STABLE and UNSTABLE REGIMES of MASS ACCRETION onto RW AUR A

Please use this identifier to cite or link to this item: https://ir.lib.ncu.edu.tw/handle/987654321/101916

Title:	STABLE and UNSTABLE REGIMES of MASS ACCRETION onto RW AUR A
Authors:	陳文屏;Takami, Michihiro;Wei, Yu-Jie;Chou, Mei-Yin;Karr, Jennifer L.;Beck, Tracy L.;Manset, Nadine;Chen, Wen-Ping;Kurosawa, Ryuichi;Fukagawa, Misato;White, Marc;Galván-Madrid, Roberto;Liu, Hauyu Baobab;Pyo, Tae-Soo;Donati, Jean-Francois
Contributors:	理學院天文研究所
Keywords:	ABSORPTION;Accretion;ACCRETION DISKS;accretion, accretion disks;ASTROPHYSICS, COSMOLOGY AND ASTRONOMY;CALCIUM;ECLIPSE;EMISSION;Fluxes;HELIUM;High resolution;line: profiles;LITHIUM;MASS;MONITORING;OXYGEN;PHOTOMETRY;Photosphere;RED SHIFT;RESOLUTION;Sciences of the Universe;Spectroscopic telescopes;STAR ACCRETION;stars: individual (RW Aur A);stars: pre-main sequence;T TAURI STARS;TELESCOPES;X RADIATION
Date:	2016-04-01
Issue Date:	2026-04-21 14:51:00 (UTC+8)
Publisher:	IOP Publishing Ltd.;United States: The American Astronomical Society
Abstract:	摘要： ABSTRACT We present monitoring observations of the active T Tauri star RW Aur, from 2010 October to 2015 January, using optical high-resolution (R ≥ 10,000) spectroscopy with Canada-France-Hawaii Telescope/ESPaDOnS. Optical photometry in the literature shows bright, stable fluxes over most of this period, with lower fluxes (by 2-3 mag) in 2010 and 2014. In the bright period our spectra show clear photospheric absorption, complicated variation in the Ca ii λ8542 emission profile shapes, and a large variation in redshifted absorption in the O i λλ7772 and 8446 and He i λ5876 lines, suggesting unstable mass accretion during this period. In contrast, these line profiles are relatively uniform during the faint periods, suggesting stable mass accretion. During the faint periods, the photospheric absorption lines are absent or marginal, and the averaged Li i profile shows redshifted absorption due to an inflow. We discuss (1) occultation by circumstellar material or a companion and (2) changes in the activity of mass accretion to explain the above results, together with near-infrared and X-ray observations from 2011 to 2015. Neither scenario can simply explain all the observed trends, and more theoretical work is needed to further investigate their feasibilities. 其他題名： APJ 其他題名： Astrophys. J 出版者： United States: The American Astronomical Society 出版日期： 2016-04-01 出處： The Astrophysical Journal, 2016-04, Vol.820 (2), p.139--139 資源來源： Institute of Physics Journals 版權： 2016. The American Astronomical Society. All rights reserved. 版權： licence_http://creativecommons.org/publicdomain/zero 識別號： ISSN: 0004-637X 識別號： ISSN: 1538-4357 識別號： EISSN: 1538-4357 識別號： DOI: 10.3847/0004-637X/820/2/139
Appears in Collections:	[Graduate Institute of Astronomy] journal & Dissertation

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