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dc.contributor.authorSchimoia, Jáderson da Silvapt_BR
dc.contributor.authorStorchi-Bergmann, Thaisapt_BR
dc.contributor.authorNemmen, Rodrigo S.pt_BR
dc.contributor.authorWinge, Claudiapt_BR
dc.contributor.authorEracleous, Michaelpt_BR
dc.date.accessioned2015-01-20T02:15:16Zpt_BR
dc.date.issued2012pt_BR
dc.identifier.issn0004-637Xpt_BR
dc.identifier.urihttp://hdl.handle.net/10183/109056pt_BR
dc.description.abstractThe broad (FWHM ∼ 10,000 km s-ˡ) double-peaked Hα profile from the LINER/Seyfert 1 nucleus of NGC 1097 was discovered in 1991 and monitored for the following 11 years. The profile showed variations attributed to the rotation of gas in a non-axisymmetric Keplerian accretion disk, ionized by a varying radiatively inefficient accretion flow (RIAF) located in the inner parts of the disk. We present and model 11 new spectroscopic observations of the double-peaked profile taken between 2010 March and 2011 March. This series of observations was motivated by the finding that in 2010 March the flux in the double-peaked line was again strong, indeed, in 2010 December, even stronger than in the observations of a decade ago. We also discovered shorter timescale variations than in the previous observations: (1) the first, of ∼7 days, is interpreted as due to “reverberation” of the variation of the ionizing source luminosity, and the timescale of 7 days as the light crossing time between the source and the accretion disk; this new timescale and its interpretation provides a distance between the emitting gas and the supermassive black hole and as such introduces a new constraint on its mass; (2) the second, of ≈5 months, was attributed to the rotation of a spiral arm in the disk, which was found to occur on the dynamical timescale. We use two accretion disk models to fit theoretical profiles to the new data, both having non-axisymmetric emissivities produced by the presence of an one-armed spiral. Our modeling constrains the rotation period for the spiral to be ≈18 months. This work supports our previous conclusion that the broad double-peaked Balmer emission lines in NGC 1097—and probably also in other low-luminosity active nuclei—originate from an accretion disk ionized by a central RIAF.en
dc.format.mimetypeapplication/pdf
dc.language.isoengpt_BR
dc.relation.ispartofThe astrophysical journal. Bristol. Vol. 748, no. 2 (Apr. 2012), 145, 12 p.pt_BR
dc.rightsOpen Accessen
dc.subjectAcreçãopt_BR
dc.subjectAccretion, accretion disksen
dc.subjectGalaxies: individual (NGC 1097)en
dc.subjectDiscos de acrecaopt_BR
dc.subjectBuracos negrospt_BR
dc.subjectGalaxies: nucleien
dc.subjectGalaxies: seyferten
dc.subjectNucleo galaticopt_BR
dc.subjectGalaxias seyfertpt_BR
dc.subjectLine: profilesen
dc.titleShort timescale variations of the Hα double-peaked profile of the nucleus of NGC 1097pt_BR
dc.typeArtigo de periódicopt_BR
dc.identifier.nrb000869119pt_BR
dc.type.originEstrangeiropt_BR


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