Interaction between a pulsating jet and a surrounding disk wind

Tabone, B.; Raga, A. C.; Cabrit, S.; Forêts, G. Pineau des

doi:10.1051/0004-6361/201732031

Cited by 24 publications

(23 citation statements)

References 29 publications

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“…Now with new ALMA observations about two times deeper and a spatial resolution of ∼ 13 au (0 ′′ . 033), we retrieve additional SO emission structures reconciling the above seemingly contradictory results, providing a confirmation for an extended disk wind as well as the first evidence of jet-disk wind interaction first predicted by Tabone et al (2018). This interaction provides unique first clues to the unknown magnetic field strength and distribution in young protostellar disks.…”

Section: Introductionsupporting

confidence: 81%

“…The jet from the innermost disk (r 0 ∼ 0.05 − 0.20 au) drives large bow shocks interacting with the extended disk wind and producing a cavity, with the thin SO shell forming its boundary. These data are thus providing the first unambiguous evidence for the theoretically predicted interaction between a time-variable jet and an outer disk wind (Tabone et al 2018). Resolving such an interaction is crucial for the proper interpretation and modeling of less well resolved disk wind candidates.…”

Section: Discussionmentioning

confidence: 57%

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First Detection of Interaction between a Magnetic Disk Wind and an Episodic Jet in a Protostellar System

Lee,

Tabone,

Cabrit

et al. 2021

Preprint

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Rotating outflows from protostellar disks might trace extended magnetohydrodynamic (MHD) disk winds (DWs), providing a solution to the angular momentum problem in disk accretion for star formation. In the jet system HH 212, a rotating outflow was detected in SO around an episodic jet detected in SiO.Here we spatially resolve this SO outflow into three components: a collimated jet aligned with the SiO jet, the wide-angle disk outflow, and an evacuated cavity in between created by a large jet-driven bowshock. Although it was theoretically predicted before, it is the first time that such a jet-DW interaction is directly observed and resolved, and it is crucial for the proper interpretation and modeling of non-resolved DW candidates. The resolved kinematics and brightness distribution both support the wide-angle outflow to be an extended MHD DW dominating the local angular momentum extraction out to 40 au, but with an inner launching radius truncated to ∼ > 4 au. Inside 4 au, where the DW may not exist, the magneto-rotational instability (MRI) might be transporting angular momentum outwards. The jet-DW interaction in HH 212, potentially present in other similar systems, opens an entirely new avenue to probe the large-scale magnetic field in protostellar disks.

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Section: Introductionsupporting

confidence: 81%

Section: Discussionmentioning

confidence: 57%

First Detection of Interaction between a Magnetic Disk Wind and an Episodic Jet in a Protostellar System

Lee,

Tabone,

Cabrit

et al. 2021

Preprint

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“…gas tracing the interaction of the wind with the jet (Tabone et al 2018), also seen in DG Tau B and HH212 (de Valon et al 2020;Lee et al 2021). This perturbation of the wind by a fast jet might bias the determination of the angular momentum extracted by the wind or the launching region.…”

Section: Observational Constraints Of Mhd Disc Windsmentioning

confidence: 96%

Secular evolution of MHD wind-driven discs: analytical solutions in the expanded α-framework

Tabone

Rosotti

Cridland

et al. 2021

Monthly Notices of the Royal Astronomical Society

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The evolution of protoplanetary discs and the related process of planet formation is regulated by angular momentum transport and mass-loss processes. Over the past decade, the paradigm of viscosity has been challenged and MHD disc winds appear as a compelling scenario to account for disc accretion. In this work, we aim to construct the equivalent of the widely used analytical description of viscous evolution for the MHD wind case. The transport of angular momentum and mass induced by the wind is parameterized by an α-like parameter and by the magnetic lever arm parameter λ. Extensions of the paradigmatic Lynden-Bell and Pringle similarity solutions to the wind case are presented. We show that wind-driven accretion leads to a steeper decrease in the disc mass and accretion rate than in viscous models due to the absence of disc spreading. If the decline of the magnetic field strength is slower than that of the gas surface density, the disc is dispersed after a finite time. The evolution of the disc in the $\dot{M}_*-M_{D}$ plane is sensitive to the wind and turbulence parameters. A disc population evolving under the action of winds can exhibit a correlation between $\dot{M}_*$ and MD depending on the initial conditions. The simplified framework proposed in this work opens to a new avenue to test the effectiveness of wind-driven accretion from the observed disc demographics and constitutes an important step to include wind-driven accretion in planet population synthesis models.

