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dc.contributor.authorFang, M.
dc.contributor.authorSicilia-Aguilar, A.
dc.contributor.authorRoccatagliata, V.
dc.contributor.authorFedele, D.
dc.contributor.authorHenning, Th.
dc.contributor.authorEiroa, C.
dc.contributor.authorMüller, A.
dc.identifier.citationFang , 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 .
dc.identifier.otherPURE: 148513512
dc.identifier.otherPURE UUID: 267eb2df-bb71-4f0c-939c-3ca8fa0f4b1f
dc.identifier.otherScopus: 84908451457
dc.identifier.otherBibCode: 2014A&A...570A.118F
dc.identifier.otherWOS: 000344158500076
dc.descriptionMF 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).en
dc.description.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.
dc.relation.ispartofAstronomy & Astrophysicsen
dc.rights© 2014. ESOen
dc.subjectStars: pre-main sequenceen
dc.subjectStars: binaries: spectroscopicen
dc.subjectStars: individual: GW Orien
dc.subjectLine: profilesen
dc.subjectAccretion disksen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.titleGW Orionis : inner disk readjustments in a triple systemen
dc.typeJournal articleen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.description.statusPeer revieweden

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