Show simple item record

dc.contributor.authorMendigutía, I.
dc.contributor.authorBrittain, Sean D.
dc.contributor.authorEiroa, Carlos
dc.contributor.authorMeeus, Gwendolyn 
dc.contributor.authorMontesinos, Benjamín
dc.contributor.authorMora, Alcione
dc.contributor.authorMuzerolle, James C.
dc.contributor.authorOudmaijer, René D.
dc.contributor.authorRigliaco, Elisabetta
dc.contributor.otherUAM. Departamento de Física Teóricaes_ES
dc.date.accessioned2014-09-22T07:59:11Z
dc.date.available2014-09-22T07:59:11Z
dc.date.issued2013-10-10
dc.identifier.citationThe Astrophysical Journal 776.1 (2013): 44en_US
dc.identifier.issn0004-637X (print)es_ES
dc.identifier.issn1538-4357 (online)es_ES
dc.identifier.urihttp://hdl.handle.net/10486/661888
dc.descriptionThe Astrophysical Journal 776.1 (2013): 44, reproduced by permission of the AASen_US
dc.description.abstractThis work presents X-Shooter/Very Large Telescope spectra of the prototypical, isolated Herbig Ae stars HD 31648 (MWC 480) and HD 163296 over five epochs separated by timescales ranging from days to months. Each spectrum spans over a wide wavelength range covering from 310 to 2475 nm. We have monitored the continuum excess in the Balmer region of the spectra and the luminosity of 12 ultraviolet, optical, and near-infrared spectral lines that are commonly used as accretion tracers for T Tauri stars. The observed strengths of the Balmer excesses have been reproduced from a magnetospheric accretion shock model, providing a mean mass accretion rate of 1.11 × 10-7 and 4.50 × 10-7 Mʘyr-1 for HD 31648 and HD 163296, respectively. Accretion rate variations are observed, being more pronounced for HD 31648 (up to 0.5 dex). However, from the comparison with previous results it is found that the accretion rate of HD 163296 has increased by more than 1 dex, on a timescale of ∼15 yr. Averaged accretion luminosities derived from the Balmer excess are consistent with the ones inferred from the empirical calibrations with the emission line luminosities, indicating that those can be extrapolated to HAe stars. In spite of that, the accretion rate variations do not generally coincide with those estimated from the line luminosities, suggesting that the empirical calibrations are not useful to accurately quantify accretion rate variabilityen_US
dc.description.sponsorshipThis work are supported by AYA 2011-26202 and RYC-2011-07920.en_US
dc.format.extent12 pag.es_ES
dc.format.mimetypeapplication/pdfes_ES
dc.language.isoenges_ES
dc.publisherThe American Astronomical Societyen_US
dc.relation.ispartofAstrophysical Journalen_US
dc.rights© 2013. The American Astronomical Societyen_US
dc.subject.otherOpen clusters and associationsen_US
dc.subject.otherHerbig Ae/Been_US
dc.subject.otherProtoplanetary disksen_US
dc.subject.otherStars: pre-main sequenceen_US
dc.subject.otherT Taurien_US
dc.subject.otherAccretionen_US
dc.subject.otherAccretion disksen_US
dc.titleAccretion variability of Herbig Ae/Be stars observed by x-shooter HD 31648 and HD 163296en_US
dc.typearticleen
dc.subject.ecienciaFísicaes_ES
dc.relation.publisherversionhttp://dx.doi.org/10.1088/0004-637X/776/1/44es_ES
dc.identifier.doi10.1088/0004-637X/776/1/44es_ES
dc.identifier.publicationfirstpage44es_ES
dc.identifier.publicationissue1es_ES
dc.identifier.publicationlastpageundefinedes_ES
dc.identifier.publicationvolume776es_ES
dc.type.versioninfo:eu-repo/semantics/publishedVersiones_ES
dc.rights.accessRightsopenAccessen
dc.authorUAMEiroa De San Francisco, Carlos (259722)
dc.authorUAMMeeus , Gwendolyn (264398)
dc.authorUAMMontesinos Comino , Benjamín (269116)
dc.facultadUAMFacultad de Ciencias


Files in this item

Thumbnail

This item appears in the following Collection(s)

Show simple item record