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“…1). Tabone et al (2018) discuss jet-wind interactions and how a disk-wind may refill v-shaped regions emptied by jet bowshocks. Located north-west of the jet may be a such a bow-shock cavity which the disk-wind currently has not filled.…”

Section: Bow Shocks and Jet-wind Interactionsmentioning

confidence: 99%

ALMA resolves the remarkable molecular jet and rotating wind in the extremely radio-quiet galaxy NGC 1377

Aalto

Falstad

Müller

et al. 2020

A&A

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Submillimetre and millimetre line and continuum observations are important in probing the morphology, column density, and dynamics of the molecular gas and dust around obscured active galactic nuclei (AGNs) and their mechanical feedback. With very high-resolution (0.″02 × 0.″03 (2 × 3 pc)) ALMA 345 GHz observations of CO 3–2, HCO+ 4–3, vibrationally excited HCN 4–3 ν2 = 1f, and continuum we have studied the remarkable, extremely radio-quiet, molecular jet and wind of the lenticular galaxy NGC 1377. The outflow structure is resolved, revealing a 150 pc long, clumpy, high-velocity (∼600 km s−1), collimated molecular jet where the molecular emission is emerging from the spine of the jet with an average diameter of 3–7 pc. The jet widens to 10–15 pc about 25 pc from the centre, which is possibly due to jet-wind interactions. A narrow-angle (50°–70°), misaligned and rotating molecular wind surrounds the jet, and both are enveloped by a larger-scale CO-emitting structure at near-systemic velocity. The jet and narrow wind have steep radial gas excitation gradients and appear turbulent with high gas dispersion (σ > 40 km s−1). The jet shows velocity reversals that we propose are caused by precession, or more episodic directional changes. We discuss the mechanisms powering the outflow, and we find that an important process for the molecular jet and narrow wind is likely magneto-centrifugal driving. In contrast, the large-scale CO-envelope may be a slow wind, or cocoon that stems from jet-wind interactions. An asymmetric, nuclear r ∼ 2 pc dust structure with a high inferred molecular column density N(H2) ≃1.8 × 1024 cm−2 is detected in continuum and also shows compact emission from vibrationally excited HCN. The nuclear dust emission is hot (Td > 180 K) and its luminosity is likely powered by a buried AGN. The lopsided structure appears to be a warped disk, which is responsible for a significant part of the nuclear obscuration and possibly formed as a result of uneven gas inflows. The dynamical mass inside r = 1.4 pc is estimated to 9−3+2 × 106 M⊙, implying that the supermassive black hole (SMBH) has a high mass with respect to the stellar velocity dispersion of NGC 1377. We suggest that the SMBH of NGC 1377 is currently in a state of moderate growth, at the end of a more intense phase of accretion and also evolving from a state of more extreme nuclear obscuration. The nuclear growth may be fuelled by low-angular momentum gas inflowing from the gas ejected in the molecular jet and wind. Such a feedback-loop of cyclic outflows and central accretion could explain why there is still a significant reservoir of molecular gas in this ageing, lenticular galaxy. A feedback-loop would be an effective process in growing the nuclear SMBH and thus would constitute an important phase in the evolution of NGC 1377. This also invites new questions as to SMBH growth processes in obscured, dusty galaxies.

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Interaction between a pulsating jet and a surrounding disk wind

Cited by 24 publications

References 29 publications

First Detection of Interaction between a Magnetic Disk Wind and an Episodic Jet in a Protostellar System

First Detection of Interaction between a Magnetic Disk Wind and an Episodic Jet in a Protostellar System

Secular evolution of MHD wind-driven discs: analytical solutions in the expanded α-framework

ALMA resolves the remarkable molecular jet and rotating wind in the extremely radio-quiet galaxy NGC 1377

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