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

Lee, Chin-Fei; Tabone, B.; Cabrit, S.; Codella, C.; Podio, L.; Ferreira, Jonathan; Jacquemin-Ide, Jonatan

doi:10.3847/2041-8213/abda38

Cited by 30 publications

(37 citation statements)

References 37 publications

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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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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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“…Such features in outflows have been reported, for instance, for the Source I in Orion Kleinmann-Low (Hirota et al 2017), L483 , NGC 1333 IRAS 4C (Zhang et al 2018), andHH 212 (Tabone et al 2020;Lee et al 2021). They are interpreted as the rotating motion of the outflows, where the outflow blows nearly perpendicular to the line of sight.…”

Section: Rotating Motion Of the Outflowmentioning

confidence: 65%

“…Morphologically speaking, the SO emission seems to trace the outflow, or its cavity wall instead, although it may also trace the surface of a flared envelope gas. In fact, the SO emission has been reported to trace a disk wind in another protostellar system (HH 212; Tabone et al 2017;Lee et al 2021).…”

Section: Rotating Motion Of the Outflowmentioning

confidence: 99%

Rotating Motion of the Outflow of IRAS 16293-2422 A1 at its Origin Point near the Protostar

Oya,

Watanabe,

López-Sepulcre

et al. 2021

Preprint

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The Class 0 protostar IRAS 16293-2422 Source A is known to be a binary system (A1 and A2) or even a multiple system, which processes a complex outflow structure. We have observed this source in the C 34 S, SO, and OCS lines at 3.1 mm with the Atacama Large Millimeter/submillimeter Array (ALMA). A substructure of this source is traced by our high angular-resolution observation (0. ′′ 12; 20 au) of the continuum emission. The northwest-southeast (NW-SE) outflow on a 2 ′′ scale is detected in the SO (J N = 2 2 -1 1 ) line. Based on the morphology of the SO distribution, this bipolar outflow structure seems to originate from the protostar A1 and its circumstellar disk, or the circummultiple structure of Source A. The rotation motion of the NW-SE outflow is detected in the SO and OCS emissions. We evaluate the specific angular momentum of the outflowing gas to be (8.6 − 14.3) × 10 −4 km s −1 pc. If the driving source of this outflow is the protostar A1 and its circumstellar disk, it can be a potential mechanism to extract the specific angular momentum of the disk structure. These results can be a hint for the outflow launching mechanism in this source. Furthermore, they provide us with an important clue to resolve the complicated structure of IRAS 16293-2422 Source A.

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“…The base velocity of the ejected particles corresponds to the Keplerian velocity at twice the stellar radius (ii). To produce a two component outflow, combining a low-velocity, wide-angle wind (Louvet et al 2018;Zhang et al 2019;Pascucci et al 2020;Lee et al 2021) and a high-velocity jet, we modulate the base velocity with the angular distribution function derived by Matzner & McKee (1999) (see Appendix B for more details). Additionally, we add a rotational velocity component (Eq.…”

Section: Feedback Modelsmentioning

confidence: 99%

Protostellar Outflows: a window to the past

Rohde,

Walch,

Seifried

et al. 2022

Preprint

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During the early phases of low-mass star formation, episodic accretion causes the ejection of high-velocity outflow bullets, which carry a fossil record of the driving protostar's accretion history. We present 44 SPH simulations of 1 M cores, covering a wide range of initial conditions, and follow the cores for five free-fall times. Individual protostars are represented by sink particles, and the sink particles launch episodic outflows using a subgrid model. The O algorithm is used to identify individual episodic bullets within the outflows. The parameters of the overall outflow and the individual bullets are then used to estimate the age and energetics of the outflow, and the accretion events that triggered it; and to evaluate how reliable these estimates are, if observational uncertainties and selection effects (like inclination) are neglected. Of the commonly used methods for estimating outflow ages, it appears that those based on the length and speed of advance of the lobe are the most reliable in the early phases of evolution, and those based on the width of the outflow cavity and the speed of advance are most reliable during the later phases. We describe a new method that is almost as accurate as these methods, and reliable throughout the evolution. In addition we show how the accretion history of the protostar can be accurately reconstructed from the dynamics of the bullets if each lobe contains at least two bullets. The outflows entrain about ten times more mass than originally ejected by the protostar.

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

Cited by 30 publications

References 37 publications

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

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

Rotating Motion of the Outflow of IRAS 16293-2422 A1 at its Origin Point near the Protostar

Protostellar Outflows: a window to the past

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