Parameterizing the interstellar dust temperature

Abstract

The temperature of interstellar dust particles is of great importance to astronomers. It plays a crucial role in the thermodynamics of interstellar clouds, because of the gas-dust collisional coupling. It is also a key parameter in astrochemical studies that governs the rate at which molecules form on dust. In 3D (magneto)hydrodynamic simulations often a simple expression for the dust temperature is adopted, because of computational constraints, while astrochemical modelers tend to keep the dust temperature constant over a large range of parameter space. Our aim is to provide an easy-to-use parametric expression for the dust temperature as a function of visual extinction ($A_{\mathrm{V}}$) and to shed light on the critical dependencies of the dust temperature on the grain composition. We obtain an expression for the dust temperature by semi-analytically solving the dust thermal balance for different types of grains and compare to a collection of recent observational measurements. We also explore the effect of ices on the dust temperature. Our results show that a mixed carbonaceous-silicate type dust with a high carbon volume fraction matches the observations best. We find that ice formation allows the dust to be warmer by up to 15% at high optical depths ($A_{\mathrm{V}}>20$ mag) in the interstellar medium. Our parametric expression for the dust temperature is presented as $T_{\mathrm{d}}=\left[11+5.7\times \tanh (0.61-{\log }_{10}(A_{\mathrm{V}}))\right]{\chi }_{\mathrm{uv}}^{1/5.9}$, where ${\chi }_{\mathrm{uv}}$ is in units of the Draine (1978) UV field

16 pages, 17 figures, 4 tables. Accepted for publication in A&A. Version 2: the omission of factor 0.921 in equation 4 is corrected

References in corpus (22)

• Complex Chemistry in Star-Forming Regions: An Expanded Gas-Grain Warm-up Chemical Model
• Formation of methyl formate and other organic species in the warm-up phase of hot molecular cores
• The evolution of amorphous hydrocarbons in the ISM: dust modelling from a new vantage point
• Herschel Survey of Galactic OH+, H2O+, and H3O+: Probing the Molecular Hydrogen Fraction and Cosmic-Ray Ionization Rate
• Modeling Complex Organic Molecules in dense regions: Eley-Rideal and complex induced reaction
• Inverse Compton Emission from Galactic Supernova Remnants: Effect of the Interstellar Radiation Field
• Gas-grain chemistry in cold interstellar cloud cores with a microscopic Monte Carlo approach to surface chemistry
• Detection of interstellar hydrogen peroxide
• The Earliest Phases of Star formation observed with Herschel (EPoS): The dust temperature and density distributions of B68
• The properties of the 2175AA extinction feature discovered in GRB afterglows
• Impulsive Spot Heating and Thermal Explosion of Interstellar Grains Revisited
• Monte Carlo simulations of H2 formation on stochastically heated grains
• The infrared emission spectra of compositionally inhomogeneous aggregates composed of irregularly shaped constituents
• Detection of the hydroperoxyl radical HO2 toward ρOph A: Additional constraints on the water chemical network
• Evidence for Large Grains in the Star-forming Filament OMC-2/3
• Dust Emission from the Perseus Molecular Cloud
• Combining radiative transfer and diffuse interstellar medium physics to model star formation
• Estimating Column Density in Molecular Clouds with FIR and Sub-mm Emission Maps
• Prestellar core modeling in the presence of a filament - The dense heart of L1689B
• The Earliest Phases of Star formation (EPoS): Temperature, density, and kinematic structure of the star-forming core CB 17
• The physical state of selected cold clumps
• Mass estimates for very cold (< 8 K) gas in molecular cloud cores

Cited by in corpus (46)

• Photodissociation and X-Ray Dominated Regions
• Gas phase Elemental abundances in Molecular cloudS (GEMS) I. The prototypical dark cloud TMC 1
• The complex chemistry of hot cores in Sagittarius B2(N): Influence of cosmic-ray ionization and thermal history
• Gas phase Elemental abundances in Molecular cloudS (GEMS). II. On the quest for the sulphur reservoir in molecular clouds: the $H_{2}S$ case
• Gas phase Elemental abundances in Molecular cloudS (GEMS) VII. Sulfur elemental abundance
• ALMA observations of fragmentation, sub-structure, and protostars in high-mass starless clump candidates
• A pathway to peptides in space through the condensation of atomic carbon
• Gas and dust temperature in pre-stellar cores revisited: New limits on cosmic-ray ionization rate
• ALMA observations of doubly deuterated water: Inheritance of water from the prestellar environment
• Identification of prestellar cores in high-mass star forming clumps via ${\mathrm{H}}_2{\mathrm{D}}^{+}$ observations with ALMA
• Chemistry and physics of a low-metallicity hot core in the Large Magellanic Cloud
• The efficiency of photodissociation for molecules in interstellar ices
• Characterizing the line emission from molecular clouds. II. A comparative study of California, Perseus, and Orion A
• Is there any linkage between interstellar aldehyde and alcohol?
• Formation of the simplest amide in molecular clouds: formamide (NH${}_2$CHO) and its derivatives in H${}_2$O-rich and CO-rich interstellar ice analogs upon VUV irradiation
• Water and Methanol Ice in L1544
• Modeling chemistry during star formation: Water deuteration in dynamic star-forming regions
• The KOSMA-$\tau$ PDR Model -- I. Recent updates to the numerical model of photo-dissociated regions
• Chemical and radiative transfer modeling of Propylene Oxide
• The connection between warm carbon chain chemistry and interstellar irradiation of star-forming cores
• A 3D physico-chemical model of a pre-stellar core. I. Environmental and structural impact on the distribution of CH${}_3$OH and $c$-C${}_3$H${}_2$
• Chemical significance of different temperature regimes for cosmic-ray-induced heating of whole interstellar grains
• Modelling methanol and hydride formation in the JWST Ice Age era
• Chemical evolution of the gas in C-type shocks in dark clouds
• Astrochemical models of interstellar ices: History matters
• Ice mantles on dust grains: dramatic variation of thickness with grain size
• Temperature spectra of interstellar dust grains heated by cosmic-rays II: dark cloud cores
• Infrared dust arcs around the stars: I. effect of the radiation pressure
• The first frost in the Pipe Nebula
• Broadband spectroscopy of astrophysical ice analogues: II. Optical constants of CO and CO${}_2$ ices in the terahertz and infrared ranges
• Simulated observations of star formation regions: infrared evolution of globally collapsing clouds
• Three dimensional projection effects on chemistry in a Planck galactic cold clump
• Dust properties of the cometary globule Barnard 207 (LDN 1489)
• Compact dusty clouds and efficient H${}_2$ formation in diffuse ISM
• C-type shock modelling -- the effect of new H${}_2$-H collisional rate coefficients
• GGCHEMPY: A pure Python-based gas-grain chemical code for efficient simulation of interstellar chemistry
• Modelling thermochemical processes in protoplanetary disks I: numerical methods
• Constraints on the non-thermal desorption of methanol in the cold core LDN 429-C
• A multigrain-multilayer astrochemical model with variable desorption energy for surface species
• The Cosmic-Ray Induced Sputtering Process On Icy Grains
• Cosmic-ray-driven enhancement of the C${}^0$/CO abundance ratio in W51C
• Chemical constraints on the dynamical evolution of the cold core L694
• Impact of ice growth on the physical and chemical properties of dense cloud cores
• Effects of grain temperature distribution on organic protostellar envelope chemistry
• Fine-tuning the complex organic molecule formation: sulfur and CO ice as regulators of surface chemistry
• The cosmic journey of dust grains -- from nucleation to planetary system