Substructure Formation in a Protostellar Disk of L1527 IRS

Nakatani, Riouhei; Liu, Hauyu Baobab; Ohashi, Satoshi; Zhang, Yichen; Hanawa, Tomoyuki; Chandler, Claire J.; Oya, Yoko; Sakai, Nami

doi:10.3847/2041-8213/ab8eaa

Cited by 38 publications

(74 citation statements)

References 38 publications

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“…Pinte et al 2020), by resolving key disk microphysics, our simulations reveal that the mechanism drives disk angular momentum transport and evolution is inher-ently non-smooth, and could result in additional, likely shallower disk substructures. Our magnetic mechanism might be a plausible explanation for substructures found in young Class 0/I disks, for which the evolutionary stage of these systems might be too early for Jupiter-mass planets to form (Sheehan & Eisner 2018;Nakatani et al 2020;Segura-Cox et al 2020;Sheehan et al 2020). For more matured, Class II disks, Jennings et al (2021) employed a superresolution technique and discovered finer disk substructures in the DSHARP disk samples, including shallow annular substructures in the outer disks.…”

Section: Implications For Annular Substructuresmentioning

confidence: 84%

“…While the planet scenario is especially compelling, it does not necessarily apply to all annular substructures observed. In particular, rings and gaps are also discovered during the embedded Class 0/I phase (Sheehan & Eisner 2018;Nakatani et al 2020;Segura-Cox et al 2020;Sheehan et al 2020) at early stages of disk formation, requiring either rapid formation of massive planets, or alternative, planet-free interpretations.…”

Section: Annular Substructuresmentioning

confidence: 99%

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Global three-dimensional simulations of outer protoplanetary discs with ambipolar diffusion

Cui

Bai

2021

Monthly Notices of the Royal Astronomical Society

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The structure and evolution of protoplanetary disks (PPDs) are largely governed by disk angular momentum transport, mediated by magnetic fields. In the most observable outer disk, ambipolar diffusion is the primary non-ideal magnetohydrodynamic(MHD) effect. In this work, we study the gas dynamics in outer PPDs by conducting a series of global 3D non-ideal MHD simulations with ambipolar diffusion and net poloidal magnetic flux, using the Athena++ MHD code, with resolution comparable to local simulations. Our simulations demonstrate the co-existence of magnetized disk winds and turbulence driven by the magneto-rotational instability (MRI). While MHD winds dominate disk angular momentum transport, the MRI turbulence also contributes significantly. We observe that magnetic flux spontaneously concentrate into axisymmetric flux sheets, leading to radial variations in turbulence levels, stresses, and accretion rates. Annular substructures arise as a natural consequence of magnetic flux concentration. The flux concentration phenomena show diverse properties with different levels of disk magnetization and ambipolar diffusion. The disk generally loses magnetic flux over time, though flux sheets could prevent the leak of magnetic flux in some cases. Our results demonstrate the ubiquity of disk annular substructures in weakly MRI turbulent outer PPDs, and imply a stochastic nature of disk evolution.

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Section: Implications For Annular Substructuresmentioning

confidence: 84%

Section: Annular Substructuresmentioning

confidence: 99%

Global three-dimensional simulations of outer protoplanetary discs with ambipolar diffusion

Cui

Bai

2021

Monthly Notices of the Royal Astronomical Society

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“…An example of the first explanation is that inner protostellar and/or protoplanetary disks, if present, can contribute to the decrease in the dust emissivity index, and the measured dust emissivity spectral indexes in those disks are usually β ≤ 1 (e.g. Beckwith & Sargent 1991;Ricci et al 2012;Pérez et al 2012;Ubach et al 2012;Miotello et al 2014;Bracco et al 2017;Liu 2019;Nakatani et al 2020).…”

Section: Dust Propertiesmentioning

confidence: 99%

ORion Alma New GEneration Survey (ORANGES)

