Fundamental vibrational transition of CO during the outburst of EX Lupi in 2008
AuthorGoto, Miwa; Regály, Zs; Dullemond, Cornelis P.; Van Den Ancker, Mario E.; Brown, Joanna M.; Carmona, Andrés; Pontoppidan, Klaus M.; Ábrahám, Péter; Blake, Geoffrey A.; Fedele, Davide; Henning, Th H E; Juhász, Attila; Kóspál, Ågnes; Mosoni, László; Sicilia-Aguilar, Aurora; Terada, Hiroshi; Van Boekel, Roy; Van Dishoeck, Ewine F.; Usuda, Tomonori
EntityUAM. Departamento de Física Teórica
PublisherThe American Astronomical Society.
10.1088/0004-637X/728/1/5The Astrophysical Journal 728.1 (2011):5
ISSN0004-637X (print); 1538-4357 (online)
Funded byZs.R. was partly supported by MO¨ B/DAAD-841 Mobility Grant. A.C. acknowledges support from a Swiss National Science Foundation grant (PP002–110504). P.A´ .Acknowledges support from the grant OTKA K62304 of the Hungarian Scientific Research Fund. The research of A´ .K. is supported by the Netherlands Organization for Scientific Research. A.S.A. acknowledges support from the Deutsche Forschungsgemeinschaft (DFG) grant SI 1486/1-1.
SubjectsCircumstellar matter; Herbig Ae/Be; Protoplanetary disks; Stars: formation; Stars: individual (EX Lupi); Stars: pre-main sequence; Stars: variables: T Tauri; Física
NoteThe Astrophysical Journal 728.1 (2011):5 reproduced by permission of the AAS
Rights© 2011. The American Astronomical Society.
We report monitoring observations of the T Tauri star EX Lupi during its outburst in 2008 in the CO fundamental band at 4.6-5.0 μm. The observations were carried out at the Very Large Telescope and the Subaru Telescope at six epochs from 2008 April to August, covering the plateau of the outburst and the fading phase to a quiescent state. The line flux of CO emission declines with the visual brightness of the star and the continuum flux at 5 μm, but composed of two subcomponents that decay with different rates. The narrow-line emission (50 km s-1 in FWHM) is near the systemic velocity of EX Lupi. These emission lines appear exclusively in υ = 1-0. The line widths translate to a characteristic orbiting radius of 0.4 AU. The broad-line component (FWZI ∼ 150 km s-1) is highly excited up to υ ≤ 6. The line flux of the component decreases faster than the narrow-line emission. Simple modeling of the line profiles implies that the broad-line emitting gas is orbiting around the star at 0.04-0.4 AU. The excitation state, the decay speed of the line flux, and the line profile indicate that the broad-line emission component is physically distinct from the narrow-line emission component, and more tightly related to the outburst event.
Google Scholar:Goto, Miwa - Regály, Zs - Dullemond, Cornelis P. - Van Den Ancker, Mario E. - Brown, Joanna M. - Carmona, Andrés - Pontoppidan, Klaus M. - Ábrahám, Péter - Blake, Geoffrey A. - Fedele, Davide - Henning, Th H E - Juhász, Attila - Kóspál, Ågnes - Mosoni, László - Sicilia-Aguilar, Aurora - Terada, Hiroshi - Van Boekel, Roy - Van Dishoeck, Ewine F. - Usuda, Tomonori
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Juhász, Attila; Dullemond, Cornelis P.; Van Boekel, Roy; Bouwman, Jeroen; Ábrahám, Péter; Acosta-Pulido, José Antonio; Kóspál, Ågnes; Sicilia-Aguilar, Aurora; Jones, Anthony P.; Moór, Attila; Mosoni, László; Regály, Zs; Szokoly, Gyula P.; Sipos, Nikoletta; Henning, Th.
Kóspál, Ågnes; Ábrahám, Péter; Goto, Miwa; Regály, Zs; Dullemond, Cornelis P.; Henning, Th H E; Juhász, Attila; Sicilia-Aguilar, Aurora; Van Den Ancker, Mario E.
Optical spectroscopy of EX Lupi during quiescence and outburst: Infall, wind, and dynamics in the accretion flow Sicilia-Aguilar, Aurora; Kóspál, Ågnes; Setiawan, Johny; Ábrahám, Péter; Dullemond, Cornelis; Eiroa, Carlos; Goto, Miwa; Henning, Th.; Juhász, Attila