Classical T Tauri stars: accretion, wind, dust

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Published: Nov 6, 2021
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DOI: https://doi.org/10.31059/aat.vol2.iss1.pp1-8
Keywords:
young stars RY Tau SU Aur RW Aur

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Petr Petrov
Crimean Astrophysical Observatory, Nauchny, 298409

Abstract

Classical T Tauri stars (CTTS) are at the early evolutionary stage when the processes of planet formation take place in the surrounding accretion disks. Most of the observed activity in CTTS is due to magnetospheric accretion and wind flows. Observations of the accreting gas flows and appearance of the line-dependent veiling of the photospheric spectrum in CTTS are considered. Evidence for the dusty wind causing the observed irregular variability of CTTS is presented. Photometric and spectroscopic monitoring of two CTTS, RY Tau and SU Aur, has been carried out at
the Crimean Astrophysical Observatory since 2013 aimed at studying the dynamics of accretion and wind flows on time scales from days to years. The observed variations in the dynamical parameters may be caused by changes in the accretion rate and in the global magnetic fields of CTTS.

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How to Cite
Petrov P., 2021. Acta Astrophysica Taurica, vols. 2, no. 1, pp. 1–8. DOI: 10.31059/aat.vol2.iss1.pp1-8
Issue
Vol. 2 No. 1 (2021)
Section
Research articles
Copyright and publishing rights for texts published in Acta Astrophysica Taurica is retained by the authors, with first publication rights granted to the journal.Texts are free to use with proper attribution and link to the licensing (Creative Commons Attribution 4.0 International).

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