Disk-driven rotating bipolar outflow in Orion Source I

Hirota, Tomoya; Machida, Masahiro N.; Matsushita, Yuko; Motogi, Kazuhito; Matsumoto, Naoko; Kim, Mi Kyoung; Burns, Ross; Honma, Mareki

doi:10.1038/s41550-017-0146

Cited by 143 publications

(170 citation statements)

References 29 publications

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“…Thus, no high-velocity component ( ∼ > 100 km s −1 ) appears in the observations. In addition, Hirota et al (2017) pointed out that they could find no evidence of the high-velocity component (or jet) in their observation of Orion KL source I. Thus, we have no clear evidence of the high-velocity jet, which is sometimes observed around the low-mass protostar, driven from the high-mass protostar.…”

Section: Spatial Resolution In Simulationsmentioning

confidence: 87%

“…Very recently, using ALMA, Hirota et al (2017) observed high-mass protostar Orion KL source I resolving the circumstellar disk and outflow and showed clear evidence of the MHD disk wind, in which the rotations of both disk and outflow were confidently identified (see also Greenhill et al 2013;Hirota et al 2016a,b). Note that they could not find any sign of a high-velocity jet, and specifically excluded other outflow driving mechanisms, such as entrainment and radiation-driven mechanisms.…”

Section: Introductionmentioning

confidence: 99%

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Massive outflows driven by magnetic effects – II. Comparison with observations

Matsushita

Sakurai

Hosokawa

et al. 2018

Monthly Notices of the Royal Astronomical Society

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The driving mechanism of massive outflows observed in high-mass star-forming regions is investigated using three-dimensional magnetohydrodynamics (MHD) and protostellar evolution calculations. In our previous paper, we showed that the mass outflow rate depends strongly on the mass accretion rate onto the circumstellar disk around a highmass protostar, and massive outflows may be driven by the magnetic effect in highmass star-forming cores. In the present study, in order to verify that the MHD disk wind is the primary driving mechanism of massive outflows, we quantitatively compare outflow properties obtained through simulations and observations. Since the outflows obtained through simulations are slightly younger than those obtained through observations, the time-integrated quantities of outflow mass, momentum, and kinetic energy are slightly smaller than those obtained through observations. On the other hand, time-derivative quantities of mass ejection rate, outflow momentum flux, and kinetic luminosity obtained through simulations are in very good agreement with those obtained through observations. This indicates that the MHD disk wind greatly contributes to the massive outflow driving from high-mass protostars, and the magnetic field might significantly control the high-mass star formation process.

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Section: Spatial Resolution In Simulationsmentioning

confidence: 87%

Section: Introductionmentioning

confidence: 99%

Massive outflows driven by magnetic effects – II. Comparison with observations

Matsushita

Sakurai

Hosokawa

et al. 2018

Monthly Notices of the Royal Astronomical Society

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“…Almost all of the known circumstellar systems in High-Mass star-formation are in a nearly edgeon orientation (e.g., Patel et al 2005;Torrelles et al 2007;Matthews et al 2010;Carrasco-González et al 2012;Sánchez-Monge et al 2013;Beltrán et al 2014;Cesaroni et al 2014;Hirota et al 2016Hirota et al , 2017Plambeck & Wright 2016). This bias is simply due to their easy identification even with limited angular resolution, based on the velocity gradient of rotating disks and/or envelopes.…”

Section: Introductionmentioning

confidence: 99%

“…Such a structure suggests a hierarchical fragmentation and accretion process around a High-Mass young stellar object (HMYSO). The innermost compact disks (< 100 au) were resolved in some very high-resolution observations (e.g., Kraus et al 2010;Hirota et al 2014Hirota et al , 2016Hirota et al , 2017Plambeck & Wright 2016).…”

Section: Introductionmentioning

confidence: 99%

A Face-on Accretion System in High-mass Star Formation: Possible Dusty Infall Streams within 100 AU

Motogi

Hirota

Saito

et al. 2017

ApJ

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We report on interferometric observations of a face-on accretion system around the High-Mass young stellar object, G353.273+0.641. The innermost accretion system of 100 au radius was resolved in a 45 GHz continuum image taken with the Jansky-Very Large Array. Our spectral energy distribution analysis indicated that the continuum could be explained by optically thick dust emission. The total mass of the dusty system is ∼ 0.2 M ⊙ at minimum and up to a few M ⊙ depending on the dust parameters. 6.7 GHz CH 3 OH masers associated with the same system were also observed with the Australia Telescope Compact Array. The masers showed a spiral-like, non-axisymmetric distribution with a systematic velocity gradient. The line-of-sight velocity field is explained by an infall motion along a parabolic streamline that falls onto the equatorial plane of the face-on system. The streamline is quasi-radial and reaches the equatorial plane at a radius of 16 au. This is clearly smaller than that of typical accretion disks in High-Mass star formation, indicating that the initial angular momentum was very small, or the CH 3 OH masers selectively trace accreting material that has small angular momentum. In the former case, the initial specific angular momentum is estimated to be 8 × 10 20 (M * /10 M ⊙ ) 0.5 cm 2 s −1 , or a significant fraction of the initial angular momentum was removed outside of 100 au. The physical origin of such a streamline is still an open question and will be constrained by the higher-resolution (∼ 10 mas) thermal continuum and line observations with ALMA long baselines.

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“…Louvet et al 2016) because of the limited spectral resolution and wavelength accuracy in the optical. Sub/mm interferometric observations do not have this limitation and have provided clear evidence for flow rotation in several younger protostellar sources, although at lower speeds than the axial jets, suggesting ejection from ∼5−25 au in the disk (Launhardt et al 2009;Matthews et al 2010;Bjerkeli et al 2016; Hirota et al 2017). Thermo-chemical models show that dusty DWs launched from this range of radii would indeed remain molecular despite magnetic acceleration (Panoglou et al 2012).…”

Section: Introductionmentioning

confidence: 99%

ALMA discovery of a rotating SO/SO₂ flow in HH212

Tabone

Cabrit

Bianchi

et al. 2017

A&A

140

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We wish to constrain the possible contribution of a magnetohydrodynamic disk wind (DW) to the HH212 molecular jet. We mapped the flow base with ALMA Cycle 4 at 0 . 13 ∼ 60 au resolution and compared these observations with synthetic DW predictions. We identified, in SO/SO 2 , a rotating flow that is wider and slower than the axial SiO jet. The broad outflow cavity seen in C 34 S is not carved by a fast wide-angle wind but by this slower agent. Rotation signatures may be fitted by a DW of a moderate lever arm launched out to ∼40 au with SiO tracing dust-free streamlines from 0.05−0.3 au. Such a DW could limit the core-to-star efficiency to ≤50%.

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Disk-driven rotating bipolar outflow in Orion Source I

Cited by 143 publications

References 29 publications

Massive outflows driven by magnetic effects – II. Comparison with observations

Massive outflows driven by magnetic effects – II. Comparison with observations

A Face-on Accretion System in High-mass Star Formation: Possible Dusty Infall Streams within 100 AU

ALMA discovery of a rotating SO/SO₂ flow in HH212

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Disk-driven rotating bipolar outflow in Orion Source I

Cited by 143 publications

References 29 publications

Massive outflows driven by magnetic effects – II. Comparison with observations

Massive outflows driven by magnetic effects – II. Comparison with observations

A Face-on Accretion System in High-mass Star Formation: Possible Dusty Infall Streams within 100 AU

ALMA discovery of a rotating SO/SO2 flow in HH212

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ALMA discovery of a rotating SO/SO₂ flow in HH212