Grain Growth

Overview

Grain growth increases dust mass by accreting gas-phase metals directly onto existing grains, following Hirashita & Kuo (2011, HK11). Alongside coagulation, it is one of the two mechanisms by which CosmicGrain builds up dust mass beyond what is injected by stellar sources, and is typically the dominant channel for reconciling short stellar dust-production timescales with the larger dust masses observed in evolved, metal-enriched galaxies. Growth is most efficient in dense, cold, metal-rich gas, and is capped by a redshift-dependent maximum dust-to-metal ratio to prevent runaway growth in metal-poor early-universe conditions.

Physical Model

CosmicGrain uses the HK11 accretion timescale,

\[ \tau_{\rm acc} = \tau_0 \left(\frac{a}{0.1\,\mu{\rm m}}\right)\left(\frac{Z_\odot}{Z}\right)\left(\frac{1000\,{\rm cm^{-3}}}{n_H}\right)\left(\frac{50\,{\rm K}}{T}\right)^{1/2}\left(\frac{0.3}{S}\right) \]

where

• \(a\) is the grain radius, \(Z\) the gas metallicity, \(n_H\) the (clumping-boosted) hydrogen number density, \(T\) an assumed effective grain surface temperature, and \(S\) the sticking coefficient,
• \(\tau_0\) is a species-dependent prefactor: \(6.30\times10^7\) yr for silicates and \(5.59\times10^7\) yr for carbonaceous material.

The current implementation evolves the carbonaceous and silicate components independently. Their requested growth increments scale as

\[ \Delta M_i \propto M_i \left[\exp\!\left(\frac{3 f_{\rm mol}\Delta t}{\tau_i}\right)-1\right], \]

and are limited by the corresponding gas-phase element reservoirs. Growth can therefore change CarbonMassFraction; it is no longer a binary species choice based on whether CF lies above or below 0.5.

For a pure component, the mass-growth expression corresponds to the familiar radius update

\[ a_{\rm new} = a \times \exp\!\left(\frac{f_{\rm mol}\,\Delta t}{\tau_{\rm acc}}\right) \]

where \(f_{\rm mol}\) is an effective molecular-gas fraction. For a mixed particle, the code first applies the separately limited carbon and silicate mass increments, then reconstructs one characteristic radius from the final total mass using the exact cubic relation. This avoids the linear \(dm\approx3M_{\rm dust}(da/a)\) approximation that previously produced a spurious mass leak during rapid growth.

Growth is bounded by a redshift-dependent maximum dust-to-metal ratio,

\[ \left(\frac{M_{\rm dust}}{M_{\rm metals}}\right)_{\rm max} = \max\!\left(0.05,\ \frac{0.5}{1+0.15z}\right) \]

which interpolates from ~0.05 at high redshift (z ≈ 6) to 0.5 at z = 0, preventing unphysical runaway growth in metal-poor early-universe gas.

Assumptions

• Growth is evaluated per dust particle against its already-paired nearest gas neighbor (established by the caller); no independent grain–grain or grain–gas search occurs inside this routine.
• The effective grain surface temperature used in the accretion timescale is a fixed 20 K, independent of the particle's actual tracked dust temperature (DustTemperature, computed elsewhere via radiative equilibrium).
• Sticking coefficient is a fixed 0.3, independent of grain size or composition.
• Carbon and silicate accretion use separate timescales and element budgets.
• The molecular fraction \(f_{\rm mol}\) is an observationally-motivated proxy binned by density/star-formation state, not a computed H₂ fraction.
• Accreted metal mass is removed from the gas particle's metallicity, conserving total metal mass between gas and dust phases.

Implementation

Growth is gated by four sequential checks — hot gas, insufficient metals, low density, and the D/Z cap — before the accretion timescale and size update are computed. Up to three separate caps (D/Z ratio, metal availability, and a per-step growth limit) can each reduce the mass a grain is allowed to accrete; the final grain radius is derived exactly from whichever mass survives all three, applied once at the end, so radius and mass always remain a self-consistent \(m \propto a^3\) pair regardless of which cap ends up binding.

Early D/Z pre-filter (intentional, not a bug)

Before computing the redshift-dependent cap, a cheap early-exit check compares dust and gas particle masses directly using a hardcoded 0.5 rather than the true cap value. Since the true cap max_dust_to_metal is always ≤ 0.5 for any redshift ≥ 0 (0.5 being its value exactly at z = 0), this pre-filter can never incorrectly reject a grain that would go on to pass the real, more expensive check — it only ever saves work in cases guaranteed to fail regardless of redshift.

