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

By B. Draine, Aigen Li. 2000

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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 in high- temperature transients. Because state-to-state transition rates are generally unavailable for complex mol ecules, we consider model polycyclic aromatic hydrocarbon (PAH), graphitic, and silicate grains with realistic vibrational mode spectra and realistic radiative properties. The vibrational density of states is used in a statistical-mechanical description of the emission process. Unlike previous treatments, our approach fully incorporates multiphoton heating effects, important for large grains or strong radiation fields. We discuss how the "temperature" of the grain is related to its vibrational energy. By comparing with an "exact" statistical calculation of the emission process, we determine the conditions under which the "thermal" and the "continuous cooling" approximations can be used to calculate the emission spec trum. We present results for the infrared emission spectra of PAH grains of various sizes heated by star light. We show how the relative strengths of the 6.2, 7.7, and 11.3 μm features depend on grain size, starlight spectrum and intensity, and grain charging conditions. We show results for grains in the "cold neutral medium" and "warm ionized medium" and representative conditions in photodissociation regions. Our model results are compared to observed ratios of emission features for the Milky Way and other galaxies and for the M17 and NGC 7023 photodissociation regions.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/a2f0402006874a689b3421e6248fb1a364e743cd

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Citations in the corpus

Interstellar Dust Models Consistent with Extinction, Emission, and Abundance Constraints (2003, methodology): “Draine & Li (2001) and Li & Draine (2001b) improved on this model by using a more realistic characterization of the optical properties of the PAHs, based on laboratory measurements.”
Dust Masses, PAH Abundances, and Starlight Intensities in the SINGS Galaxy Sample (2007, methodology): “…and tabulate the temperature distribution function dP/dT for the dust grain illuminated by the radiation field of equation (5) for selected values of U (with 0:1 U 107), using heat capacities, absorption cross sections, and numerical methods described by Draine & Li (2001), LD01, and DL07.”
The Infrared Spectral Energy Distribution of Normal Star-forming Galaxies: Calibration at Far-Infrared and Submillimeter Wavelengths (2000, background): “In fact, some of the dust emission is not even from dust in thermal equilibrium—polycyclic aromatic hydrocarbons (PAHs) and very small grains are stochastically heated (Draine & Li 2001).”
Modeling the Pan-Spectral Energy Distribution of Starburst Galaxies. I. The Role of ISM Pressure and the Molecular Cloud Dissipation Timescale (2004, methodology): “TheFIR em ission treatm entused in theM APPINGS IIIq code,whose resultsarepresented hereisbased on thealgorithm sofGuhathakurta& Draine(1989)(GD89)and Draine & Li(2001)(DL01).”
A HIGHLY CONSISTENT FRAMEWORK FOR THE EVOLUTION OF THE STAR-FORMING “MAIN SEQUENCE” FROM z ∼ 0–6 (2014, methodology): “In the IR, these templates most often are taken from Chary & Elbaz (2001) (CE01), Draine & Li (2001) (DL01), Dale & Helou (2002) (DH02), and Draine & Li (2007) (DL07).”
Infrared Emission from Interstellar Dust. II. The Diffuse Interstellar Medium (2000, unknown): “There is also an improved understanding of the heat capacities of dust candidate materials (Draine & Li 2001, hereafter DL01), the stochastic heating of very small grains (Barker & Cherchne† 1989 ; dÏHendecourt et al. 1989 ; DL01), the interstellar dust size distributions (Weingartner & Draine…”
AN ALMA SURVEY OF SUB-MILLIMETER GALAXIES IN THE EXTENDED CHANDRA DEEP FIELD SOUTH: PHYSICAL PROPERTIES DERIVED FROM ULTRAVIOLET-TO-RADIO MODELING (2015, background): “…the detailed PAH emission in SMGs may be different from our adopted template, and there may even be variations of the PAH emission between SMGs, since the strength of different features depends on factors such as the intensity of the radiation field and metallicity (e.g., Draine & Li 2001, 2007).”
