Infrared Emission from Interstellar Dust. II. The Diffuse Interstellar Medium

@article{Li2000InfraredEF,
  title={Infrared Emission from Interstellar Dust. II. The Diffuse Interstellar Medium},
  author={Aigen Li and Bruce T. Draine},
  journal={The Astrophysical Journal},
  year={2000},
  volume={554},
  pages={778 - 802}
}
We present a quantitative model for the infrared emission from dust in the diffuse interstellar medium. The model consists of a mixture of amorphous silicate grains and carbonaceous grains, each with a wide size distribution ranging from molecules containing tens of atoms to large grains ≳1 μm in diameter. We assume that the carbonaceous grains have properties like polycyclic aromatic hydrocarbons (PAHs) at very small sizes and graphitic properties for radii a ≳ 50 Å. On the basis of recent… 

Interstellar dust models: Extinction, absorption and emission

The observational constraints on interstellar dust are summarized. A dust model, consisting of a mixture of amorphous silicate, graphite, and PAH material that reproduces the observed interstellar

Infrared Emission from Interstellar Dust. IV. The Silicate-Graphite-PAH Model in the Post-Spitzer Era

IR emission spectra are calculated for dust heated by starlight, for mixtures of amorphous silicate and graphitic grains, including varying amounts of PAH particles. The models are constrained to

Interstellar Dust Models Consistent with Extinction, Emission, and Abundance Constraints

We present new interstellar dust models that have been derived by simultaneously fitting the far-ultraviolet to near-infrared extinction, the diffuse infrared (IR) emission and, unlike previous

Modeling the Infrared Interstellar Extinction

Modeling the Infrared Emission from the HD 141569A Disk

We model the infrared (IR) emission from the double-ring disk of HD 141569A, using a porous dust model that was previously shown to be successful in reproducing the spectral energy distributions

A simple model to interpret the ultraviolet, optical and infrared emission from galaxies

We present a simple, largely empirical but physically motivated model to interpret the mid- and far-infrared spectral energy distributions of galaxies consistently with the emission at ultraviolet,

The Widespread Presence of Nanometer-size Dust Grains in the Interstellar Medium of Galaxies

Interstellar dust spans a wide range in size distribution, ranging from ultrasmall grains of a few Ångströms to micrometer-size grains. While the presence of nanometer-size dust grains in the

Three-component dust models for interstellar extinction

Interstellar extinction curves obtained from the ‘extinction without standard’ method were used to constrain the dust characteristics in the mean ISM (RV = 3.1), along the lines of sight through a

VERY LARGE INTERSTELLAR GRAINS AS EVIDENCED BY THE MID-INFRARED EXTINCTION

The sizes of interstellar grains are widely distributed, ranging from a few angstroms to a few micrometers. The ultraviolet (UV) and optical extinction constrains the dust in the size range of a

Global spectral energy distributions of the Large Magellanic Cloud with interstellar dust

The effects of dust on infrared emission vary among galaxies of different morphological types. We investigated integrated spectral energy distributions (SEDs) in infrared and submillimeter/millimeter
...

References

SHOWING 1-10 OF 129 REFERENCES

Infrared Emission from Interstellar Dust. I. Stochastic Heating of Small Grains

We present a method for calculating the infrared emission from a population of dust grains heated by starlight, including very small grains for which stochastic heating by starlight photons results

Detection and Characterization of Cold Interstellar Dust and Polycyclic Aromatic Hydrocarbon Emission, from COBE Observations

Using data obtained by the DIRBE instrument on the COBE spacecraft, we present the mean 3.5-240 μm spectrum of high-latitude dust. Combined with a spectrum obtained by the FIRAS instrument, these

Temperature fluctuations in interstellar grains. I. Computational method and sublimation of small grains

A technique is presented for calculating the temperature distribution of interstellar dust grains in the presence of a radiation field or collisional heating by a hot gas, or both. The distribution

Radiative Transfer Analysis of Far-Ultraviolet Background Observations Obtained with the Far Ultraviolet Space Telescope

In 1992, the Far Ultraviolet Space Telescope provided measurements of the ultraviolet (140-180 nm) diffuse sky background at high, medium, and low Galactic latitudes. A significant fraction of the

Dust Grain-Size Distributions and Extinction in the Milky Way, Large Magellanic Cloud, and Small Magellanic Cloud

We construct size distributions for carbonaceous and silicate grain populations in different regions of the Milky Way, LMC, and SMC. The size distributions include sufficient very small carbonaceous

Far-Infrared Spectral Observations of the Galaxy by COBE

We derive Galactic continuum spectra from 5-96 cm(-1) fromCOBE/FIRAS observations. The spectra are dominated by warm dust emission,which may be fitted with a single temperature in the range 16-21 K

Dust Grain Size Distributions and Extinction in the Milky Way, LMC, and SMC

We construct size distributions for carbonaceous and silicate grain populations in different regions of the Milky Way, LMC, and SMC. The size distributions include sufficient very small carbonaceous

The Near-Infrared Interstellar Silicate Bands and Grain Theories

With nonporous spherical grains, the interstellar 9.7 and 18 μm silicate bands are observed to be too strong to be compatible with laboratory silicates if the interstellar medium has an abundance of

Infrared Properties of Molecular Cirrus. II. Cloud-to-Cloud Variations in Graphite and Polycyclic Aromatic Hydrocarbon Content

We have conducted a photometric survey of translucent molecular clouds in the four IRAS wave bands. We find notable cloud-to-cloud variations in mid-IR emission, with the ratio I12/I25 varying by up

The albedo and scattering phase function of interstellar dust and the diffuse background at far-ultraviolet wavelengths.

Evidence is presented that, as the Galactic neutral hydrogen column density approaches zero, the FUV continuum background arises primarily from scattering by dust, which implies that dust may be present in virtually all view directions.
...