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Further correction to the STARFORGE methods paper: Planck-mean dust opacities

Michael Y. Grudić, Dávid Guszejnov, Philip F. Hopkins, Stella S. R. Offner, Claude-André Faucher-Giguère

TL;DR

This erratum addresses the unphysical divergence of the previous Planck-mean opacity $κ_P(T_d,T_{rad})$ at low $T_{rad}$ by replacing the limited-range fit with an updated calculation and explicit $T_{rad}$ dependence. It clarifies that the dust opacity depends on both $T_{rad}$ and $T_d$ out of LTE and derives a consistent energy-balance framework in which absorption and emission use the appropriate temperature arguments. The authors compute $κ_P(T_d,T_{rad})$ and the Rosseland mean opacity from semenov_2003 tables across five $T_d$ regions, providing a practical on-the-fly interpolant and publicly releasing the supporting code and tables. This work improves the robustness and generality of dust radiative transfer in STARFORGE and related simulations, enabling more accurate thermal evolution and fragmentation predictions in star-forming environments.

Abstract

The model for the Planck-mean dust opacity $κ_{P}$ given in Appendix C of the STARFORGE simulations methods paper does not extrapolate well to low radiation temperature $T_{\rm rad}$, so we provide an updated calculation suitable for general use. We also clarify the role of the dust and radiation temperatures in setting the dust opacity, and provide code and calculations of the Planck- and Rosseland- mean dust opacity as a function of both the dust temperature $T_{\rm d}$ and the radiation temperature $T_{\rm rad}$.

Further correction to the STARFORGE methods paper: Planck-mean dust opacities

TL;DR

This erratum addresses the unphysical divergence of the previous Planck-mean opacity at low by replacing the limited-range fit with an updated calculation and explicit dependence. It clarifies that the dust opacity depends on both and out of LTE and derives a consistent energy-balance framework in which absorption and emission use the appropriate temperature arguments. The authors compute and the Rosseland mean opacity from semenov_2003 tables across five regions, providing a practical on-the-fly interpolant and publicly releasing the supporting code and tables. This work improves the robustness and generality of dust radiative transfer in STARFORGE and related simulations, enabling more accurate thermal evolution and fragmentation predictions in star-forming environments.

Abstract

The model for the Planck-mean dust opacity given in Appendix C of the STARFORGE simulations methods paper does not extrapolate well to low radiation temperature , so we provide an updated calculation suitable for general use. We also clarify the role of the dust and radiation temperatures in setting the dust opacity, and provide code and calculations of the Planck- and Rosseland- mean dust opacity as a function of both the dust temperature and the radiation temperature .

Paper Structure

This paper contains 3 sections, 6 equations, 2 figures.

Table of Contents

  1. The error
  2. Planck-mean dust opacities for emission and absorption
  3. Mean dust opacity as a function of $T_{\rm rad}$ and $T_{\rm d}$

Figures (2)

  • Figure 1: Planck-mean opacity as a function of both dust temperature $T_{\rm d}$ and radiation temperature $T_{\rm rad}$, computed from the monochromatic opacity tables of semenov_2003 for their 'porous 5-layered sphere' model. The dotted lines in corresponding colours plot the fit given in starforge_methods. The dashed line plots the Planck-mean opacity assuming $T_{\rm d} = T_{\rm rad}$, which disagrees with $\kappa_{\rm P}\left(T_{\rm d},T_{\rm rad}\right)$ in general.
  • Figure 2: Rosseland mean dust opacity as a function of both dust temperature $T_{\rm d}$ and radiation temperature $T_{\rm rad}$, computed from the opacity tables of semenov_2003 for their 'porous 5-layered sphere' model.