A New Look at T Tauri Star Forbidden Lines: MHD-driven Winds from the Inner Disk

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dc.citation.articleNumber28
dc.citation.issueNumber1
dc.citation.journalTitleThe Astrophysical Journal
dc.citation.volumeNumber868
dc.contributor.authorFang, Min
dc.contributor.authorPascucci, Ilaria
dc.contributor.authorEdwards, Suzan
dc.contributor.authorGorti, Uma
dc.contributor.authorBanzatti, Andrea
dc.contributor.authorFlock, Mario
dc.contributor.authorHartigan, Patrick
dc.contributor.authorHerczeg, Gregory J.
dc.contributor.authorDupree, Andrea K.
dc.date.accessioned2019-01-11T15:35:23Z
dc.date.available2019-01-11T15:35:23Z
dc.date.issued2018
dc.description.abstractMagnetohydrodynamic (MHD) and photoevaporative winds are thought to play an important role in the evolution and dispersal of planet-forming disks. We report the first high-resolution (Δ v ∼ 6 km s −1 ) analysis of [S ii ] λ 4068, [O i ] λ 5577, and [O i ] λ 6300 lines from a sample of 48 T Tauri stars. Following Simon et al. we decompose them into three kinematic components: a high-velocity component (HVC) associated with jets, and low-velocity narrow (LVC-NC) and broad (LVC-BC) components. We confirm previous findings that many LVCs are blueshifted by more than 1.5 km s −1 and thus most likely trace a slow disk wind. We further show that the profiles of individual components are similar in the three lines. We find that most LVC-NC and LVC-BC line ratios are explained by thermally excited gas with temperatures between 5000 and 10,000 K and electron densities of ∼10 7 –10 8 cm −3 . The HVC ratios are better reproduced by shock models with a pre-shock H number density of ∼10 6 –10 7 cm −3 . Using these physical properties, we estimate ##IMG## [http://ej.iop.org/images/0004-637X/868/1/28/apjaae780ieqn1.gif] $\dotM_\mathrmwind/\dotM_\mathrmacc$ for the LVC and ##IMG## [http://ej.iop.org/images/0004-637X/868/1/28/apjaae780ieqn2.gif] $\dotM_\mathrmjet/\dotM_\mathrmacc$ for the HVC. In agreement with previous work, the mass carried out in jets is modest compared to the accretion rate. With the likely assumption that the LVC-NC wind height is larger than the LVC-BC, the LVC-BC ##IMG## [http://ej.iop.org/images/0004-637X/868/1/28/apjaae780ieqn3.gif] $\dotM_\mathrmwind/\dotM_\mathrmacc$ is found to be higher than the LVC-NC. These results suggest that most of the mass loss occurs close to the central star, within a few au, through an MHD-driven wind. Depending on the wind height, MHD winds might play a major role in the evolution of the disk mass.
dc.identifier.citationFang, Min, Pascucci, Ilaria, Edwards, Suzan, et al.. "A New Look at T Tauri Star Forbidden Lines: MHD-driven Winds from the Inner Disk." <i>The Astrophysical Journal,</i> 868, no. 1 (2018) IOP Publishing: https://doi.org/10.3847/1538-4357/aae780.
dc.identifier.digitalFang_2018
dc.identifier.doihttps://doi.org/10.3847/1538-4357/aae780
dc.identifier.urihttps://hdl.handle.net/1911/105070
dc.language.isoeng
dc.publisherIOP Publishing
dc.rightsArticle is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use.
dc.titleA New Look at T Tauri Star Forbidden Lines: MHD-driven Winds from the Inner Disk
dc.typeJournal article
dc.type.dcmiText
dc.type.publicationpublisher version
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