Astronomy and Astrophysics – Astronomy
Scientific paper
Mar 2012
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012astl...38..167d&link_type=abstract
Astronomy Letters, Volume 38, Issue 3, pp.167-179
Astronomy and Astrophysics
Astronomy
Stars—Individual: Rw Aur, T Tau, T Tauri Stars, Magnetic Field, Disk Accretion, Wind
Scientific paper
Results of ourmeasurements of the longitudinal magnetic field B z for the young star RWAur A are presented. B z measured from the so-called narrow component of the He I 5876 line varies in the range from -1.47 ± 0.15 to +1.10 ± 0.15 kG. Our data are consistent with a stellar rotation period of }~5.6 days and the model of two hot spots with opposite magnetic field polarities spaced about 180° apart in longitude. Relative to the Earth, the spot with B z < 0 lies in the hemisphere above the midplane of the accretion disk, while the spot with B z > 0 is below the midplane. The upper limit for B z (at the 3 σ level) obtained by averaging all observations is 180 G for the photosphere and 220 and 230 G for the H α and [OI] 6300 line formation regions, respectively. We have also failed to detect a field in the formation region of broad emission line components: the upper limit for B z is 600 G. In two of 11 cases, we have detected a magnetic field in the formation region of the blue absorption wing of the Na I D doublet lines, i.e., in the wind from RW Aur A: B z = -180 ± 50 and -810 ± 80 G. The radial velocity of the photospheric lines in RW Aur A averaged over all our observations is }~+10.5 km s-1, i.e., a value lower than that obtained by Petrov et al. (2001) ten years earlier by 5.5 km s-1. Therefore, we discuss the possibility that RW Aur is not a binary but a triple system.
Chuntonov G. A.
Dodin A. V.
Lamzin Sergei A.
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