A protostellar system fed by a streamer of 10,500 au length

Pineda, Jaime E.; Segura-Cox, Dominique; Caselli, P.; Cunningham, Nichol; Zhao, Bo; Schmiedeke, A.; Maureira, María José; Neri, R.

doi:10.1038/s41550-020-1150-z

Cited by 122 publications

(147 citation statements)

References 56 publications

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“…We report the presence of accretion streamers (already observed in the low-mass regime, see Pineda et al 2020), which are reminiscent of the accretion channels found by Seifried et al (2015) and the bridges in the study of Kuffmeier et al (2019) and Kuffmeier et al (2020). In agreement with Seifried et al (2015), ram pressure dominates magnetic pressure, but we further show that magnetic pressure is also dominated by thermal pressure.…”

Section: Comparison With Previous Worksupporting

confidence: 77%

Collapse of turbulent massive cores with ambipolar diffusion and hybrid radiative transfer

Mignon-Risse

González

Commerçon

et al. 2021

A&A

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Context. Massive stars form in magnetized and turbulent environments and are often located in stellar clusters. The accretion and outflows mechanisms associated with forming massive stars and the origin of the stellar multiplicity of their system are poorly understood. Aims. We study the effect of magnetic fields and turbulence on the accretion mechanism of massive protostars and their multiplicity. We also focus on disk formation as a prerequisite for outflow launching. Methods. We present a series of four radiation-magnetohydrodynamical simulations of the collapse of a massive magnetized, turbulent core of 100 M⊙ with the adaptive-mesh-refinement code RAMSES, including a hybrid radiative transfer method for stellar irradiation and ambipolar diffusion. We varied the Mach and Alfvénic Mach numbers to probe sub- and super-Alfvénic turbulence and sub- and supersonic turbulence regimes. Results. Sub-Alfvénic turbulence leads to single stellar systems, and super-Alfvénic turbulence leads to binary formation from disk fragmentation following the collision of spiral arms, with mass ratios of 1.1–1.6 and a separation of several hundred AU that increases with initial turbulent support and with time. In these runs, infalling gas reaches the individual disks through a transient circumbinary structure. Magnetically regulated, thermally dominated (plasma beta β > 1) Keplerian disks form in all runs, with sizes 100–200 AU and masses 1–8 M⊙. The disks around primary and secondary sink particles have similar properties. We obtain mass accretion rates of ~10−4 M⊙ yr−1 onto the protostars and observe higher accretion rates onto the secondary stars than onto their primary star companion. The primary disk orientation is found to be set by the initial angular momentum carried by turbulence rather than by magnetic fields. Even without turbulence, axisymmetry and north–south symmetry with respect to the disk plane are broken by the interchange instability and thermally dominated streamers, respectively. Conclusions. Small (≲300 AU) massive protostellar disks such as those that are frequently observed today can so far only be reproduced in the presence of (moderate) magnetic fields with ambipolar diffusion, even in a turbulent medium. The interplay between magnetic fields and turbulence sets the multiplicity of stellar clusters. A plasma beta β > 1 is a good indicator for distinguishing streamers and individual disks from their surroundings.

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Section: Comparison With Previous Worksupporting

confidence: 77%

Collapse of turbulent massive cores with ambipolar diffusion and hybrid radiative transfer

Mignon-Risse

González

Commerçon

et al. 2021

A&A

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“…These include emission from an envelope/accretion streamer or outflow cavity, or perturbations by an unseen companion. This arc is similar to the streamer that is feeding material from the local environment onto Per-emb-2 (Pineda et al 2020), [BHB2007] 1 (Alves et al 2020), SU Aur (Ginski et al 2021), and, on a smaller scale, HL Tau (Yen et al 2019). However, what is unique about the emission around [MGM2012] 512 is that it is detected in the continuum.…”

Section: Structure Around [Mgm2012] 512mentioning

confidence: 86%

Herschel Observations of Protoplanetary Disks in Lynds 1641*

Grant

Espaillat

Megeath

et al. 2018

ApJ

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We analyze Herschel Space Observatory observations of 104 young stellar objects with protoplanetary disks in the ∼1.5 Myr star-forming region Lynds 1641 (L1641) within the Orion A Molecular Cloud. We present spectral energy distributions from the optical to the far-infrared including new photometry from the Herschel Photodetector Array Camera and Spectrometer (PACS) at 70 µm. Our sample, taken as part of the Herschel Orion Protostar Survey, contains 24 transitional disks, eight of which we identify for the first time in this work. We analyze the full disks with irradiated accretion disk models to infer dust settling properties. Using forward modeling to reproduce the observed n K S −[70] index for the full disk sample, we find the observed disk indices are consistent with models that have depletion of dust in the upper layers of the disk relative to the midplane, indicating significant dust settling. We perform the same analysis on full disks in Taurus with Herschel data and find that Taurus is slightly more evolved, although both samples show signs of dust settling. These results add to the growing literature that significant dust evolution can occur in disks by ∼1.5 Myr.

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“…Nevertheless, the observed SO emission is consistent with the geometry seen in the H 2 CO emission. The morphology near the protostar in the H 2 CO and C 18 O emission and the apparent symmetry in the SO emission strongly suggest that these features are part of an outflow structure, rather than a structure formed from gas accreting toward the protostar as seen in the source Per-emb-2 by Pineda et al (2020).…”

Section: Linear Structure In the Northwest To Southeast Directionmentioning

confidence: 95%

FAUST. II. Discovery of a Secondary Outflow in IRAS 15398−3359: Variability in Outflow Direction during the Earliest Stage of Star Formation?

Okoda

Oya

Francis

et al. 2021

ApJ

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We have observed the very low-mass Class 0 protostar IRAS 15398−3359 at scales ranging from 50 to 1800 au, as part of the Atacama Large Millimeter/Submillimeter Array Large Program FAUST. We uncover a linear feature, visible in H 2 CO, SO, and C 18 O line emission, which extends from the source in a direction almost perpendicular to the known active outflow. Molecular line emission from H 2 CO, SO, SiO, and CH 3 OH further reveals an arc-like structure connected to the outer end of the linear feature and separated from the protostar, IRAS 15398−3359, by 1200 au. The arc-like structure is blueshifted with respect to the systemic velocity. A velocity gradient of 1.2 km s −1 over 1200 au along the linear feature seen in the H 2 CO emission connects the protostar and the arc-like structure

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A protostellar system fed by a streamer of 10,500 au length

Cited by 122 publications

References 56 publications

Collapse of turbulent massive cores with ambipolar diffusion and hybrid radiative transfer

Collapse of turbulent massive cores with ambipolar diffusion and hybrid radiative transfer

Herschel Observations of Protoplanetary Disks in Lynds 1641*

FAUST. II. Discovery of a Secondary Outflow in IRAS 15398−3359: Variability in Outflow Direction during the Earliest Stage of Star Formation?

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