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- W2892086275 abstract "The FU Ori-type young stellar objects are characterized by a sudden increase in luminosity by 1$-$2 orders of magnitude, followed by slow return to the pre-outburst state on timescales of $sim$10$-$100 yr. The outburst strongly affects the entire disk, changing its thermal structure and radiation field. In this paper, using a detailed physical-chemical model we study the impact of the FU Ori outburst on the disk chemical inventory. Our main goal is to identify gas-phase molecular tracers of the outburst activity that could be observed after the outburst with modern telescopes such as ALMA and NOEMA. We find that the majority of molecules experience a considerable increase in the total disk gas-phase abundances due to the outburst, mainly due to the sublimation of their ices. Their return to the pre-outburst chemical state takes different amounts of time, from nearly instantaneous to very long. Among the former ones we identify CO, NH$_3$, C$_2$H$_6$, C$_3$H$_4$, etc. Their abundance evolution tightly follows the luminosity curve. For CO the abundance increase does not exceed an order of magnitude, while for other tracers the abundances increase by 2$-$5 orders of magnitude. Other molecules like H$_2$CO and NH$_2$OH have longer retention timescales, remaining in the gas phase for $sim10-10^3$ yr after the end of the outburst. Thus H$_2$CO could be used as an indicator of the previous outbursts in the post-outburst FU Ori systems. We investigate the corresponding time-dependent chemistry in detail and present the most favorable transitions and ALMA configurations for future observations." @default.
- W2892086275 created "2018-09-27" @default.
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- W2892086275 date "2018-10-10" @default.
- W2892086275 modified "2023-10-15" @default.
- W2892086275 title "Chemical Signatures of the FU Ori Outbursts" @default.
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- W2892086275 doi "https://doi.org/10.3847/1538-4357/aadfd9" @default.
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