PLUTO: A Numerical Code for Computational Astrophysics

Mignone, A.; Bodo, G.; Massaglia, S.; Matsakos, T.; Tešileanu, O.; Zanni, C.; Ferrari, A.

doi:10.1086/513316

Cited by 1,465 publications

(1,330 citation statements)

References 64 publications

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“…We perfom two-dimensional simulations using the code PLUTO (Mignone et al 2007(Mignone et al , 2012 to model the circumstellar medium of moving core-collapse supernova progenitors. We Table 1.…”

Section: Modelling the Circumstellar Mediummentioning

confidence: 99%

“…We tested that the code PLUTO (Mignone et al 2007(Mignone et al , 2012 reproduced the one-dimensional models of core-collapse supernovae interacting with their surroundings in Whalen et al (2008) and van Veelen et al (2009) using a uniform, spherically symmetric grid. Our numerical method (Paper I) is different from that in Whalen et al (2008) because (i) they utilise a finite-difference scheme coupled to a network of chemical reactions following the non-equilibrium rates of the species composing the gas and (ii) their algorithm includes artificial viscosity (ZEUS code, see Stone & Norman 1992).…”

Section: Comparison With Previous Workmentioning

confidence: 99%

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Asymmetric supernova remnants generated by Galactic, massive runaway stars

Meyer¹,

Langer²,

Mackey³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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After the death of a runaway massive star, its supernova shock wave interacts with the bow shocks produced by its defunct progenitor, and may lose energy, momentum, and its spherical symmetry before expanding into the local interstellar medium (ISM). We investigate whether the initial mass and space velocity of these progenitors can be associated with asymmetric supernova remnants. We run hydrodynamical models of supernovae exploding in the pre-shaped medium of moving Galactic core-collapse progenitors. We find that bow shocks that accumulate more than about 1.5 M ⊙ generate asymmetric remnants. The shock wave first collides with these bow shocks 160 − 750 yr after the supernova, and the collision lasts until 830 − 4900 yr. The shock wave is then located 1.35 − 5 pc from the center of the explosion, and it expands freely into the ISM, whereas in the opposite direction it is channelled into the region of undisturbed wind material. This applies to an initially 20 M ⊙ progenitor moving with velocity 20 km s −1 and to our initially 40 M ⊙ progenitor. These remnants generate mixing of ISM gas, stellar wind and supernova ejecta that is particularly important upstream from the center of the explosion. Their lightcurves are dominated by emission from optically-thin cooling and by X-ray emission of the shocked ISM gas. We find that these remnants are likely to be observed in the [OIII] λ 5007 spectral line emission or in the soft energy-band of X-rays. Finally, we discuss our results in the context of observed Galactic supernova remnants such as 3C391 and the Cygnus Loop.

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Section: Modelling the Circumstellar Mediummentioning

confidence: 99%

Section: Comparison With Previous Workmentioning

confidence: 99%

Asymmetric supernova remnants generated by Galactic, massive runaway stars

Meyer¹,

Langer²,

Mackey³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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“…Enzo is an open source AMR HD code (an MHD version exists but is not public) with cosmology capabilities and two different radiation methods (Abel & Wandelt 2002;Norman et al 2008;Reynolds et al 2009). Pluto is an open source AMR MHD code with a newly-developed radiation solver (Mignone et al 2007;Kuiper et al 2010). There are also a number of fixed, nested grid codes in use, but I will not mention these by name.…”

Section: Codesmentioning

confidence: 99%

Star Formation with Adaptive Mesh Refinement Radiation Hydrodynamics

Krumholz

2010

Proc. IAU

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Abstract. I provide a pedagogic review of adaptive mesh refinement (AMR) radiation hydrodynamics (RHD) methods and codes used in simulations of star formation, at a level suitable for researchers who are not computational experts. I begin with a brief overview of the types of RHD processes that are most important to star formation, and then I formally introduce the equations of RHD and the approximations one uses to render them computationally tractable. I discuss strategies for solving these approximate equations on adaptive grids, with particular emphasis on identifying the main advantages and disadvantages of various approximations and numerical approaches. Finally, I conclude by discussing areas ripe for improvement.

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“…The evolution of the gas density, velocity, pressure, and total energy density is computed using the magneto-hydrodynamics code Pluto3 (Mignone et al 2007), including full tensor viscosity. The derivation and numerical details of the newly developed frequency dependent hybrid radiation transport method are summarized by Kuiper et al (2010a).…”

Section: The Codementioning

confidence: 99%

The role of accretion disks in the formation of massive stars

et al. 2010

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Abstract. We present radiation hydrodynamics simulations of the collapse of massive pre-stellar cores. We treat frequency dependent radiative feedback from stellar evolution and accretion luminosity at a numerical resolution down to 1.27 AU. In the 2D approximation of axially symmetric simulations, it is possible for the first time to simulate the whole accretion phase of several 10 5 yr for the forming massive star and to perform a comprehensive scan of the parameter space. Our simulation series show evidently the necessity to incorporate the dust sublimation front to preserve the high shielding property of massive accretion disks. Our disk accretion models show a persistent high anisotropy of the corresponding thermal radiation field, yielding to the growth of the highest-mass stars ever formed in multi-dimensional radiation hydrodynamics simulations. Non-axially symmetric effects are not necessary to sustain accretion. The radiation pressure launches a stable bipolar outflow, which grows in angle with time as presumed from observations. For an initial mass of the pre-stellar host core of 60, 120, 240, and 480 the masses of the final stars formed in our simulations add up to 28.2, 56.5, 92.6, and at least 137.2 respectively.

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PLUTO: A Numerical Code for Computational Astrophysics

Cited by 1,465 publications

References 64 publications

Asymmetric supernova remnants generated by Galactic, massive runaway stars

Asymmetric supernova remnants generated by Galactic, massive runaway stars

Star Formation with Adaptive Mesh Refinement Radiation Hydrodynamics

The role of accretion disks in the formation of massive stars

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