The 2008 outburst of EX Lup-Silicate crystals in motion
EntidadUAM. Departamento de Física Teórica
EditorThe American Astronomical Society.
Fecha de edición2012-01-10
10.1088/0004-637X/744/2/118The Astrophysical Journal 744.2 (2012): 118
ISSN0004-637X (print); 1538-4357 (online)
Financiado porThe research of A.K. is supported by the Netherlands Organization for Scientific Research. The research of Zs.R. is supported by the “Lendület” Young Researcher Program of the Hungarian Academy of Sciences.
Versión del editorhttp://dx.doi.org/10.1088/0004-637X/744/2/118
MateriasAccretion; Accretion disks; Astrochemistry; Circumstellar matter; Infrared: stars; Protoplanetary disks; Stars: formation; Stars: individual (EX Lup); Física
NotaThe Astrophysical Journal 744.2 (2012): 118 reproduced by permission of the AAS
Derechos© 2012 The American Astronomical Society.
EXLup is the prototype of the EXor class of eruptive young stars. These objects show optical outbursts which are thought to be related to runaway accretion onto the star. In a previous study we observed in situ crystal formation in the disk of EXLup during its latest outburst in 2008, making the object an ideal laboratory to investigate circumstellar crystal formation and transport. This outburst was monitored by a campaign of ground-based and Spitzer Space Telescope observations. Here we modeled the spectral energy distribution (SED) of EXLup in the outburst from optical to millimeter wavelengths with a two-dimensional radiative transfer code. Our results showed that the shape of the SED at optical wavelengths was more consistent with a single-temperature blackbody than a temperature distribution. We also found that this single-temperature component emitted 80%-100% of the total accretion luminosity. We concluded that a thermal instability, the most widely accepted model of EXor outbursts, was likely not the triggering mechanism of the 2008 outburst of EXLup. Our mid-infrared Spitzer spectra revealed that the strength of all crystalline bands between 8 and 30μm increased right after the end of the outburst. Six months later, however, the crystallinity in the 10μm silicate feature complex decreased. Our modeling of the mid-infrared spectral evolution of EXLup showed that, although vertical mixing should be stronger during the outburst than in the quiescent phase, fast radial transport of crystals (e.g., by stellar/disk wind) was required to reproduce the observed mid-infrared spectra.
Google Scholar: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.
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