Evolution of Hubble wedges in episodic protostellar outflows

Rohde, P. F.; Walch, Stefanie; Seifried, D.; Whitworth, Anthony Peter; Clarke, S. D.; Hubber, D. A.

doi:10.1093/mnras/sty3302

Cited by 15 publications

(44 citation statements)

References 122 publications

(163 reference statements)

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“…We use the episodic accretion rate for the following subgrid models. Varying dM dt | MRI has little effect on the outcome of the simulations (Rohde et al 2019).…”

Section: Episodic Accretionmentioning

confidence: 94%

“…As in Rohde et al (2019), we use the approximate radiative heating and cooling algorithm of Stamatellos et al (2007). This method uses local SPH particle quantities to estimate a mean optical depth, which is then used to compute heating and cooling rates.…”

Section: Sph Code Gandalfmentioning

confidence: 99%

“…It is presently not computationally feasible to follow the evolution of protostars through the whole protostellar phase using such a high resolution. Other authors therefore mitigate this problem by invoking almost resolution-independent subgrid models to launch outflows (Nakamura & Li 2007;Cunningham et al 2011;Federrath et al 2014;Myers et al 2014;Offner & Arce 2014;Peters et al 2014;Kuiper, Yorke & Turner 2015;Offner & Chaban 2017;Li et al 2018;Rohde et al 2019) Exactly how the gas is launched is still not well understood (see, e.g. the reviews of Arce et al 2007;Frank et al 2014;Bally 2016).…”

mentioning

confidence: 99%

“…The paper is structured as follows. In Section 2, we describe the computational method, outline modifications to the subgrid outflow model developed earlier by Rohde et al (2019), and define the initial and boundary conditions. In Section 3, we present the results of the simulations and discuss how the stellar properties depend on the initial conditions.…”

mentioning

confidence: 99%

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The impact of episodic outflow feedback on stellar multiplicity and the star formation efficiency

Rohde

Walch

Clarke

et al. 2020

Monthly Notices of the Royal Astronomical Society

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The accretion of material onto young protostars is accompanied by the launching of outflows. Observations show that accretion, and therefore also outflows, are episodic. However, the effects of episodic outflow feedback on the core-scale are not well understood. We have performed 88 Smoothed Particle Hydrodynamic simulations of turbulent dense $1 \, \rm {M}_{\odot }$ cores, to study the influence of episodic outflow feedback on the stellar multiplicity and the star formation efficiency (SFE). Protostars are represented by sink particles, which use a sub-grid model to capture stellar evolution, inner-disc evolution, episodic accretion and the launching of outflows. By comparing simulations with and without episodic outflow feedback, we show that simulations with outflow feedback reproduce the binary statistics of young stellar populations, including the relative proportions of singles, binaries, triples, etc. and the high incidence of twin binaries with q ≥ 0.95; simulations without outflow feedback do not. Entrainment factors (the ratio between total outflowing mass and initially ejected mass) are typically ∼7 ± 2, but can be much higher if the total mass of stars formed in a core is low and/or outflow episodes are infrequent. By decreasing both the mean mass of the stars formed and the number of stars formed, outflow feedback reduces the SFE by about a factor of 2 (as compared with simulations that do not include outflow feedback).

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“…We use the episodic accretion rate for the following subgrid models. Varying dM dt | MRI has little effect on the outcome of the simulations (Rohde et al 2019).…”

Section: Episodic Accretionmentioning

confidence: 94%

Section: Sph Code Gandalfmentioning

confidence: 99%

mentioning

confidence: 99%

mentioning

confidence: 99%

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The impact of episodic outflow feedback on stellar multiplicity and the star formation efficiency

Rohde

Walch

Clarke

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…The velocity structures look like "Hubble wedges" (Arce & Goodman 2001). Recent theoretical models of episodic protostellar outflows (e.g., Federrath et al 2014;Offner & Arce 2014;Offner & Chaban 2017;Rohde et al 2019) have been built to reproduce such features. A separate blueshifted emission feature seems to be driven by the continuum core C6c5, which is associated with a CO(2-1) outflow (Kong et al 2019).…”

