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

Matsushita, Yuko; Sakurai, Yosito; Hosokawa, Takashi; Machida, Masahiro N.

doi:10.1093/mnras/stx3070

Cited by 28 publications

(23 citation statements)

References 76 publications

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“…Magnetohydrodynamical (MHD) simulations show that jets and molecular outflows are common in massive YSOs and that they have an important role in the formation process (e.g., Tan et al 2014;Matsushita et al 2018). For instance, Banerjee & Pudritz (2007) showed that early outflows can reduce the radiation pressure allowing the further growth of the protostar.…”

Section: 2015;mentioning

confidence: 99%

EVN observations of 6.7 GHz methanol maser polarization in massive star-forming regions

Surcis

Vlemmings

Langevelde

et al. 2019

A&A

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Context. Magnetohydrodynamical simulations show that the magnetic field can drive molecular outflows during the formation of massive protostars. The best probe to observationally measure both the morphology and the strength of this magnetic field at scales of 10–100 au is maser polarization. Aims. We measure the direction of magnetic fields at milliarcsecond resolution around a sample of massive star-forming regions to determine whether there is a relation between the orientation of the magnetic field and of the outflows. In addition, by estimating the magnetic field strength via the Zeeman splitting measurements, the role of magnetic field in the dynamics of the massive star-forming region is investigated. Methods. We selected a flux-limited sample of 31 massive star-forming regions to perform a statistical analysis of the magnetic field properties with respect to the molecular outflows characteristics. We report the linearly and circularly polarized emission of 6.7 GHz CH3OH masers towards seven massive star-forming regions of the total sample with the European VLBI Network. The sources are: G23.44−0.18, G25.83−0.18, G25.71−0.04, G28.31−0.39, G28.83−0.25, G29.96−0.02, and G43.80−0.13. Results. We identified a total of 219 CH3OH maser features, 47 and 2 of which showed linearly and circularly polarized emission, respectively. We measured well-ordered linear polarization vectors around all the massive young stellar objects and Zeeman splitting towards G25.71−0.04 and G28.83−0.25. Thanks to recent theoretical results, we were able to provide lower limits to the magnetic field strength from our Zeeman splitting measurements. Conclusions. We further confirm (based on ∼80% of the total flux-limited sample) that the magnetic field on scales of 10–100 au is preferentially oriented along the outflow axes. The estimated magnetic field strength of |B||| > 61 mG and >21 mG towards G25.71−0.04 and G28.83−0.25, respectively, indicates that it dominates the dynamics of the gas in both regions.

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Section: 2015;mentioning

confidence: 99%

EVN observations of 6.7 GHz methanol maser polarization in massive star-forming regions

Surcis

Vlemmings

Langevelde

et al. 2019

A&A

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“…XXXV 2016;Planck Collaboration Int. XXXIII 2016;Matsushita et al 2018;Beuther et al 2018). Large-scale observations (∼1 pc) of the magnetic field revealed a well-ordered structure in the lowdensity envelopes of molecular clouds, suggesting that parsecscale envelopes are magnetically supported against gravitational collapse (e.g., Franco et al 2010).…”

Section: Introductionmentioning

confidence: 99%

Outflows, cores, and magnetic field orientations in W43-MM1 as seen by ALMA

Arce-Tord

Louvet

Cortés

et al. 2020

A&A

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Aims. It has been proposed that the magnetic field, which is pervasive in the interstellar medium, plays an important role in the process of massive star formation. To better understand the impact of the magnetic field at the pre- and protostellar stages, high-angular resolution observations of polarized dust emission toward a large sample of massive dense cores are needed. We aim to reveal any correlation between the magnetic field orientation and the orientation of the cores and outflows in a sample of protostellar dense cores in the W43-MM1 high-mass star-forming region. Methods. We used the Atacama Large Millimeter Array in Band 6 (1.3 mm) in full polarization mode to map the polarized emission from dust grains at a physical scale of ~2700 au. We used these data to measure the orientation of the magnetic field at the core scale. Then, we examined the relative orientations of the core-scale magnetic field, of the protostellar outflows, and of the major axis of the dense cores determined from a 2D Gaussian fit in the continuum emission. Results. We find that the orientation of the dense cores is not random with respect to the magnetic field. Instead, the dense cores are compatible with being oriented 20–50° with respect to the magnetic field. As for the outflows, they could be oriented 50–70° with respect to the magnetic field, or randomly oriented with respect to the magnetic field, which is similar to current results in low-mass star-forming regions. Conclusions. The observed alignment of the position angle of the cores with respect to the magnetic field lines shows that the magnetic field is well coupled with the dense material; however, the 20–50° preferential orientation contradicts the predictions of the magnetically-controlled core-collapse models. The potential correlation of the outflow directions with respect to the magnetic field suggests that, in some cases, the magnetic field is strong enough to control the angular momentum distribution from the core scale down to the inner part of the circumstellar disks where outflows are triggered.

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“…We employ the same numerical code as in Machida & Hosokawa (2013), assuming spherical accretion onto the protostar (Hosokawa & Omukai 2009). While we use a different stellar evolution code in Matsushita et al (2018) and Machida & Hosokawa (2020), an advantage of the current method is that the evolution of the stellar radius only depends on the accretion history, not on other control parameters (see Section 3 in Matsushita et al 2018). The details in modeling the protostellar evolution do not affect our conclusions anyway (e.g.…”

Section: Stellar Evolution and Termination Condition Of Simulationmentioning

confidence: 99%

Impact of Magnetic Braking on High-mass Close Binary Formation

Harada,

Hirano,

Machida

et al. 2021

Preprint

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Combining numerical simulations and analytical modeling, we investigate whether close binary systems form by the effect of magnetic braking. Using magnetohydrodynamics simulations, we calculate the cloud evolution with a sink, for which we do not resolve the binary system or binary orbital motion to realize long-term time integration. Then, we analytically estimate the binary separation using the accreted mass and angular momentum obtained from the simulation. In unmagnetized clouds, wide binary systems with separations of > 100 au form, in which the binary separation continues to increase during the main accretion phase. In contrast, close binary systems with separations of < 100 au can form in magnetized clouds. Since the efficiency of magnetic braking strongly depends on both the strength and configuration of the magnetic field, they also affect the formation conditions of a close binary.In addition, the protostellar outflow has a negative impact on close binary formation, especially when the rotation axis of the prestellar cloud is aligned with the global magnetic field. The outflow interrupts the accretion of gas with small angular momentum, which is expelled from the cloud, while gas with large angular momentum preferentially falls from the side of the outflow onto the binary system and widens the binary separation. This study shows that a cloud with a magnetic field that is not parallel to the rotation axis is a favorable environment for the formation of close binary systems.

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

Cited by 28 publications

References 76 publications

EVN observations of 6.7 GHz methanol maser polarization in massive star-forming regions

EVN observations of 6.7 GHz methanol maser polarization in massive star-forming regions

Outflows, cores, and magnetic field orientations in W43-MM1 as seen by ALMA

Impact of Magnetic Braking on High-mass Close Binary Formation

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