3D SIMULATIONS OF MAGNETOSPHERIC FLOW IN CLASSICAL T TAURI STARS. M.M. Romanova 1
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Line profiles of CO 137 IS 113, and H alpha, observed in a dozen T Tauri stars with the KENO 4m echelle spectrograph, provide probes of the density, spatial extent, and anisotropy of T Tauri winds.
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view Abstract Citations (54) References (11) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Polarization observations of the T Tauri stars RY Tauri, T Tauri, and V866 Scorpii. Bastien, P. ; Landstreet, J. D. Abstract Observations of the wavelength dependence of linear polarization of the T Tauri stars RY Tauri, T Tauri, and V866 Scorpii are presented. These observations show that most of the polarization of these stars arises in extended circumstellar dust envelopes which lie outside the high-temperature gas-emitting regions. The distribution of this matter around the stars has no fixed axis of symmetry, such as is usually found in Be stars. Strong variations in the wavelength dependence of polarization are observed, which suggest large variations in the grain size in the dust scattering regions. Publication: The Astrophysical Journal Pub Date: May 1979 DOI: 10.1086/182947 Bibcode: 1979ApJ...229L.137B Keywords: Linear Polarization; Polarimetry; Stellar Envelopes; T Tauri Stars; Variable Stars; Interstellar Matter; Main Sequence Stars; Particle Size Distribution; Thomson Scattering; Astrophysics; Circumstellar Envelopes:T Tauri Stars; Polarization:T Tauri Stars full text sources ADS | data products SIMBAD (3)
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We have investigated the magnetic field strength of one weak-line and four classical T Tauri stars. The magnetic field strength is derived from the differential change of the equivalent width of photospheric Fei lines in the presence of a magnetic field, calculated using a full radiative transfer code. The method was successfully tested by applying it to a non- magnetic solar-type star, and to VY Ari which is believed to have a strong magnetic field. For two of the classical T Tauri stars, we find a product of magnetic field strength and filling factor B f =( 2:35 0:15) kG for T Tau, and B f =( 1:1 0:2) kG for LkCa 15. For the classical T Tauri star UX Tau A and the weak-line T Tauri star LkCa 16 the detection is only marginal, indicating magnetic field strengths of the order of 1 kG and possibly of more than 2 kG, respectively. No field could be de- tected for the classical T Tauri star GW Ori. For the two classical T Tauri stars for which we have detected a field, we find the fil- ling factors to be larger than 0:5, which indicates that the magnetic field covers most of the photosphere. We also show that ignoring a magnetic field can, depending on the lines used, result in errors in effective temperature and underestimates of veiling.
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Classical T Tauri stars (hereinafter CTTS) are protostars formed by collapse of molecular clouds. As they evolve towards the main sequence, CCTS accrete from the circumstellar matter and contract due to self-gravitation. Mass accretion and gravitational contraction can accelerate the spin velocities of CTTS up to break-up (～300—400km·s) within
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On considere le rayonnement d'ondes MHD lorsque le nuage de plasma protostellaire tombe le long d'un champ magnetique ambiant a l'interieur d'une etoile T Tauri
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