Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/31387
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | Pascucci, Ilaria | en_US |
dc.contributor.author | Banzatti, Andrea | en_US |
dc.contributor.author | Gorti, Uma | en_US |
dc.contributor.author | Fang, Min | en_US |
dc.contributor.author | Pontoppidan, Klaus | en_US |
dc.contributor.author | Alexander, Richard | en_US |
dc.contributor.author | Ballabio, Giulia | en_US |
dc.contributor.author | Edwards, Suzan | en_US |
dc.contributor.author | Salyk, Colette | en_US |
dc.contributor.author | SACCO, GIUSEPPE GERMANO | en_US |
dc.contributor.author | FLACCOMIO, Ettore | en_US |
dc.contributor.author | Blake, Geoffrey A. | en_US |
dc.contributor.author | Carmona, Andres | en_US |
dc.contributor.author | Hall, Cassandra | en_US |
dc.contributor.author | Kamp, Inga | en_US |
dc.contributor.author | Käufl, Hans Ulrich | en_US |
dc.contributor.author | Meeus, Gwendolyn | en_US |
dc.contributor.author | Meyer, Michael | en_US |
dc.contributor.author | Pauly, Tyler | en_US |
dc.contributor.author | Steendam, Simon | en_US |
dc.contributor.author | Sterzik, Michael | en_US |
dc.date.accessioned | 2022-02-11T11:42:56Z | - |
dc.date.available | 2022-02-11T11:42:56Z | - |
dc.date.issued | 2020 | en_US |
dc.identifier.issn | 0004-637X | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/31387 | - |
dc.description.abstract | We analyze high-resolution (Δv ≤ 10 km s<SUP>-1</SUP>) optical and infrared spectra covering the [O I] λ6300 and [Ne II] 12.81 μm lines from a sample of 31 disks in different evolutionary stages. Following work at optical wavelengths, we use Gaussian profiles to fit the [Ne II] lines and classify them into high-velocity component (HVC) or low-velocity component (LVC) if the line centroid is more or less blueshifted than 30 km s<SUP>-1</SUP> with respect to the stellar radial velocity, respectively. Unlike for the [O I], where an HVC is often accompanied by an LVC, all 17 sources with an [Ne II] detection have either an HVC or an LVC. [Ne II] HVCs are preferentially detected toward high accretors ( ${\dot{M}}_{\mathrm{acc}}\gt {10}^{-8}$ M<SUB>⊙</SUB> yr<SUP>-1</SUP>), while LVCs are found in sources with low ${\dot{M}}_{\mathrm{acc}}$ , low [O I] luminosity, and large infrared spectral index (n<SUB>13-31</SUB>). Interestingly, the [Ne II] and [O I] LVC luminosities display an opposite behavior with n<SUB>13-31</SUB>: as the inner dust disk depletes (higher n<SUB>13-31</SUB>), the [Ne II] luminosity increases while the [O I] weakens. The [Ne II] and [O I] HVC profiles are generally similar, with centroids and FWHMs showing the expected behavior from shocked gas in microjets. In contrast, the [Ne II] LVC profiles are typically more blueshifted and narrower than the [O I] profiles. The FWHM and centroid versus disk inclination suggest that the [Ne II] LVC predominantly traces unbound gas from a slow, wide-angle wind that has not lost completely the Keplerian signature from its launching region. We sketch an evolutionary scenario that could explain the combined [O I] and [Ne II] results and includes screening of hard (∼1 keV) X-rays in inner, mostly molecular, MHD winds. | en_US |
dc.language.iso | eng | en_US |
dc.title | The Evolution of Disk Winds from a Combined Study of Optical and Infrared Forbidden Lines | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.3847/1538-4357/abba3c | en_US |
dc.identifier.scopus | 2-s2.0-85096062506 | en_US |
dc.identifier.isi | WOS:000585690100001 | en_US |
dc.identifier.url | https://api.elsevier.com/content/abstract/scopus_id/85096062506 | en_US |
dc.identifier.url | https://iopscience.iop.org/article/10.3847/1538-4357/abba3c | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 903 | en_US |
dc.relation.issue | 2 | en_US |
dc.relation.firstpage | 78 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.international | sì | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | THE ASTROPHYSICAL JOURNAL | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2020ApJ...903...78P | en_US |
dc.relation.ercsector | ERC sectors::Physical Sciences and Engineering::PE9 Universe sciences: astro-physics/chemistry/biology; solar systems; stellar, galactic and extragalactic astronomy, planetary systems, cosmology, space science, instrumentation | en_US |
dc.description.apc | no | en_US |
dc.description.oa | 1 – prodotto con file in versione Open Access (allegare il file al passo 5-Carica) | en_US |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.openairetype | Article | - |
item.languageiso639-1 | en | - |
item.cerifentitytype | Publications | - |
item.grantfulltext | open | - |
item.fulltext | With Fulltext | - |
crisitem.author.dept | O.A. Arcetri | - |
crisitem.author.dept | O.A. Palermo | - |
crisitem.author.orcid | 0000-0002-6893-2221 | - |
crisitem.author.orcid | 0000-0002-3638-5788 | - |
crisitem.journal.journalissn | 0004-637X | - |
crisitem.journal.ance | E016252 | - |
È visualizzato nelle collezioni: | 1.01 Articoli in rivista |
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File | Descrizione | Dimensioni | Formato | |
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2009.09114.pdf | preprint | 1.32 MB | Adobe PDF | Visualizza/apri |
Pascucci_2020_ApJ_903_78.pdf | [Administrators only] | 1.95 MB | Adobe PDF |
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