Two‐Fluid Magnetohydrodynamic Simulations of Converging H<scp>i</scp>Flows in the Interstellar Medium. I. Methodology and Basic Results

Inoue, Tsuyoshi; Inutsuka, Shu‐ichiro

doi:10.1086/590528

Cited by 134 publications

(161 citation statements)

References 29 publications

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“…This observationally informed paradigm has been reproduced by recent simulations of magnetized selfgravitating filaments (e.g., Inoue & Inutsuka 2008, 2012Li et al 2010;Soler et al 2013). Cores then form on filaments, becoming gravitationally unstable and subsequently collapsing to form protostars (André et al 2014).…”

Section: Theoretical Modelsmentioning

confidence: 77%

First Results from BISTRO: A SCUBA-2 Polarimeter Survey of the Gould Belt

Ward-Thompson

Pattle

Bastien

et al. 2017

ApJ

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We present the first results from the B-fields In STar-forming Region Observations (BISTRO) survey, using the Sub-millimetre Common-User Bolometer Array2 camera, with its associated polarimeter (POL-2), on the James Clerk Maxwell Telescope in Hawaii. We discuss the survey's aims and objectives. We describe the rationale behind the survey, and the questions thatthe survey will aim to answer. The most important of these is the role of magnetic fields in the star formation process on the scale of individual filaments and cores in dense regions. We describe the data acquisition and reduction processes for POL-2, demonstrating both repeatability and consistency with previous data. We present a first-look analysis of the first results from the BISTRO survey in the OMC1 region. We see that the magnetic field lies approximately perpendicular to the famous "integral filament" in the densest regions of that filament. Furthermore, we see an "hourglass" magnetic field morphology extending beyond the densest region of the integral filament into the less-dense surrounding material, and discuss possible causes for this. We also discuss the more complex morphology seen along the Orion Bar region. We examine the morphology of the field along the lower-density northeastern filament. We find consistency with previous theoretical models that predict magnetic fields lying parallel to low-density, non-self-gravitating filaments, and perpendicular to higher-density, self-gravitating filaments.

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Section: Theoretical Modelsmentioning

confidence: 77%

First Results from BISTRO: A SCUBA-2 Polarimeter Survey of the Gould Belt

Ward-Thompson

Pattle

Bastien

et al. 2017

ApJ

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“…According to the series of papers by Inoue & Inutsuka (2008, however, including the magnetic field is expected to reduce the density of the swept-up shell substantially. Therefore the magnetic field should significantly affect the actual structure of compressed shell and subsequent star formation process (cf., 3D simulation by Arthur et al 2011).…”

Section: Expanding Hii Regions In Magnetized Ismmentioning

confidence: 99%

“…This simplifies the question of the initial conditions of star formation, but poses the problem of how such filamentary molecular clouds are created in the interstellar medium (ISM) prior to star formation. Recent highresolution magneto-hydrodynamical simulations of two-fluid dynamics with radiative cooling, radiative heating, and thermal conduction by Inoue & Inutsuka (2008 have shown that the formation of molecular clouds requires multiple episodes of supersonic compression (see also Heitsch et al 2009). Inoue & Inutsuka (2012) further investigated the formation of molecular clouds in the magnetized ISM and revealed the formation of a magnetized molecular cloud by the accretion of HI clouds created through thermal instability.…”

Section: Introductionmentioning

confidence: 99%

The formation and destruction of molecular clouds and galactic star formation

Inutsuka

Inoue

Iwasaki

et al. 2015

A&A

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We describe an overall picture of galactic-scale star formation. Recent high-resolution magneto-hydrodynamical simulations of twofluid dynamics with cooling, heating, and thermal conduction have shown that the formation of molecular clouds requires multiple episodes of supersonic compression. This finding enables us to create a scenario in which molecular clouds form in interacting shells or bubbles on a galactic scale. First, we estimated the ensemble-averaged growth rate of molecular clouds on a timescale longer than a million years. Next, we performed radiation hydrodynamics simulations to evaluate the destruction rate of magnetized molecular clouds by the stellar far-ultraviolet radiation. We also investigated the resulting star formation efficiency within a cloud, which amounts to a low value (a few percent) if we adopt the power-law exponent ∼− 2.5 for the mass distribution of stars in the cloud. We finally describe the time evolution of the mass function of molecular clouds on a long timescale (>1 Myr) and discuss the steady state exponent of the power-law slope in various environments.

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“…In this work, we use the piecewise exact solution for the gas-dust friction term (Inoue & Inutsuka 2008). The piecewise exact solution is an operator splitting method and used to integrate numerically a stiff differential equation.…”

Section: Gas-dust Frictionmentioning

confidence: 99%

Non-linear development of secular gravitational instability in protoplanetary disks

Tominaga

Inutsuka

Takahashi

2018

Publications of the Astronomical Society of Japan

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We perform non-linear simulation of secular gravitational instability (GI) in protoplanetary disks that has been proposed as a mechanism of the planetesimal formation and the multiple ring formation. Since the timescale of the growth of the secular GI is much longer than the Keplerian rotation period, we develop a new numerical scheme for a long term calculation utilizing the concept of symplectic integrator. With our new scheme, we first investigate the non-linear development of the secular GI in a disk without a pressure gradient in the initial state. We find that the surface density of dust increases by more than a factor of one hundred while that of gas does not increase even by a factor of two, which results in the formation of dust-dominated rings. A line mass of the dust ring tends to be very close to the critical line mass of a self-gravitating isothermal filament. Our results indicate that the non-linear growth of the secular GI provides a powerful mechanism to concentrate the dust. We also find that the dust ring formed via the non-linear growth of the secular GI migrates inward with a low velocity, which is driven by the self-gravity of the ring. We give a semi-analytical expression for the inward migration speed of the dusty ring.

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Two‐Fluid Magnetohydrodynamic Simulations of Converging HiFlows in the Interstellar Medium. I. Methodology and Basic Results

Cited by 134 publications

References 29 publications

First Results from BISTRO: A SCUBA-2 Polarimeter Survey of the Gould Belt

First Results from BISTRO: A SCUBA-2 Polarimeter Survey of the Gould Belt

The formation and destruction of molecular clouds and galactic star formation

Non-linear development of secular gravitational instability in protoplanetary disks

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