Dust grain coagulation modelling : From discrete to continuous

Paruta, Paola; Hendrix, Tom; Keppens, Rony

doi:10.1016/j.ascom.2016.05.002

Cited by 25 publications

(4 citation statements)

References 28 publications

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“…The result of the time dependent evolution of the dust size distribution is shown in e.g. Silsbee et al (2020); Paruta et al (2016); Ormel et al (2011Ormel et al ( , 2009; Weingartner & Draine (2001). In these models, at the very first stage of aggregation, the size boundaries of the distribution do not move significantly, as there is mostly a redistribution of the most numerous small grains aggregating to other grains of the distribution, and the parameter affected is the slope of the distribution.…”

Section: Dust Grains Growth and Size Distributionmentioning

confidence: 99%

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Influence of grain growth on CO₂ ice spectroscopic profiles

Dartois

Noble

Ysard

et al. 2022

A&A

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Interstellar dust grain growth in dense clouds and protoplanetary disks, even moderate, affects the observed interstellar ice profiles as soon as a significant fraction of dust grains is in the size range close to the wave vector at the considered wavelength. The continuum baseline correction made prior to analysing ice profiles influences the subsequent analysis and hence the estimated ice composition, typically obtained by band fitting using thin film ice mixture spectra. We explore the effect of grain growth on the spectroscopic profiles of ice mantle constituents, focusing particularly on carbon dioxide, with the aim of understanding how it can affect interstellar ice mantle spectral analysis and interpretation. Using the Discrete Dipole Approximation for Scattering and Absorption of Light, the mass absorption coefficients of several distributions of grains -composed of ellipsoidal silicate cores with water and carbon dioxide ice mantles -are calculated. A few models also include amorphous carbon in the core and pure carbon monoxide in the ice mantle. We explore the evolution of the size distribution starting in the dense core phase in order to simulate the first steps of grain growth up to three microns in size. The resulting mass absorption coefficients are injected into RADMC-3D radiative transfer models of spherical dense core and protoplanetary disk templates to retrieve the observable spectral energy distributions. Calculations are performed using the full scattering capabilities of the radiative transfer code. We then focus on the particularly relevant calculated profile of the carbon dioxide ice band at 4.27 𝜇m. The carbon dioxide antisymmetric stretching mode profile is a meaningful indicator of grain growth. The observed profile toward dense cores with the Infrared space observatory and Akari satellites already showed profiles possibly indicative of moderate grain growth. The observation of true protoplanetary disks at high inclination with the JWST should present distorted profiles that will allow constraints to be placed on the extent of dust growth. The more evolved the dust size distribution, the more the extraction of the ice mantle composition will require both understanding and taking into account grain growth.

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Section: Dust Grains Growth and Size Distributionmentioning

confidence: 99%

“…With such calculations, we reproduce qualitatively the range of evolution of the model results presented in, for example, Figs. 2-3 of Paruta et al (2016) or Figs. 4-6 of Silsbee et al (2020.…”

Section: Dust Grain Growth and Size Distributionmentioning

confidence: 99%

Influence of grain growth on CO₂ ice spectroscopic profiles

Dartois

Noble

Ysard

et al. 2022

A&A

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“…Appendix A details how grain velocities in the CNM and WIM are combined with our equation of state model to estimate velocities for populations of grains in the ISM. These velocity curves allow us to calculate the relative velocities vrel(a1, a2) that determine shattering rates, which have been studied in a variety of works (Voelk et al 1980;Markiewicz, Mizuno & Voelk 1991;Cuzzi & Hogan 2003;Yan, Lazarian & Draine 2004;Ormel & Cuzzi 2007;Ormel et al 2009;Hirashita & Li 2013;Paruta, Hendrix & Keppens 2016).…”

Section: Shatteringmentioning

confidence: 99%

“…The formalism of dust coagulation also shares many similarities with a wide class of population balance equations (Smoluchowski 1916;Vigil & Ziff 1989;Dubovskii, Galkin & Stewart 1992;Krivitsky 1995;Lee 2001;Filbet & Laurenc ¸ot 2004;Fournier & Laurenc ¸ot 2005). A variety of methods have been used to numerically model dust coagulation, including a piecewise constant grain size discretisation (Hirashita & Yan 2009), a Monte Carlo-based collision evolution simulator (Ormel et al 2009), direct numerical integration of the integro-differential coagulation equation (Asano et al 2013b), a method of moments approach that does not explicitly evolve the grain size distribution (Mattsson 2016), and a finite volume method applied to the conservative form of the coagulation equation (Paruta, Hendrix & Keppens 2016).…”

Section: Coagulationmentioning

confidence: 99%

Simulating galactic dust grain evolution on a moving mesh

McKinnon

Vogelsberger

Torrey

et al. 2018

Monthly Notices of the Royal Astronomical Society

128

139

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We present a model for the interaction between dust and radiation fields in the radiation hydrodynamic code AREPO-RT, which solves the moment-based radiative transfer equations on an unstructured moving mesh. Dust is directly treated using live simulation particles, each of which represent a population of grains that are coupled to hydrodynamic motion through a drag force. We introduce methods to calculate radiation pressure on and photon absorption by dust grains. By including a direct treatment of dust, we are able to calculate dust opacities and update radiation fields self-consistently based on the local dust distribution. This hybrid scheme coupling dust particles to an unstructured mesh for radiation is validated using several test problems with known analytic solutions, including dust driven via spherically-symmetric flux from a constant luminosity source and photon absorption from radiation incident on a thin layer of dust. Our methods are compatible with the multifrequency scheme in AREPO-RT, which treats UV and optical photons as single-scattered and IR photons as multi-scattered. At IR wavelengths, we model heating of and thermal emission from dust. Dust and gas are not assumed to be in local thermodynamic equilibrium but transfer energy through collisional exchange. We estimate dust temperatures by balancing these dust-radiation and dust-gas energy exchange rates. This framework for coupling dust and radiation can be applied in future radiation hydrodynamic simulations of galaxy formation.

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