Hydrodynamic and magnetohydrodynamic simulations of wire turbulence

Fogerty, Erica; Liu, Baowei; Frank, Adam; Carroll-Nellenback, Jonathan; Lebedev, S. V.

doi:10.1016/j.hedp.2019.100699

Cited by 2 publications

(2 citation statements)

References 47 publications

(58 reference statements)

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“…To simulate the dynamical evolution of a reverse shock impacting a clump of ejecta material in the SNR, the MHD code A BEAR 1 (Cunningham et al 2009;Carroll-Nellenback et al 2013) was used, a highly parallelized, multidimensional adaptive mesh refinement code which solves the conservative equations of magnetohydrodynamics on a Cartesian grid (see e.g. Poludnenko et al 2002;Cunningham et al 2009;Kaminski et al 2014;Fogerty et al 2016Fogerty et al , 2017Fogerty et al , 2019. A BEAR models only the gas phase of the ejecta environment, for the analysis of the dust evolution we will employ the post-processing code P (Paper I; Section 4).…”

Section: Magneto-hydrodynamical Simulationsmentioning

confidence: 99%

Dust survival rates in clumps passing through the Cas A reverse shock – I. Results for a range of clump densities

Kirchschlager

Schmidt

Barlow

et al. 2019

Monthly Notices of the Royal Astronomical Society

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The reverse shock in the ejecta of core-collapse supernovae is potentially able to destroy newly formed dust material. In order to determine dust survival rates, we have performed a set of hydrodynamic simulations using the grid-based code AstroBEAR in order to model a shock wave interacting with clumpy supernova ejecta. Dust motions and destruction rates were computed using our newly developed external, postprocessing code Paperboats, which includes gas drag, grain charging, sputtering and grain-grain collisions. We have determined dust destruction rates for the oxygen-rich supernova remnant Cassiopeia A as a function of initial grain sizes and clump gas density. We found that up to 30 % of the carbon dust mass is able to survive the passage of the reverse shock if the initial grain size distribution is narrow with radii around ∼ 10 − 50 nm for high gas densities, or with radii around ∼ 0.5 − 1.5 µm for low and medium gas densities. Silicate grains with initial radii around 10 − 30 nm show survival rates of up to 40 % for medium and high density contrasts, while silicate material with micron sized distributions is mostly destroyed. For both materials, the surviving dust mass is rearranged into a new size distribution that can be approximated by two components: a power-law distribution of small grains and a log-normal distribution of grains having the same size range as the initial distribution. Our results show that grain-grain collisions and sputtering are synergistic and that grain-grain collisions can play a crucial role in determining the surviving dust budget in supernova remnants.

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Section: Magneto-hydrodynamical Simulationsmentioning

confidence: 99%

Dust survival rates in clumps passing through the Cas A reverse shock – I. Results for a range of clump densities

Kirchschlager

Schmidt

Barlow

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…To simulate the dynamical evolution of a reverse shock impacting a clump of ejecta material in the SNR, the MHD code ASTROBEAR 1 (Cunningham et al 2009 ;Carroll-Nellenback et al 2013 ) was used, a highly parallelized, multidimensional adaptive mesh refinement code which solves the conserv ati ve equations of MHD on a Cartesian grid (see e.g. Poludnenko, Frank & Blackman 2002 ;Cunningham et al 2009 ;Kaminski et al 2014 ;Fogerty et al 2016Fogerty et al , 2017Fogerty et al , 2019. ASTROBEAR models only the gas-phase of the ejecta environment for the analysis of the dust evolution, we will employ the postprocessing code PAPERBOATS ( Paper I ; Section 4 ).…”

Section: Ag N E To H Y D Ro Dy Na M I C a L S I M U L At I O N Smentioning

confidence: 99%

Dust survival rates in clumps passing through the Cas A reverse shock – II. The impact of magnetic fields

Kirchschlager

Schmidt

Barlow

et al. 2023

Monthly Notices of the Royal Astronomical Society

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Dust grains form in the clumpy ejecta of core-collapse supernovae where they are subject to the reverse shock, which is able to disrupt the clumps and destroy the grains. Important dust destruction processes include thermal and kinetic sputtering as well as fragmentation and grain vaporization. In the present study, we focus on the effect of magnetic fields on the destruction processes. We have performed magneto-hydrodynamical simulations using AstroBEAR to model a shock wave interacting with an ejecta clump. The dust transport and destruction fractions are computed using our post-processing code Paperboats in which the acceleration of grains due to the magnetic field and a procedure that allows partial grain vaporization have been newly implemented. For the oxygen-rich supernova remnant Cassiopeia A we found a significantly lower dust survival rate when magnetic fields are aligned perpendicular to the shock direction compared to the non-magnetic case. For a parallel field alignment, the destruction is also enhanced but at a lower level. The survival fractions depend sensitively on the gas density contrast between the clump and the ambient medium and on the grain sizes. For a low-density contrast of 100, e.g., 5 nm silicate grains are completely destroyed while the survival fraction of 1 μm grains is 86 per cent. For a high-density contrast of 1000, 95 per cent of the 5 nm grains survive while the survival fraction of 1 μm grains is 26 per cent. Alternative clump sizes or dust materials (carbon) have non-negligible effects on the survival rate but have a lower impact compared to density contrast, magnetic field strength, and grain size.

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Hydrodynamic and magnetohydrodynamic simulations of wire turbulence

Cited by 2 publications

References 47 publications

Dust survival rates in clumps passing through the Cas A reverse shock – I. Results for a range of clump densities

Dust survival rates in clumps passing through the Cas A reverse shock – I. Results for a range of clump densities

Dust survival rates in clumps passing through the Cas A reverse shock – II. The impact of magnetic fields

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