Caire, W., J. D. Tyler, B. P. Glass, and M. A. Mares. MAMMALS OF OKLAHOMA. Univ. Oklahoma Press, Norman, xiii + 567 pp., illustrated, 1990. Price (hardbound), $29.95

Jones, J. Knox

doi:10.2307/1381814

Cited by 57 publications

(81 citation statements)

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“…In fact, observational evidence strongly suggests that carbon dust consists of hydrogenated amorphous carbon (HAC or a-C:H) materials that form around evolved stars, metamorphose there (e.g., Goto et al 2003) and further evolve in the ISM (e.g., Jones et al 1990;Pino et al 2008;Jones 2009). HAC material could also form directly into the ISM from the UV processing of ice mantles after leaving the dense medium as suggested by Greenberg et al (1995) or via direct accretion of carbon and hydrogen (e.g.…”

Section: The Nature Of Interstellar Carbon Grainsmentioning

confidence: 99%

The global dust SED: tracing the nature and evolution of dust with DustEM

Compiègne

Verstraete

Jones

et al. 2010

A&A

411

724

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The Planck and Herschel missions are currently measuring the far-infrared to millimeter emission of dust, which combined with existing IR data, will for the first time provide the full spectral energy distribution (SED) of the galactic interstellar medium dust emission, from the mid-IR to the mm range, with an unprecedented sensitivity and down to spatial scales ∼30 . Such a global SED will allow a systematic study of the dust evolution processes (e.g. grain growth or fragmentation) that directly affect the SED because they redistribute the dust mass among the observed grain sizes. The dust SED is also affected by variations of the radiation field intensity. Here we present a versatile numerical tool, DustEM, that predicts the emission and extinction of dust grains given their size distribution and their optical and thermal properties. In order to model dust evolution, DustEM has been designed to deal with a variety of grain types, structures and size distributions and to be able to easily include new dust physics. We use DustEM to model the dust SED and extinction in the diffuse interstellar medium at high-galactic latitude (DHGL), a natural reference SED that will allow us to study dust evolution. We present a coherent set of observations for the DHGL SED, which has been obtained by correlating the IR and HI-21 cm data. The dust components in our DHGL model are (i) polycyclic aromatic hydrocarbons; (ii) amorphous carbon and (iii) amorphous silicates. We use amorphous carbon dust, rather than graphite, because it better explains the observed high abundances of gas-phase carbon in shocked regions of the interstellar medium. Using the DustEM model, we illustrate how, in the optically thin limit, the IRAS/Planck HFI (and likewise Spitzer/Herschel for smaller spatial scales) photometric band ratios of the dust SED can disentangle the influence of the exciting radiation field intensity and constrain the abundance of small grains (a < ∼ 10 nm) relative to the larger grains. We also discuss the contributions of the different grain populations to the IRAS, Planck (and similarly to Herschel) channels. Such information is required to enable a study of the evolution of dust as well as to systematically extract the dust thermal emission from CMB data and to analyze the emission in the Planck polarized channels. The DustEM code described in this paper is publically available.

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Section: The Nature Of Interstellar Carbon Grainsmentioning

confidence: 99%

The global dust SED: tracing the nature and evolution of dust with DustEM

Compiègne

Verstraete

Jones

et al. 2010

A&A

411

724

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“…The accretion of C and H atoms in the diffuse ISM is often assumed to lead to the formation of a-C:H mantles on aromatic-rich carbonaceous dust surfaces (e.g., Jones et al 1990;Mennella et al 2002;Chiar et al 2013;Cecchi-Pestellini et al 2014a,b). The supposition of inner aromatic/outer aliphatic layering on carbonaceous dust has now been called into question in works that point out the likely dominant effects of UV photo-processing in the diffuse ISM 3 (Godard et al 2011;Jones 2012aJones ,b,c, 2013Jones et al 2013Jones et al , 2014.…”

Section: A-c:h Formationmentioning

confidence: 99%

Mantle formation, coagulation, and the origin of cloud/core shine

Jones

Koehler

Ysard

et al. 2016

A&A

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Context. The observed cloudshine and coreshine (C-shine) have been explained in terms of grain growth leading to enhanced scattering from clouds in the J, H, and K photometric bands and the Spitzer IRAC 3.6 and 4.5 μm bands. Aims. Using our global dust-modelling approach THEMIS (The Heterogeneous dust Evolution Model at the IaS), we explore the effects of dust evolution in dense clouds, through aliphatic-rich carbonaceous mantle formation and grain-grain coagulation. Methods. We model the effects of wide band gap a-C:H mantle formation and the low-level aggregation of diffuse interstellar medium dust in the moderately-extinguished outer regions of molecular clouds. Results. The formation of wide band gap a-C:H mantles on amorphous silicate and amorphous carbon (a-C) grains leads to a decrease in their absorption cross-sections but no change in their scattering cross-sections at near-infrared wavelengths, resulting in higher albedos. Conclusions. The evolution of dust, with increasing density and extinction in the diffuse-to-dense molecular cloud transition, through mantle formation and grain aggregation, appears to be a likely explanation for the observed C-shine.

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“…18 the same β(E g ) data is shown plotted in logarithmic form over a narrower range of E g in order to allow a comparison with β vs. T dust plots, where T dust could be considered a proxy for E g , implying that higher band gap materials are to be found in lower dust temperature-higher extinction regions, as might be expected by the accretion of increasingly hydrogen-rich a-C:H materials in denser regions of the ISM (e.g., Jones et al 1990). …”

Section: A-c(:h) Extinction and Absorptionmentioning

confidence: 99%

Variations on a theme – the evolution of hydrocarbon solids (Corrigendum)

Jones

2012

A&A

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Caire, W., J. D. Tyler, B. P. Glass, and M. A. Mares. MAMMALS OF OKLAHOMA. Univ. Oklahoma Press, Norman, xiii + 567 pp., illustrated, 1990. Price (hardbound), $29.95

Cited by 57 publications

References 0 publications

The global dust SED: tracing the nature and evolution of dust with DustEM

The global dust SED: tracing the nature and evolution of dust with DustEM

Mantle formation, coagulation, and the origin of cloud/core shine

Variations on a theme – the evolution of hydrocarbon solids (Corrigendum)

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