An unreachable failure path

The low-\(f_{\rm mol}\) failure branch (f_mol < 0.01) can never currently fire: \(f_{\rm mol}\) is initialized at a 0.05 floor and is only ever multiplied upward by the metal-rich boost, never downward. The associated diagnostic counter will always read zero in practice.

Numerical floors

• Accretion timescale is clamped to [10⁶, 5×10⁹] yr.
• The clumping-boosted density used in the timescale calculation is floored at 10⁻³ cm⁻³ as a purely numerical safeguard.
• Accreted mass can never exceed 99% of the gas particle's available metal mass.
• Mass gain per call is capped at 20% of the dust particle's current mass.
• Multiple corruption guards detect and remove grains with unphysical state (zeroed fields from domain exchange, or NaN/negative values from upstream numerical issues) before they can propagate into the growth calculation.

Algorithm

1. Gate on gas temperature — hot gas above the sputtering threshold inhibits accretion entirely.
2. Gate on gas metallicity — gas with negligible metal content cannot supply growth.
3. Gate on local density — diffuse gas below a minimum clumping-boosted density is skipped early.
4. Apply the cheap D/Z pre-filter, then the exact redshift-dependent D/Z cap.
5. Determine the molecular fraction \(f_{\rm mol}\) from local density, star-forming state, and metallicity.
6. Validate the dust particle's state, removing corrupted particles if found.
7. Compute separate HK11 accretion requests for the carbonaceous and silicate components.
8. Apply the D/Z and 20%-per-call total-growth caps while preserving the requested component ratio.
9. Remove the requested elements from gas, allowing the element-resolved helper to impose the final physical availability limits.
10. Update dust mass, radius, and carbon fraction together, resynchronize the gas mass/metallicity fields, and update diagnostics.

Parameters

Parameter	Description
DustEnableGrowth	Enables or disables grain growth via accretion.
DustGrowthCalibration	Multiplicative calibration factor applied to the HK11 accretion timescale.
DustMinGrainSize	Minimum grain radius (shared across all dust physics modules).
DustMaxGrainSize	Maximum grain radius reachable via growth (shared across all dust physics modules).

The HK11 prefactors (6.30×10⁷ / 5.59×10⁷ yr), the effective grain surface temperature (20 K), the sticking coefficient (0.3), the molecular-fraction density bins, and the D/Z cap's functional form and floor (0.05) are hardcoded and not currently exposed as parameters.

Where in the Code?

src/dust/dust.cc

• Growth routine
• dust_grain_growth_subgrid()
  • Applies all gating checks, evolves carbon and silicate accretion separately, updates grain radius/mass/composition, and enforces the D/Z and availability caps.
• tau_acc_yr_HK11()
  • Evaluates the HK11 accretion timescale formula for a given density, temperature, metallicity, grain size, sticking coefficient, and species.
• dust_clumping_factor()
  • Supplies the subgrid density enhancement used to compute the clumping-boosted \(n_{\rm eff}\) that gates growth and sets \(f_{\rm mol}\).
• Bookkeeping: NGrainGrowthEvents, TotalMassGrown.

src/dust/update_dust_dynamics()

• Caller
• Invokes dust_grain_growth_subgrid() using the Hsml-aware association radius \(\max(2\,{\rm kpc},\min(H_{\rm sml},10\,{\rm kpc}))\), on the same cadence as coagulation and shattering.

Primary References

Foundational papers relevant to interstellar grain growth via accretion.

Hirashita & Kuo (2011)

Hirashita, H., & Kuo, T.-M. (2011). Effects of Grain Size Distribution on the Interstellar Dust Mass Growth. Monthly Notices of the Royal Astronomical Society, 416, 1340–1353.

Source of the accretion timescale formula CosmicGrain implements directly (HK11).

📚 ADS 🔗 DOI

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Asano, Takeuchi, Hirashita & Nozawa (2013)

Asano, R. S., Takeuchi, T. T., Hirashita, H., & Nozawa, T. (2013). What Determines the Grain Size Distribution in Galaxies? Monthly Notices of the Royal Astronomical Society, 432, 637–652.

Extends the HK11 accretion framework alongside coagulation, shattering, and destruction to model the evolving grain size distribution — the broader framework CosmicGrain's combined growth and coagulation modules draw on.

📚 ADS 🔗 DOI