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arxiv: 1906.11308 · v1 · pith:IUWQIWAUnew · submitted 2019-06-26 · 🌌 astro-ph.GA

Shiva: the dust destruction model

M. S. Murga , D. S. Wiebe , E. E. Sivkova , V. V. Akimkin This is my paper

Pith reviewed 2026-05-25 15:10 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords dust destructionHAC grainsphoto-processingsputteringshatteringinterstellar mediumsize distributionnumerical tool
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The pith

The Shiva tool calculates time-dependent evolution of dust grain size distributions and band gap energies under photo-processing, sputtering, and shattering.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper presents Shiva, a numerical tool built to model dust destruction and evolution in warm neutral, warm ionized, and hot ionized interstellar media. It tracks processes including dehydrogenation and carbon atom loss in hydrogenated amorphous carbon grains, which shift material from aliphatic to aromatic forms while altering band gap energy and optical properties. Inputs such as gas number densities, ionization state, temperature, radiation flux, and relative velocities determine the output of evolving size distributions for multiple grain types. The model also produces example evolutionary timescales and shows how grain properties and infrared spectra change in photo-dissociation regions, H II regions, and supernova remnant shocks. A reader would care because the tool supplies concrete predictions for grain lifetimes and observable spectral changes under specified conditions.

Core claim

Shiva is a tool that simulates dust destruction by photo-processing, sputtering, and shattering, computing the time-dependent evolution of the dust size distribution from given hydrogen, helium, and carbon number densities, ionization state, gas temperature, radiation flux, and relative gas-dust and grain-grain velocities; for HAC grains the evolution of the band gap energy distribution is computed as well.

What carries the argument

The Shiva numerical code that integrates rates for dehydrogenation, carbon atom loss, sputtering, and shattering to advance grain size distributions and, for HACs, band gap energies.

If this is right

  • Grain lifetimes can be estimated rapidly once external conditions are specified.
  • Time-dependent changes in grain properties and corresponding infrared spectra can be followed in photo-dissociation regions, H II regions, and supernova remnant shocks.
  • The same framework supports simulations of polycyclic aromatic hydrocarbons, silicate grains, and graphite grains in addition to HACs.
  • Evolution of band gap energy distributions accompanies size-distribution changes for HAC grains.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • Coupling the tool to hydrodynamic codes could allow dust evolution to be followed inside time-varying flows.
  • The computed spectral changes could be compared directly with multi-wavelength observations to test which destruction channel dominates in a given region.
  • Extending the inputs to include molecular-cloud conditions would test whether the same rates remain applicable at lower temperatures and radiation fields.

Load-bearing premise

The coded rates and cross-sections for dehydrogenation, carbon loss, sputtering, and shattering correctly capture the dominant destruction processes on real grains.

What would settle it

Observed dust size distributions or infrared spectra in an H II region or supernova remnant shock with independently measured gas densities, temperature, and radiation field that differ from the tool's predicted evolution for those inputs.

Figures

Figures reproduced from arXiv: 1906.11308 by D. S. Wiebe, E. E. Sivkova, M. S. Murga, V. V. Akimkin.

