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CSI 2264: Accretion process in classical T Tauri stars in the young cluster NGC 2264

Sousa, A. P. and Alencar, S. H. P. and Bouvier, J. and Stauffer, J. and Venuti, L. and Hillenbrand, L. and Cody, A. M. and Teixeira, P. S. and Guimarães, M. M. and McGinnis, P. T. and Rebull, L. and Flaccomio, E. and Fűrész, G. and Micela, G. and Gameiro, J. F. (2016) CSI 2264: Accretion process in classical T Tauri stars in the young cluster NGC 2264. Astronomy & Astrophysics, 586 . Art. No. A47. ISSN 0004-6361. http://resolver.caltech.edu/CaltechAUTHORS:20160314-122019386

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Abstract

Context. NGC 2264 is a young stellar cluster (~3 Myr) with hundreds of low-mass accreting stars that allow a detailed analysis of the accretion process taking place in the pre-main sequence. Aims. Our goal is to relate the photometric and spectroscopic variability of classical T Tauri stars to the physical processes acting in the stellar and circumstellar environment, within a few stellar radii from the star. Methods. NGC 2264 was the target of a multiwavelength observational campaign with CoRoT, MOST, Spitzer, and Chandra satellites and photometric and spectroscopic observations from the ground. We classified the CoRoT light curves of accreting systems according to their morphology and compared our classification to several accretion diagnostics and disk parameters. Results. The morphology of the CoRoT light curve reflects the evolution of the accretion process and of the inner disk region. Accretion burst stars present high mass-accretion rates and optically thick inner disks. AA Tau-like systems, whose light curves are dominated by circumstellar dust obscuration, show intermediate mass-accretion rates and are located in the transition of thick to anemic disks. Classical T Tauri stars with spot-like light curves correspond mostly to systems with a low mass-accretion rate and low mid-IR excess. About 30% of the classical T Tauri stars observed in the 2008 and 2011 CoRoT runs changed their light-curve morphology. Transitions from AA Tau-like and spot-like to aperiodic light curves and vice versa were common. The analysis of the Hα emission line variability of 58 accreting stars showed that 8 presented a periodicity that in a few cases was coincident with the photometric period. The blue and red wings of the Hα line profiles often do not correlate with each other, indicating that they are strongly influenced by different physical processes. Classical T Tauri stars have a dynamic stellar and circumstellar environment that can be explained by magnetospheric accretion and outflow models, including variations from stable to unstable accretion regimes on timescales of a few years.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1051/0004-6361/201526599DOIArticle
http://www.aanda.org/articles/aa/abs/2016/02/aa26599-15/aa26599-15.htmlPublisherArticle
http://arxiv.org/abs/1509.05354arXivDiscussion Paper
ORCID:
AuthorORCID
Stauffer, J.0000-0003-3595-7382
Cody, A. M.0000-0002-3656-6706
Rebull, L.0000-0001-6381-515X
Additional Information:© 2016 ESO. Received 25 May 2015. Accepted 4 September 2015. A.P.S. and S.H.P.A. acknowledge support from CNPq, CAPES and Fapemig. J.F.G. acknowledges support from FCT ref project UID/FIS/04434/2013.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
Fundação para a Ciência e a Tecnologia (FCT)UID/FIS/04434/2013
Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq)UNSPECIFIED
Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES)UNSPECIFIED
Fundação de Amparo a Pesquisa do Estado de Minas Gerais (FAPEMIG)UNSPECIFIED
Subject Keywords:stars: formation – stars: variables: T Tauri, Herbig Ae/Be – open clusters and associations: individual: NGC 2264 – accretion, accretion disks
Record Number:CaltechAUTHORS:20160314-122019386
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20160314-122019386
Official Citation:CSI 2264: Accretion process in classical T Tauri stars in the young cluster NGC 2264 A. P. Sousa, S. H. P. Alencar, J. Bouvier, J. Stauffer, L. Venuti, L. Hillenbrand, A. M. Cody, P. S. Teixeira, M. M. Guimarães, P. T. McGinnis, L. Rebull, E. Flaccomio, G. Fürész, G. MicelaA. P. Sousa, S. H. P. Alencar, J. Bouvier, J. Stauffer, L. Venuti, L. Hillenbrand, A. M. Cody, P. S. Teixeira, M. M. Guimarães, P. T. McGinnis, L. Rebull, E. Flaccomio, G. Fürész, G. Micela and J. F. Gameiro A&A, 586 (2016) A47 DOI: http://dx.doi.org/10.1051/0004-6361/201526599
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:65336
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:14 Mar 2016 23:43
Last Modified:24 Oct 2017 23:54

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