scholarly journals A polarization outburst in the T Tauri star UY Aurigae

1987 ◽  
Vol 122 ◽  
pp. 133-134 ◽  
Author(s):  
F. Ménard ◽  
P. Bastien
Keyword(s):  
Linear Polarization ◽  
T Tauri Stars ◽  
Tauri Star ◽  
Monitoring Programme ◽  
Strong Polarization ◽  
Visual Binary ◽  
T Tauri ◽  
First Time

During the course of a monitoring programme of the linear polarization of various T Tauri stars, UY Aur was observed to undergo a strong polarization burst between 1984 October and 1985 January. The linear polarization rised from about 1.5% early in 1984 to a maximum of 7.6% in 1984 October and declined back to the earlier value after 3 to 4 months. It is the first time that such a large increase in linear polarization is reported in a T Tauri star. However the interpretation is complicated by the fact that UY Aur is a visual binary with a separation of 0.8 and both components were included in the measurements.

Seeking for magnetic fields in rotating disk/jets with ALMA polarimetry

2018 ◽  
Vol 14 (A30) ◽  
pp. 128-129
Author(s):  
Francesca Bacciotti ◽  
Josep Miquel Girart ◽  
Marco Padovani
Keyword(s):  
Linear Polarization ◽  
Thermal Emission ◽  
Rotating Disk ◽  
Polarization Angle ◽  
T Tauri ◽  
Magnetic Signatures ◽  
Dust Evolution ◽  
First Time ◽  
Crucial Ingredient ◽  
Polarization Fraction

AbstractThe Atacama Large Millimeter/submillimeter Array (ALMA) is providing important advances in studies of star formation. In particular, polarimetry can reveal the disk magnetic configuration, a crucial ingredient in many processes, as, for example, the transport of angular momentum. We analized ALMA Band 7 (870 μm) polarimetric data at 0.”2 resolution for the young rotating disk/jet systems DG Tau and CW Tau, to find magnetic signatures. From the Stokes I, U, Q maps, we derive the linear polarization intensity, $P = \sqrt {{Q^2} + {U^2}} $ , the linear polarization fraction, and the polarization angle. The alignment of the latter with the disk minor axis (Fig. 1) shows that self-scattering of dust thermal emission rather than magnetic alignment dominates the polarization in both targets (Bacciotti et al. 2018). However, several dust properties can be diagnosed comparing the polarization data with the models of self-scattering (e.g. Kataoke et al. 2017, Yang et al. 2017). The maximum grain size turns out to be in the range 50 - 70 μm for DG Tau and 100 - 150 μm for CW Tau. The asymmetry of the polarized intensity in DG Tau, observed for the first time around a T Tauri star, indicates that the disk is flared. Moreover, the observed belt-like feature may betray the presence of a disk substructure. In contrast, the polarization maps of CW Tau indicate that here the grains have settled to the disk midplane. Polarimetry is thus very important in studies of the dust evolution.

scholarly journals Circular polarization in T Tauri stars

1987 ◽  
Vol 122 ◽  
pp. 131-132
Author(s):  
P. Bastien ◽  
R. Nadeau
Keyword(s):  
Circular Polarization ◽  
Linear Polarization ◽  
T Tauri Stars ◽  
T Tauri

We report the detection of circular polarization in three T Tauri stars with known intrinsic linear polarization. A circumstellar origin is required.

scholarly journals Properties of CVSO 30 from TESS measurements: probably a binary T Tauri star with complex light curves and no obvious planets

2020 ◽  
Vol 494 (3) ◽  
pp. 4349-4356
Author(s):  
C Koen
Keyword(s):  
Light Curve ◽  
Small Group ◽  
T Tauri Stars ◽  
Light Curves ◽  
Tauri Star ◽  
Curve Shape ◽  
T Tauri

ABSTRACT ‘Transiting Exoplanet Survey Satellite’ (TESS) photometry of CVSO 30 spanned 21.8 d, with a single large gap of 1.1 d. This allows alias-free determination of the two periodicities in the data. It is confirmed that both of these are non-sinusoidal: the dominant P1 = 0.4990 d has two detectable harmonics and P2 = 0.4486 d has seven. The large number of harmonics in the second periodicity characterizes a very complex light curve shape. One of the features in the light curve is a sharp dip of duration ∼2 h: this is probably the source of the previously claimed planetary transit signature. The star is a member of a small group of T Tauri stars with complex light curves, which have recently been exhaustively studied using Kepler and TESS observations. The two non-commensurate periods are most simply interpreted as being from two stars, i.e. CVSO 30 is probably a binary.