Figure 1
Figure 1. Figure 1: Optical properties of HAC grains with a size of 5 ˚A and Eg = 0.1 eV (left panel) and Eg = 2.67 eV (right panel). The original neutral grain properties from the work of Jones (2012c) are shown with blue lines (labelled as J12), the adopted properties for neutral grains modified according to the work of Jones et al. (2013) are shown with green lines, and the adopted properties for charged grains are shown w… view at source ↗
Figure 2
Figure 2. Figure 2: On the left: dependence of the IR emission rate on the photon energy. Blue solid and dashed lines correspond to 3.3 ˚A grains with zero and unit charges, respectively. Red solid and dashed lines show the same data for 5 ˚A grains. On the right: dependence of the ionization yield on the photon energy for a 3.3 ˚A grain with charge numbers of 0 (blue), 1 (green), 2 (red), 3 (black). should be destroyed on a … view at source ↗
Figure 3
Figure 3. Figure 3: A ratio between photo-destruction rates of a neutral grain and a positively charged grain for various charge values. The blue line corresponds to a grain radius of 3.3 ˚A, and the red line corresponds to a grain radius of 5 ˚A. 0 2 4 6 log10U 0 2 4 6 8 10 12 log10τ and log10τa, yr a = 5 ˚A, pd a = 5 ˚A, arom a = 50 ˚A, arom a = 1000 ˚A, arom [PITH_FULL_IMAGE:figures/full_fig_p007_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Dependence of the photo-destruction and aromati￾sation time-scales on the scaled radiation field, U. The photo￾destruction time-scale of a 5 ˚A-grain is shown with a red line. Aromatisation time-scales for 5, 50 and 1000 ˚A-grains are shown with blue, green, and magenta lines, correspondingly. distribution (Jones et al. 2013), assuming that all grains are initially hydrogenated. We took the evolution time … view at source ↗
Figure 5
Figure 5. Figure 5: On the left: a fraction of photo-destroyed dust grains (blue line) and a fraction of aromatised dust grains with radii 5 ˚A (orange), 50 ˚A (green), 1000 ˚A (red) as functions of the radiation field intensity after 1 Myr of evolution. On the right: infrared spectra of dust exposed to the UV radiation with intensities in the range from 1 to 105 of MMP83. This is further illustrated in [PITH_FULL_IMAGE:figu… view at source ↗
Figure 7
Figure 7. Figure 7: Dependence of radiation field intensity on wavelength for three representative locations considered in the work at 5 and 150 kyr. The MMP 83 (Mathis et al. 1983) radiation field is also presented. that in spite of very strong radiation field around massive stars only the smallest grains can be photo-destroyed within Hii regions, at least, according to the evolutionary model implemented in Shiva. We use the… view at source ↗
Figure 6
Figure 6. Figure 6: Evolution of infrared spectra at different RF intensities with parameters from J13 and DL07 models. The value of U and the adopted size distribution from top to bottom are U = 1 and J13, U = 103 and J13, U = 2 · 104 and J13, U = 2 · 104 and WD01. Colours indicate the model time. 103 104 λ, ˚A 100 102 104 106 Jλ, erg cm−2 s −1cm−1 n max H , 5 kyr 0.5n max H , 5 kyr n max H+ , 5 kyr n max H , 150 kyr 0.5n ma… view at source ↗
Figure 8
Figure 8. Figure 8: Evolution of number density of dust grains with radii of 4 ˚A (left panel), 6 ˚A (middle panel) and 8 ˚A (right panel). Blue colour corresponds to the location with the maximum density of neutral hydrogen, orange colour corresponds to the location with the density of neutral hydrogen 0.5nmax H , and green colour corresponds to the location with the maximum density of ionized hydrogen. 10 100 1000 λ, µm 10−… view at source ↗
Figure 9
Figure 9. Figure 9: Infrared spectra for various locations within the expanding Hii region: left panel — the point of the maximum neutral hydrogen density, middle panel – the point where neutral hydrogen density is a half of its maximum value, right panel – the point of the maximum ionized hydrogen density. Spectra for three time moments are shown in each panel: blue curves — 0 kyr, orange curves — 5 kyr, green curves — 150 k… view at source ↗
Figure 10
Figure 10. Figure 10: Top row: time-scales τ of grain destruction for grains with initial radii of 5, 50 and 1000 ˚A as functions of the gas velocity and temperature assuming the initial size distribution from the work of Jones et al. (2013). Middle row: time-scales τa of aromatisation for grains of the same initial sizes as in the top row. Bottom row: the same as in the top row, but for the WD01 initial size distribution. Not… view at source ↗
Figure 11
Figure 11. Figure 11: Left: evolution of grain radius (solid line, taken from Nozawa et al. 2006) and band gap energy (dashed line, this work) for different initial grain sizes. Right: the infrared spectra of dust in the SNR shock wave region at different time steps. The starting time of the calculation is 2·103 yr. of HACs and their subsequent aliphatisation, volatile accre￾tion and coagulation processes that dominate in the … view at source ↗
read the original abstract

We present a numerical tool Shiva designed to simulate the dust destruction in warm neutral, warm ionized, and hot ionized media under the influence of photo-processing, sputtering, and shattering. The tool is designed primarily to study the evolution of hydrogenated amorphous carbons (HACs), but options to simulate polycyclic aromatic hydrocarbons (PAHs), silicate and graphite grains are also implemented. HAC grain photo-processing includes both dehydrogenation and carbon atom loss. Dehydrogenation leads to material transformation from aliphatic to aromatic structure. Simultaneously, some other physical properties (band gap energy, optical properties, etc.) of the material change as well. The Shiva tool allows calculating the time-dependent evolution of the dust size distribution depending on hydrogen, helium, and carbon number densities and ionization state, gas temperature, radiation flux, relative gas-dust and grain-grain velocities. For HAC grains the evolution of band gap energy distribution is also computed. We describe a dust evolution model, on which the tool relies, and present evolutionary time-scales for dust grains of different sizes depending on external conditions. This allows a user to estimate quickly a lifetime of a specific dust grain under relevant conditions. As an example of the tool usage, we demonstrate how grain properties and corresponding infrared spectra evolve in photo-dissociation regions, H II regions, and supernova remnant shocks.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 1 minor

Summary. The paper presents the Shiva numerical tool for simulating dust destruction in warm neutral, warm ionized, and hot ionized media through photo-processing (including dehydrogenation and carbon atom loss for HACs), sputtering, and shattering. The tool computes time-dependent dust size distributions (and band-gap energy distributions for HACs) from inputs of n_H, n_He, n_C, ionization state, T_gas, radiation flux, and relative velocities; it also supplies example evolutionary timescales for grains of different sizes and demonstrates applications to PDRs, H II regions, and SNR shocks with resulting changes in grain properties and IR spectra.

