L’UDF et l’Europe

Manigand, Christine

doi:10.4000/books.pur.114848

Cited by 1 publication

(2 citation statements)

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“…However, hints of a shift were also seen in high-resolution VLA continuum observations at 42 GHz reported by Rodríguez et al (2005)a n dH e r n ández- Gómez et al (2019b), unlike what is seen in the case of the highly inclined disc in HH212 (Lin et al 2021). Furthermore, the line emission from complex organic molecules from the ALMA-PILS survey also appears to show a peak shifted to the west (Calcutt et al 2018a, b;Manigand et al 2020Manigand et al , 2021. Likewise, the source does not show a significant gradient indicative of rotation in previous ALMA line observations from 100 au down to 70 au scales.…”

Section: Continuum Observations At 13 and 3 MMmentioning

confidence: 82%

“…1, the minimum value is fairly close to the centre of the overall structure, while the peak of the dust continuum emission is not. This difference may be due to the continuum peak tracing instead the position of a hot structure close to the protostar and not the protostar itself, which would also be supported by the asymmetric distribution of the complex organic molecule emission (Calcutt et al Manigand et al 2020Manigand et al , 2021. This asymmetry could also be associated with asymmetric accretion from the envelope on to the disc, based on the previous detection of infalling material in source B (Pineda et al 2012;Z a p a t ae ta l .2013).…”

Section: The Origin Of the Observed Asymmetrymentioning

confidence: 99%

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The young protostellar disc in IRAS 16293−2422 B is hot and shows signatures of gravitational instability

Zamponi

Maureira

Zhao

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Deeply embedded protostars are actively fed from their surrounding envelopes through their protostellar disk. The physical structure of such early disks might be different from that of more evolved sources due to the active accretion. We present 1.3 and 3 mm ALMA continuum observations at resolutions of 6.5 au and 12 au respectively, towards the Class 0 source IRAS 16293-2422 B. The resolved brightness temperatures appear remarkably high, with Tb > 100 K within ∼30 au and Tb peak over 400 K at 3 mm. Both wavelengths show a lopsided emission with a spectral index reaching values less than 2 in the central ∼ 20 au region. We compare these observations with a series of radiative transfer calculations and synthetic observations of magnetohydrodynamic and radiation hydrodynamic protostellar disk models formed after the collapse of a dense core. Based on our results, we argue that the gas kinematics within the disk may play a more significant role in heating the disk than the protostellar radiation. In particular, our radiation hydrodynamic simulation of disk formation, including heating sources associated with gravitational instabilities, is able to generate the temperatures necessary to explain the high fluxes observed in IRAS 16293B. Besides, the low spectral index values are naturally reproduced by the high optical depth and high inner temperatures of the protostellar disk models. The high temperatures in IRAS 16293B imply that volatile species are mostly in the gas phase, suggesting that a self-gravitating disk could be at the origin of a hot corino.

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