Twenty-five years of accretion onto the classical T Tauri star TW Hya

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dc.creatorGregory Herczeg
dc.creatorYuguang Chen
dc.creatorJean-Francois Donat
dc.creatorAndrea Dupree
dc.creatorFrederick Walter
dc.creatorLynne Anne Hillenbrand
dc.creatorChristopher Johns-Krull
dc.creatorCarlo Felice Manara
dc.creatorHans Moritz Günther
dc.creatorMin Fang
dc.creatorChristian Philip Schneider
dc.creatorJeff Valenti
dc.creatorSilvia Helena Paixão Alencar
dc.creatorLaura Venuti
dc.creatorJuan Manuel Alcalá
dc.creatorAntonio Frasca
dc.creatorNicole Arulanantham
dc.creatorJeffrey Linsky
dc.creatorJerome Bouvier
dc.creatorNancy Susan Brickhouse
dc.creatorNuria Calvet
dc.creatorCatherine Espaillat
dc.creatorJustyn Campbell-White
dc.creatorJohn Carpenter
dc.creatorSeok-Jun Chang
dc.creatorKelle Cruz
dc.creatorScott Dahm
dc.creatorJochen Eislöffel
dc.creatorSuzan Edwards
dc.creatorWilliam Fischer
dc.creatorZhen Guo
dc.creatorThomas Henning
dc.creatorTao Ji
dc.creatorJessy Jose
dc.creatorJoel Kastner
dc.creatorRalf Launhardt
dc.creatorDavid Principe
dc.creatorConnor Robinson
dc.creatorGregory Schwarz
dc.creatorMichael Sterzik
dc.creatorShinsuke Takasao
dc.date.accessioned2025-02-03T14:25:27Z
dc.date.accessioned2025-09-09T00:45:31Z
dc.date.available2025-02-03T14:25:27Z
dc.date.issued2023-10-20
dc.format.mimetypepdf
dc.identifier.doihttps://doi.org/10.3847/1538-4357/acf468
dc.identifier.issn0004-637X
dc.identifier.urihttps://hdl.handle.net/1843/79602
dc.languageeng
dc.publisherUniversidade Federal de Minas Gerais
dc.relation.ispartofThe Astrophysical Journal
dc.rightsAcesso Aberto
dc.subjectEstrelas T Tauri
dc.subjectEspectroscopia de alta resolução
dc.subjectEstrelas variaveis
dc.subject.otherAcreção magnetosférica
dc.subject.otherVelamento espectral
dc.titleTwenty-five years of accretion onto the classical T Tauri star TW Hya
dc.typeArtigo de periódico
local.citation.epage27
local.citation.issue2
local.citation.spage1
local.citation.volume956
local.description.resumoAccretion plays a central role in the physics that governs the evolution and dispersal of protoplanetary disks. The primary goal of this paper is to analyze the stability over time of the mass accretion rate onto TW Hya, the nearest accreting solar-mass young star. We measure veiling across the optical spectrum in 1169 archival high-resolution spectra of TW Hya, obtained from 1998–2022. The veiling is then converted to accretion rate using 26 flux-calibrated spectra that cover the Balmer jump. The accretion rate measured from the excess continuum has an average of 2.51 × 10−9M⊙ yr−1 and a Gaussian distribution with an FWHM of 0.22 dex. This accretion rate may be underestimated by a factor of up to 1.5 because of uncertainty in the bolometric correction and another factor of 1.7 because of excluding the fraction of accretion energy that escapes in lines, especially Lyα. The accretion luminosities are well correlated with He line luminosities but poorly correlated with Hα and Hβ luminosity. The accretion rate is always flickering over hours but on longer timescales has been stable over 25 years. This level of variability is consistent with previous measurements for most, but not all, accreting young stars.
local.identifier.orcidhttps://orcid.org/0000-0002-7154-6065
local.identifier.orcidhttps://orcid.org/0000-0003-4520-5395
local.identifier.orcidhttps://orcid.org/0000-0001-5541-2887
local.identifier.orcidhttps://orcid.org/0000-0002-8985-8489
local.identifier.orcidhttps://orcid.org/0000-0001-7796-1756
local.identifier.orcidhttps://orcid.org/0000-0002-4265-047X
local.identifier.orcidhttps://orcid.org/0000-0002-8828-6386
local.identifier.orcidhttps://orcid.org/0000-0003-3562-262X
local.identifier.orcidhttps://orcid.org/0000-0003-4243-2840
local.identifier.orcidhttps://orcid.org/0000-0001-8060-1321
local.identifier.orcidhttps://orcid.org/0000-0002-5094-2245
local.identifier.orcidhttps://orcid.org/0000-0003-3305-6281
local.identifier.orcidhttps://orcid.org/0000-0002-5171-8376
local.identifier.orcidhttps://orcid.org/0000-0002-4115-0318
local.identifier.orcidhttps://orcid.org/0000-0001-8657-095X
local.identifier.orcidhttps://orcid.org/0000-0002-0474-0896
local.identifier.orcidhttps://orcid.org/0000-0003-2631-5265
local.identifier.orcidhttps://orcid.org/0000-0003-4446-3181
local.identifier.orcidhttps://orcid.org/0000-0002-7450-6712
local.identifier.orcidhttps://orcid.org/0000-0002-8704-4473
local.identifier.orcidhttps://orcid.org/0000-0002-3950-5386
local.identifier.orcidhttps://orcid.org/0000-0001-9227-5949
local.identifier.orcidhttps://orcid.org/0000-0003-2251-0602
local.identifier.orcidhttps://orcid.org/0000-0002-0112-5900
local.identifier.orcidhttps://orcid.org/0000-0002-1821-0650
local.identifier.orcidhttps://orcid.org/0000-0002-2968-2418
local.identifier.orcidhttps://orcid.org/0000-0001-6496-0252
local.identifier.orcidhttps://orcid.org/0000-0002-3232-665X
local.identifier.orcidhttps://orcid.org/0000-0002-3747-2496
local.identifier.orcidhttps://orcid.org/0000-0003-0292-4832
local.identifier.orcidhttps://orcid.org/0000-0002-1493-300X
local.identifier.orcidhttps://orcid.org/0000-0003-4908-4404
local.identifier.orcidhttps://orcid.org/0000-0002-3138-8250
local.identifier.orcidhttps://orcid.org/0000-0002-8298-2663
local.identifier.orcidhttps://orcid.org/0000-0002-7939-377X
local.identifier.orcidhttps://orcid.org/0000-0003-1639-510X
local.identifier.orcidhttps://orcid.org/0000-0002-0786-7307
local.identifier.orcidhttps://orcid.org/0000-0002-5784-4437
local.identifier.orcidhttps://orcid.org/0000-0003-3882-3945
local.publisher.countryBrasil
local.publisher.departmentICX - DEPARTAMENTO DE FÍSICA
local.publisher.initialsUFMG
local.url.externahttps://iopscience.iop.org/article/10.3847/1538-4357/acf468/pdf

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