Bouvier

López-Sepulcre

Ceccarelli

et al. 2021

A&A

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Context. The spectral energy distribution (SED) in the millimetre to centimetre range is an extremely useful tool for characterising the dust in protostellar envelopes as well as free-free emission from the protostar and outflow. Actually, the evolutionary status of solar-type protostars is often based on their SED in the near-infrared to millimetre range. In addition, the presence or absence of free-free emission can be considered an indicator of the source evolutionary stage (Class 0/I versus Class II/III). While many studies have been carried out towards low- and high-mass protostars, little exists so far about solar-type protostars in high-mass star-forming regions, which are likely to be representatives of the conditions where the Solar System was born. Aims. In this work, we focus on the embedded solar-type protostars in the Orion Molecular Cloud (OMC) 2 and 3 filaments, which are bounded by nearby HII regions and which are, therefore, potentially affected by the high-UV illumination of the nearby OB stars. We use various dust parameters to understand whether the small-scale structure (≤1000 au) and the evolutionary status of these solar-type protostars are affected by the nearby HII regions, as is the case for the large-scale (≤104 au) gas chemical composition. Methods. We used the Atacama Large (sub-)Millimeter Array (ALMA) in the 1.3 mm band (246.2 GHz) to image the continuum of 16 young (Class 0/I) OMC-2/3 solar-type protostars, with an angular resolution of 0.25″ (100 au). We completed our data with archival data from the ALMA and VLA VANDAM survey of Orion Protostars at 333 and 32.9 GHz, respectively, to construct the dust SED and extract the dust temperature, the dust emissivity spectral index, the envelope plus disk mass of the sources and to assess whether free-free emission is contaminating their dust SED in the centimetre range. Results. From the millimetre to centimetre range dust SED, we found low dust emissivity spectral indexes (β < 1) for the majority of our source sample and free-free emission towards only 5 of the 16 sample sources. We were also able to confirm or correct the evolutionary status of the source sample reported in the literature. Finally, we did not find any dependence of the source dust parameters on their location in the OMC-2/3 filament. Conclusions. Our results show that the small-scale dust properties of the embedded OMC-2/3 protostars are not affected by the high-UV illumination from the nearby HII regions and that the formation of protostars likely takes place simultaneously throughout the filament.

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Section: Dust Propertiesmentioning

confidence: 99%

ORion Alma New GEneration Survey (ORANGES) I. Dust continuum and free-free emission of OMC-2/3 filament protostars

Bouvier,

López-Sepulcre,

Ceccarelli

et al. 2021

Preprint

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Context. The spectral energy distribution (SED) in the millimetre to centimetre range is an extremely useful tool for characterising the dust in protostellar envelopes as well as free-free emission from the protostar and outflow. Actually, the evolutionary status of solar-type protostars is often based on their SED in the near-infrared to millimetre range. In addition, the presence or absence of free-free emission can be considered an indicator of the source evolutionary stage (Class 0/I versus Class II/III). While many studies have been carried out towards low-and high-mass protostars, little exists so far about solar-type protostars in high-mass star-forming regions, which are likely to be representatives of the conditions where the Solar System was born. Aims. In this work we focus on the embedded solar-type protostars in the Orion Molecular Cloud (OMC) 2 and 3 filaments, which are bounded by nearby HII regions and which are, therefore, potentially affected by the high-UV illumination of the nearby OB stars. We use various dust parameters to understand whether the small-scale structure (≤ 1000 au) and the evolutionary status of these solar-type protostars are affected by the nearby HII regions, as is the case for the large-scale (≤ 10 4 au) gas chemical composition. Methods. We used the Atacama Large (sub-)Millimeter Array (ALMA) in the 1.3 mm band (246.2 GHz) to image the continuum of 16 young (Class 0/I) OMC-2/3 solar-type protostars, with an angular resolution of 0.25 (100 au). We completed our data with archival data from the ALMA and VLA VANDAM survey of Orion Protostars at 333 and 32.9 GHz, respectively, to construct the dust SED and extract the dust temperature, the dust emissivity spectral index, the envelope plus disk mass of the sources and to assess whether free-free emission is contaminating their dust SED in the centimetre range. Results. From the millimetre to centimetre range dust SED, we found low dust emissivity spectral indexes (β < 1) for the majority of our source sample and free-free emission towards only 5 of the 16 sample sources. We were also able to confirm or correct the evolutionary status of the source sample reported in the literature. Finally, we did not find any dependence of the source dust parameters on their location in the OMC-2/3 filament. Conclusions. Our results show that the small-scale dust properties of the embedded OMC-2/3 protostars are not affected by the high-UV illumination from the nearby HII regions and that the formation of protostars likely takes place simultaneously throughout the filament.

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Substructure Formation in a Protostellar Disk of L1527 IRS

Cited by 38 publications

References 38 publications

Global three-dimensional simulations of outer protoplanetary discs with ambipolar diffusion

Global three-dimensional simulations of outer protoplanetary discs with ambipolar diffusion

ORion Alma New GEneration Survey (ORANGES)

ORion Alma New GEneration Survey (ORANGES) I. Dust continuum and free-free emission of OMC-2/3 filament protostars

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