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GW Orionis : inner disk readjustments in a triple system

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Date
10/2014
Author
Fang, M.
Sicilia-Aguilar, A.
Roccatagliata, V.
Fedele, D.
Henning, Th.
Eiroa, C.
Müller, A.
Keywords
Astro-ph.SR
Stars: pre-main sequence
Stars: binaries: spectroscopic
Stars: individual: GW Ori
Line: profiles
Accretion disks
QB Astronomy
QC Physics
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Abstract
(abridged) We study the young stellar system GW Ori, concentrating on its accretion/wind activity by using our high-resolution optical spectra and U-band photometry. We also characterize the disk properties of GW Ori by modeling its spectral energy distribution (SED). By comparing our data to the synthetical spectra, we classify GW Ori as a G8 star. Based on the RVs derived from the spectra, we confirm the previous result as a close companion in GW Ori with a period of ~242 days and an orbital semi-major axis of ~1 AU. The RV residuals after the subtraction of the orbital solution with the equivalent widths of accretion-related emission lines vary with periods of 5-6.7 days during short time intervals, which are caused by the rotational modulation. The H-alpha and H-beta line profiles of GW Ori can be decomposed in two central-peaked emission components and one blue-shifted absorption component. The absorption components are due to a disk wind modulated by the orbital motion of the close companion. Therefore, the systems like GW Ori can be used to study the extent of disk winds. We find that the accretion rates of GW Ori are rather constant but can occasionally be enhanced by a factor of 2-3. We reproduce the SED of GW Ori by using disk models with gaps ~25-55 AU in size. A small population of tiny dust particles within the gap produces the excess emission at near-infrared bands and the strong and sharp silicate feature at 10 μm. The SED of GW Ori exhibits dramatic changes on timescales of ~20 yr in the near-infrared bands, which can be explained as the change in the amount and distribution of small dust grains in the gap. We collect a sample of binary/multiple systems with disks in the literature and find a strong positive correlation between their gap sizes and separations from the primaries to companions, which is generally consistent with the prediction from the theory.
Citation
Fang , M , Sicilia-Aguilar , A , Roccatagliata , V , Fedele , D , Henning , T , Eiroa , C & Müller , A 2014 , ' GW Orionis : inner disk readjustments in a triple system ' , Astronomy & Astrophysics , vol. 570 , A118 . https://doi.org/10.1051/0004-6361/201424146
Publication
Astronomy & Astrophysics
Status
Peer reviewed
DOI
https://doi.org/10.1051/0004-6361/201424146
ISSN
0004-6361
Type
Journal article
Rights
© 2014. ESO
Description
MF acknowledges support of the action “Proyectos de Investigaci´on fundamental no orientada”, grant number AYA2012-35008. ASA support of the Spanish MICINN/MINECO “Ram´on y Cajal” program, grant number RYC-2010-06164, and the action “Proyectos de Investigaci´on fundamental no orientada”, grant number AYA2012-35008. V.R. was partially supported by the Bayerischen Gleichstellungsforderung (BGF).
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  • University of St Andrews Research
URL
http://adsabs.harvard.edu/abs/2014A%26A...570A.118F
URI
http://hdl.handle.net/10023/5662

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