Significance. If the hard-coded rates prove reliable, the tool would offer a practical forward model for estimating grain lifetimes and spectral evolution under specified conditions, with the timescale examples providing a quick reference for users. The inclusion of multiple grain types and the explicit tracking of HAC band-gap evolution add utility for modeling material transformation in radiative and shock environments.

major comments (2)
  1. [Abstract] Abstract: the central claim that Shiva 'allows calculating the time-dependent evolution' rests on the accuracy of the implemented rates for dehydrogenation, carbon loss, sputtering, and shattering, yet the manuscript supplies no validation, error analysis, comparison to laboratory data, other codes, or observations to support these rates.
  2. [Abstract] The description of evolutionary timescales (mentioned in the abstract) is presented without accompanying sensitivity tests or uncertainty estimates on the input cross-sections and rate coefficients, which directly affects the reliability of the reported lifetimes under the stated external conditions.
minor comments (1)
  1. [Abstract] The abstract lists options for PAHs, silicates, and graphite but does not indicate whether the same rate-coefficient framework is applied uniformly or whether grain-specific adjustments are documented.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the detailed comments. We address each major comment point by point below.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the central claim that Shiva 'allows calculating the time-dependent evolution' rests on the accuracy of the implemented rates for dehydrogenation, carbon loss, sputtering, and shattering, yet the manuscript supplies no validation, error analysis, comparison to laboratory data, other codes, or observations to support these rates.

    Authors: The manuscript presents Shiva as a tool that implements a specific dust evolution model (detailed in the methods) to compute time-dependent size and band-gap distributions. The rate coefficients for the listed processes are taken directly from the cited literature on HAC photo-processing, sputtering yields, and shattering; the paper's contribution is the integrated numerical framework rather than new empirical validation of those rates. We agree the abstract could be phrased more precisely to indicate that evolution follows the implemented model, and we will revise the abstract and add a short paragraph in the methods clarifying the literature origins of each rate coefficient. revision: partial

  2. Referee: [Abstract] The description of evolutionary timescales (mentioned in the abstract) is presented without accompanying sensitivity tests or uncertainty estimates on the input cross-sections and rate coefficients, which directly affects the reliability of the reported lifetimes under the stated external conditions.

    Authors: The timescales shown are example outputs obtained by running the model with its default rate coefficients under the stated conditions; they are intended to illustrate tool usage rather than to serve as definitive lifetime predictions. The manuscript does not contain sensitivity tests or formal uncertainty propagation. We acknowledge that such tests would be useful for users and will add a brief discussion noting the dependence on the input rates together with references to existing sensitivity studies in the sputtering and shattering literature. New dedicated sensitivity runs are outside the scope of the present work. revision: partial

Circularity Check

0 steps flagged

Shiva is a forward simulation tool with no self-referential derivations or fitted predictions

full rationale

The Shiva tool implements a forward numerical model that evolves dust size distributions and band-gap energies from externally supplied inputs (n_H, n_He, n_C, ionization state, T_gas, radiation flux, relative velocities). The manuscript describes the numerical scheme and presents example evolutionary time-scales computed from these inputs using hard-coded physical rates; no equations, parameters, or outputs are shown to be fitted to or defined in terms of the simulation results themselves. No self-citation chains or uniqueness theorems are invoked to justify the central model, and the derivation chain remains independent of its own outputs.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The central claim rests on the assumption that the coded destruction rates are accurate representations of real physics; no free parameters or invented entities are named in the abstract, but the model necessarily imports rate coefficients from prior work.

axioms (1)
  • domain assumption Rates and cross-sections for photo-processing, sputtering, and shattering are taken as known inputs from the literature and correctly implemented.
    The tool's outputs are only as reliable as these imported rates; the abstract does not derive them.

pith-pipeline@v0.9.0 · 5776 in / 1222 out tokens · 43057 ms · 2026-05-25T15:10:47.947700+00:00 · methodology

discussion (0)

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Reference graph

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    " write newline "" before.all 'output.state := FUNCTION fin.entry write newline FUNCTION new.block output.state before.all = 'skip after.block 'output.state := if FUNCTION new.sentence output.state after.block = 'skip output.state before.all = 'skip after.sentence 'output.state := if if FUNCTION not #0 #1 if FUNCTION and 'skip pop #0 if FUNCTION or pop #1...

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