ISM properties in low-metallicity environments. III. The dust spectral energy distributions of II Zw 40, He 2-10 and NGC 1140 (2005, unknown): “In recent dust models (Draine & Li 2001; Li & Draine 2001; Zubko et al. 2004), the carriers of the bump are both PAHs and solid carbonaceous grains.”
A refined model for spinning dust radiation (2008, background): “We follow Draine & Li (2001), hereafter DL01, for the number NH of H-atoms in the grains (see their Eq.”
Dust formation and survival in supernova ejecta (2007, unknown): “…1.06 (120, 300] 1.42 107 0.25 (300, 2000] 9.44 107 0 (2000,∞) AC 3.82 102 2 (0, 70] Chase et al. (1985) Zubko et al. (1996, ACAR) 3.27 103 1.50 (70, 300] Draine & Li (2001) 5.58 104 1.00 (300, 700] 1.09 107 0.19 (700, 3000] 5.09 107 0 (3000,∞) SiO2 9.95 102 2 (0, 60] Chase et al. (1985) Philipp…”
Scattering by Interstellar Dust Grains. II. X-Rays (2003, background): “Because of their small size, scattering by these grains is negligible, and the IR-opticalUV absorption can be calculated using absorption cross sections estimated for PAH molecules or ions (Draine & Li 2001; Li & Draine 2001).”
Analysis of the emission of very small dust particles from Spitzer spectro-imagery data using blind signal separation methods (2007, background): “The problem of calculating the infrared emission from VSGs in the ISM has been addressed by several authors (Désert et al. 1990; Siebenmorgen et al. 1992; Draine & Li 2001; Zubko et al. 2004).”
EFFICIENT THREE-DIMENSIONAL NLTE DUST RADIATIVE TRANSFER WITH SKIRT (2011, background): “As the intensity of the ISRF is the main parameter that drives the shape of the dust emissivity spectrum (Draine & Li 2001; Compiègne et al. 2011), 11 it is appropriate to choose NTeq somewhat larger than Nλ̄; the values we propose are NTeq = 25 and Nλ̄ = 10.”
THE EMISSION BY DUST AND STARS OF NEARBY GALAXIES IN THE HERSCHEL KINGFISH SURVEY (2011, background): “It has long been known that dust grains may be heated by old stars (see, e.g., Helou 1986; Sauvage & Thuan 1994; Calzetti et al. 1995; Kennicutt 1998; Draine & Li 2001); however, the clearly different Tdust − fdust/f∗ trend for early-types and spirals is a new result.”
The Mid-Infrared Spectrum of Star-forming Galaxies: Global Properties of Polycyclic Aromatic Hydrocarbon Emission (2006, methodology): “…photons to high temperatures (higher than their equilibrium temperatures; see Leger & Puget 1984; Draine & Anderson 1985; Allamandola et al. 1985; Draine & Li 2001), the emission spectrum produced by a single grain population is relatively insensitive to the strength and hardness of the exciting…”
Laboratory Infrared Spectroscopy of Cationic Polycyclic Aromatic Hydrocarbon Molecules (2003, background): “To a large extent, this may reflect that the carriers are likely to be ions and/or radicals (Allamandola et al. 1985; Bakes, Tielens, & Bauschilcher 2001a; Bakes et al. 2001b; Draine & Li 2001), i.e., species whose spectra are difficult to measure in the laboratory.”
Inverse Compton Origin of the Hard X-Ray and Soft Gamma-Ray Emission from the Galactic Ridge (2008, methodology): “The stochastic heating of grains smaller than ∼0.1 µm is treated using the “thermal continuous” approach of Draine & Li (2001); we calculate the equilibrium heating of larger dust grains by balancing absorption with re-emission as described by Li & Draine (2001).”
The CO-to-H2 Conversion Factor (2013, background): “…the translation of a SED into a dust mass relies almost entirely on dust grain properties (composition, mass emissivity, 30 size distribution) that have been derived for the Milky Way (Draine & Li 2001, 2007b), and are extremely uncertain even for local galaxies (e.g., Galliano et al. 2011).”
Spectroscopy of polycyclic aromatic hydrocarbons and very small grains in photodissociation regions (2005, background): “This has been calculated for very small carbonaceous (PAH-like) grains by Draine & Li (2001).”
Variations of the Mid-IR Aromatic Features inside and among Galaxies (2008, background): “With silicate and carbon grains, PAHs are a main component of dust models (Désert et al. 1990; Dwek et al. 1997; Draine & Li 2001; Zubko et al. 2004).”