Linear polarization of T Tauri stars. I - Variability of southern stars

1989 ◽  
Vol 97 ◽  
pp. 814 ◽  
Author(s):  
Laurent Drissen ◽  
Pierre Bastien ◽  
Nicole St.-Louis
Keyword(s):  
Linear Polarization ◽  
T Tauri Stars ◽  
T Tauri

scholarly journals Accretion dynamics and star-disk interaction in NCG 2264

2009 ◽  
Vol 5 (H15) ◽  
pp. 735-735 ◽  
Author(s):  
Silvia H. P. Alencar ◽  
Jérôme Bouvier ◽  
Claude Catala ◽  
Matilde Fernandez ◽  
Jorge Filipe Gameiro ◽  
...  
Keyword(s):  
Magnetic Field ◽  
T Tauri Stars ◽  
Stellar Cluster ◽  
Its Analysis ◽  
T Tauri ◽  
Long Run ◽  
Hydrodynamical Simulations ◽  
First Time

The Corot satellite observed the young stellar cluster NGC 2264 during 23 days in March 2008. This was the first time a group of young accreting stars, classical T Tauri stars (CTTS), were followed ininterruptedly with high photometric accuracy for such a long run. Before the Corot observations, AA Tau (Bouvier et al. 2003, A&A, 409, 169 and Bouvier et al. 2007, A&A, 463, 1017) was one of the few CTTS systems that had been analysed synoptically over several consecutive rotational periods. Its analysis suggested a highly dynamical star-disk interaction mediated by the stellar magnetic field, as predicted by magneto-hydrodynamical simulations of young accreting systems.

scholarly journals LAMP: the long-term accretion monitoring programme of T Tauri stars in Chamaeleon I

2012 ◽  
Vol 427 (2) ◽  
pp. 1344-1362 ◽  
Author(s):  
G. Costigan ◽  
A. Scholz ◽  
B. Stelzer ◽  
T. Ray ◽  
J. S. Vink ◽  
...  
Keyword(s):  
T Tauri Stars ◽  
Monitoring Programme ◽  
T Tauri

scholarly journals A giant X-ray flare from a B9 + Post-T Tauri system detected by EXOSAT

1989 ◽  
Vol 104 (2) ◽  
pp. 131-134
Author(s):  
G. Tagliaferri ◽  
P. Giommi ◽  
L. Angelini ◽  
J.P. Osborne ◽  
R. Pallavicini
Keyword(s):  
Tauri Star ◽  
Optical Methods ◽  
Type I ◽  
Late Type ◽  
Optical Studies ◽  
X Ray ◽  
Visual Binary ◽  
T Tauri ◽  
Seyfert Type

AbstractWe report the serendipitous discovery by EXOSAT of a flaring X-ray source in the field of the Seyfert type I galaxy III ZW 2. We identify this source with the visual binary HD 560 (B9V + G5Ve) and argue that virtually all of the observed X-ray flux, including the flare, came from its late-type component (HD 560 B). Optical studies have lead to the identification of HD 560 B as a post-T Tauri star. Since these stars are difficult to detect by optical methods, X-ray observations may prove to be the best way to identify them.

scholarly journals Gas at the inner disk edge

2007 ◽  
Vol 3 (S243) ◽  
pp. 135-146 ◽  
Author(s):  
John S. Carr
Keyword(s):  
Infrared Spectroscopy ◽  
Molecular Spectroscopy ◽  
T Tauri Stars ◽  
Tauri Star ◽  
T Tauri ◽  
Short Period ◽  
Innermost Region

AbstractInfrared molecular spectroscopy is a key tool for the observation of gas in the innermost region of disks around T Tauri stars. In this contribution, we examine how infrared spectroscopy of CO can be used to study the inner truncation region of disks around T Tauri stars. The inferred inner gas radii for T Tauri star disks are compared to the inner dust radii of disks, to the expectations of models for disk truncation, and to the orbital distribution of short-period extra-solar planets.

Sign in / Sign up

Export Citation Format

Share Document