Section: Morphology and Kinematicsmentioning

confidence: 99%

Sio Outflows as Tracers of Massive Star Formation in Infrared Dark Clouds

Liu¹

2017

Proceedings of the 72nd International Symposium on Molecular Spectroscopy

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To study the early phases of massive star formation, we present ALMA observations of SiO(5-4) emission and VLA observations of 6 cm continuum emission towards 32 Infrared Dark Cloud (IRDC) clumps, which are spatially resolved down to 0.05 pc. Out of the 32 clumps observed, we have detected SiO emission in 20 clumps, and in 11 of them it is relatively strong and likely tracing protostellar outflows. Some SiO outflows are collimated, while others are less well ordered. There is evidence for episodic ejection events, as well as multiple outflows originating from scales of 0.1 pc. For the six strongest SiO outflows, we estimate basic outflow properties. We do not see clear dependence of the degree of collimation of the outflows on core mass, luminosity and evolutionary stage. In our entire sample, where there is SiO emission, we always find 1.3 mm continuum emission and some infrared emission nearby, but not vice versa. We build the spectral energy distributions (SEDs) of all the cores with 1.3 mm continuum emission and fit them with radiative transfer (RT) models. The low luminosities and stellar masses returned by SED fitting suggest these are early stage protostars. We see a slight trend of increasing SiO line luminosity with bolometric luminosity, which suggests more powerful shocks in the vicinity of more massive YSOs. However, we do not see a clear relation between the SiO luminosity and the evolutionary stage indicated by L/M. We conclude that as a protostar approaches a bolometric luminosity of ∼ 10 2 L , the shocks in the outflow are generally strong enough to form SiO emission. The VLA 6 cm observations toward the 15 clumps with the strongest SiO emission detect emission in four clumps, which is likely to be shock ionized jets associated with the more massive of these protostellar cores.

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Episodic accretion constrained by a rich cluster of outflows

Nony

Motte

Louvet

et al. 2020

A&A

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Context. The accretion history of protostars remains widely mysterious even though it represents one of the best ways to understand the protostellar collapse that leads to the formation of stars. Aims. Molecular outflows, which are easier to detect than the direct accretion onto the prostellar embryo, are here used to characterize the protostellar accretion phase in W43-MM1. Methods. The W43-MM1 protocluster host a sufficient number of protostars to statistically investigate molecular outflows in a single, homogeneous region. We used the CO(2-1) and SiO(5-4) line datacubes, taken as part of an ALMA mosaic with a 2000 AU resolution, to search for protostellar outflows, evaluate the influence that the environment has on these outflows' characteristics and put constraints on outflow variability in W43-MM1. Results. We discovered a rich cluster of 46 outflow lobes, driven by 27 protostars with masses of 1−100 M . The complex environment inside which these outflow lobes develop has a definite influence on their length, limiting the validity of using outflows' dynamical timescales as a proxy of the ejection timescale in clouds with high dynamics and varying conditions. We performed a detailed study of Position-Velocity (PV) diagrams of outflows that revealed clear events of episodic ejection. The time variability of W43-MM1 outflows is a general trend and is more generally observed than in nearby, low-to intermediate-mass star-forming regions. The typical timescale found between two ejecta, ∼500 yr, is consistent with that found in nearby protostars.Conclusions. If ejection episodicity reflects variability in the accretion process, either protostellar accretion is more variable or episodicity is easier to detect in high-mass star-forming regions than in nearby clouds. The timescale found between accretion events could be resulting from instabilities, associated with bursts of inflowing gas arising from the close dynamical environment of highmass star-forming cores.

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Evolution of Hubble wedges in episodic protostellar outflows

Cited by 15 publications

References 122 publications

The impact of episodic outflow feedback on stellar multiplicity and the star formation efficiency

The impact of episodic outflow feedback on stellar multiplicity and the star formation efficiency

Sio Outflows as Tracers of Massive Star Formation in Infrared Dark Clouds

Episodic accretion constrained by a rich cluster of outflows

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