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• W3101268896 endingPage "A87" @default.
• W3101268896 startingPage "A87" @default.
• W3101268896 abstract "Mass loss from jets and winds is a key ingredient in the evolution of accretion discs in young stars. While slow winds have been recently extensively studied in T Tauri stars, little investigation has been devoted on the occurrence of high velocity jets and on how the two mass-loss phenomena are connected with each other, and with the disc mass accretion rates. In this framework, we have analysed the [O i ]6300 Å line in a sample of 131 young stars with discs in the Lupus, Chamaeleon and σ Orionis star forming regions. The stars were observed with the X-shooter spectrograph at the Very Large Telescope and have mass accretion rates spanning from 10 -12 to 10 -7 M ⊙ yr -1 . The line profile was deconvolved into a low velocity component (LVC, | V r | < 40 km s -1 ) and a high velocity component (HVC, | V r | > 40 km s -1 ), originating from slow winds and high velocity jets, respectively. The LVC is by far the most frequent component, with a detection rate of 77%, while only 30% of sources have a HVC. The fraction of HVC detections slightly increases (i.e. 39%) in the sub-sample of stronger accretors (i.e. with log ( L acc / L ⊙ ) >−3). The [O i ]6300 Å luminosity of both the LVC and HVC, when detected, correlates with stellar and accretion parameters of the central sources (i.e. L ∗ , M ∗ , L acc , Ṁ acc ), with similar slopes for the two components. The line luminosity correlates better (i.e. has a lower dispersion) with the accretion luminosity than with the stellar luminosity or stellar mass. We suggest that accretion is the main drivers for the line excitation and that MHD disc-winds are at the origin of both components. In the sub-sample of Lupus sources observed with ALMA a relationship is found between the HVC peak velocity and the outer disc inclination angle, as expected if the HVC traces jets ejected perpendicularly to the disc plane. Mass ejection rates ( Ṁ jet ) measured from the detected HVC [O i ]6300 Å line luminosity span from ~10 -13 to ~10 -7 M ⊙ yr -1 . The corresponding Ṁ jet / Ṁ acc ratio ranges from ~0.01 to ~0.5, with an average value of 0.07. However, considering the upper limits on the HVC, we infer a Ṁ jet / Ṁ acc ratio < 0.03 in more than 40% of sources. We argue that most of these sources might lack the physical conditions needed for an efficient magneto-centrifugal acceleration in the star-disc interaction region. Systematic observations of populations of younger stars, that is, class 0/I, are needed to explore how the frequency and role of jets evolve during the pre-main sequence phase. This will be possible in the near future thanks to space facilities such as the James Webb space telescope (JWST)." @default.
• W3101268896 created "2020-11-23" @default.
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• W3101268896 date "2018-01-01" @default.
• W3101268896 modified "2023-10-18" @default.
• W3101268896 title "Connection between jets, winds and accretion in T Tauri stars" @default.
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• W3101268896 doi "https://doi.org/10.1051/0004-6361/201730834" @default.
• W3101268896 hasPublicationYear "2018" @default.
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