CTTS) are low-mass pre-main-sequence objects with intense emission line spectra. We report new magnetic field measurements for 14 classical T Tauri stars (CTTSs). 0000000691 00000 n 1991, 1992; Malbet & Bertout 1992 and others). 0000006362 00000 n 0000003095 00000 n The MHD equations, including radiative energy transport, are solved for an axisymmetric system with a resistive, turbulent gas. The weak T Tauri stars are of particular interest since they provide astronomers with a look at early stages of stellar evolution unencumbered by nebulous material. We report here results of spectropolarimetric observations of the classical T Tauri star (cTTS) GQ Lup carried out with ESPaDOnS at the Canada–France–Hawaii Telescope (CFHT) in the framework of the ‘Magnetic Protostars and Planets’ (MaPP) programme, and … 2004) campaign on theSpitzer Space Telescope(Werner et al. To find out more, see our Privacy and Cookies policy. High-resolution (R ≈ 60,000) circular spectropolarimetry of the classical T Tauri star T Tau is presented. This phenomenon has only been observed in one other source, the classical T Tauri (CTTS) star RW Aur. In standard models the spectacular emission spectrum is explained as the manifes-tation of magnetospheric accretion of material from a circum-stellar disk. Classical T-Tauri Star (CTTS) actively accreting matter, UV & Infared excess. The classical T Tauri stage lasts about 10 million years. Apr 23, 2007 Abstract. T Tauri Stars in Galactic Star-Forming Regions. tion, the classical T Tauri stars provide the opportunity to probe the interface between a young low-mass star and its accretion disk. T Tauri stars (TTS) are a class of variable stars that are less than about ten million years old. The physical mechanism responsible for the brightening of the redshifted lobe although as yet unknown must also now apply at BD masses to include the ISO-ChaI 217 outflow. The Spectral Variability of the Classical T Tauri Star TW Hydrae This information should not be considered complete, up to date, and is not intended to be used in place of a visit, consultation, or advice of a legal, medical, or any other professional. 5000 Å to 9000 Å. The weak T Tauri stars are of particular interest since they provide astronomers with a look at early stages of stellar evolution unencumbered by nebulous material. Combining these temperature and gravity results with magnetic stellar evolutionary models, we nd the age of T Tau N to be less than 1 Myr old. Classical T Tauri stars have extensive disks that result in strong emission lines. A 1.8 kG dipole tilted at 129 with respect to the rotation axis and a … We argue that accreting objects can be identified from low-resolution optical spectroscopy, when their Hα flux is stronger than the saturation limit at Log {Lum(Hα)/Lum(bol)} = −3.3. G. Gregory, J.-F. Donati3 and G. Hussain4 1University of Vienna, Department of Astrophysics, Turkenschanzstrasse 17, A-1180 Vienna, Austria¨ 2School of Physics and Astronomy, Universtiy of St Andrews, St Andrews, KY16 9SS, UK A → T Tauri star in which → accretion from a → circumstellar disk is responsible for ultraviolet and infrared excess emission and for a moderate to strong emission line spectrum superimposed on the photospheric spectrum. 0000002857 00000 n The origin and the physical conditions of the wind from YSOs are crucial to our understanding of the protostellar … A maximum longitudinal ﬁeld of 370 ± 80 G is detected from the photospheric lines on BP Tau. 2004). By M. M. Jardine, S. G. Gregory and J.-F. Donati. G. Gregory, J.-F. Donati3 and G. Hussain4 1University of Vienna, Department of Astrophysics, Turkenschanzstrasse 17, A-1180 Vienna, Austria¨ 2School of Physics and Astronomy, Universtiy of St Andrews, St Andrews, KY16 9SS, UK Cite . 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