Evolution of dust properties in an interstellar filament

By B. Stepnik, Alain Abergel, J. Bernard, F. Boulanger, L. Cambrésy, M. Giard, A. Jones, G. Lagache, J. Lamarre, C. Meny and 5 more. 2003

227 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atmospheric Science

View Paper: https://www.semanticscholar.org/paper/601d1767589d8a2bd005becfbaa519b4a8eba82d

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Infrared Extinction toward Nearby Star-forming Regions (2007, background): “The lack of emission from small grains has been observed along lines of sight with high column densities (Stepnik et al. 2003; del Burgo et al. 2003; Cambresy et al. 2005) suggesting grain growth leading to porous grains with enhanced emissivity within these clouds.”
ISM properties in low-metallicity environments II. The dust spectral energy distribution of NGC 1569 (2003, background): “This has been invoked to explain the elevated opacity of circumstellar dusty envelopes and dense molecular cores (Ossenkopf & Henning 1994; Stepnik et al. 2003).”
THE CO-TO-H2 CONVERSION FACTOR FROM INFRARED DUST EMISSION ACROSS THE LOCAL GROUP (2011, background): “The origin of this enhanced emissivity is thought to be a change in the size distribution of dust, with “fluffy,” low-albedo grains created in dense environments (Dwek 1997; Stepnik et al. 2003; Cambrésy et al. 2005).”
Inverse temperature dependence of the dust submillimeter spectral index (2003, methodology): “This experiment has observed various phases of the interstellar medium, from diffuse clouds in Polaris (Bernard et al. 1999) and Taurus (Stepnik et al. 2003) to massive star-forming regions in Orion (Ristorcelli et al. 1998 and Dupac et al. 2001), Messier 17 (Dupac et al. 2002), Cygnus B, and the du”
The global dust SED: tracing the nature and evolution of dust with DustEM (2010, background): “…abundance betweenth PAH band emitters and the mid-IR continuum emitters (SamC in our 6 This process has been shown to alter the sub-mm opacity by factors 2 to 3 (Stepnik et al. 2003; Paradis et al. 2009a). case) is known to vary (e.g Berné et al. 2007; Compiègne et al. 2008; Flagey et al. 2009).”
Probing the dust properties of galaxies up to submillimetre wavelengths. II. Dust-to-gas mass ratio trends with metallicity and the submm excess in dwarf galaxies (2011, methodology): “Within the ISM, dust undergoes constructive processes of accretion or coagulation (Stepnik et al. 2003; Hirashita & Omukai 2009) or destructive/disruptive processes of vaporisation, fragmentation, erosion and shattering (Jones et al. 1994, 1996).”
IRIS: A New Generation of IRAS Maps (2004, background): “Several studies of dust emission at high Galactic latitudes showed large variations of dust properties at all scales, even in the diffuse interstellar medium (Boulanger et al. 1990; Lagache et al. 1998; Bernard et al. 1999; Miville-Deschênes et al. 2002a; Stepnik et al. 2003).”
Planckintermediate results (2013, unknown): “It can stem from dust evolution, where dust properties change with environment, and which has been invoked to explain a roughly 3-fold increase in dust emissivity in molecular regions (Stepnik et al. 2003; Martin et al. 2012; Roy et al. 2013; Planck Collaboration Int.”
Planck 2013 results. XI. All-sky model of thermal dust emission (2013, methodology): “Many studies have revealed increases of the dust emissivity with (column) density in molecular clouds accompanied by a decrease in dust temperature (Stepnik et al. 2003; Schnee et al. 2008; Planck Collaboration XXV 2011; Arab et al. 2012; Martin et al. 2012; Roy et al. 2013).”
Cold Dark Clouds: The Initial Conditions for Star Formation (2007, background): “…of a filament in Taurus by the PRONAOS balloon-borne experiment suggest that at the highest densities, the population of smallest grains disappears and the submillimeter emissivity increases by a factor of about 3, as expected by models of dust coagulation into fluffy grains (Stepnik et al. 2003).”
Chemical modeling of L183 (= L134N) : an estimate of the ortho/para H2 ratio (2008, background): “We can see that N2D+/N2H+ ratios above 100 are possible in dense gas though they require very low electronic abundances and therefore very small grains which are probably absent from these dense and cold regions due to grain coagulation (see e.g. Stepnik et al. 2003).”
Dust coagulation and fragmentation in molecular clouds. I. How collisions between dust aggregates alter the dust size distribution (2009, background): “Likewise, evidence for grain coagulation is also provided by a comparison of visual absorption studies (e.g., star counts) and sub-millimeter emission studies which imply that the smallest grains have been removed e ﬃ ciently from the interstellar grain size distribution (Stepnik et al. 2003).”
Are PAHs precursors of small hydrocarbons in photo-dissociation regions? The Horsehead case (2005, background): “Stepnik et al. (2003) describe a convincing case for such a process in a small filament of the Taurus cloud.”
Non-standard grain properties, dark gas reservoir, and extended submillimeter excess, probed by Herschel in the Large Magellanic Cloud (2011, background): “…interpreted as variations of the grain size distribution (Draine, 2003a; Fitzpatrick & Massa, 2005); (iii) coagulation occurs in dense regions (e.g. Stepnik et al., 2003; Berné et al., 2007); (iv) blast waves are responsible for grain fragmentation and erosion in the low-velocity phase (Jones et…”
DEVELOPMENT OF THE MODEL OF GALACTIC INTERSTELLAR EMISSION FOR STANDARD POINT-SOURCE ANALYSIS OF FERMI LARGE AREA TELESCOPE DATA (2016, background): “…of the ISM due to the good penetration of CRs at the GeV-TeV energies relevant for the LAT (Skilling & Strong 1976), dust opacity (optical depth per gas nucleon) is known to increase from the diffuse H I to dense H I and H2 gas (Stepnik et al. 2003; Abergel et al. 2013, 2014; Ade et al. 2014b).”
THE MAGELLANIC MOPRA ASSESSMENT (MAGMA). I. THE MOLECULAR CLOUD POPULATION OF THE LARGE MAGELLANIC CLOUD (2011, background): “I. 9 10 that the FIR emissivity of dust grains is enhanced in regions of higher gas density (e.g., Bernard et al. 1999; Stepnik et al. 2003; Paradis et al. 2009; Planck Collaboration et al. 2011), which would cause the dust-based approach to overestimate the amount of molecular gas.”
The global dust modelling framework THEMIS (The Heterogeneous dust Evolution Model for Interstellar Solids) (2017, background): “As they noted the dust emissivity needs to be higher by about a factor of three, which is consistent with the results of Stepnik et al. (2003), Köhler et al. (2012) and, more particularly, with those of Köhler et al. (2015) for the onset of dust aggregation, i.e. the CM→CMM→AMM dust evolution of…”
THE EFFECT OF LINE-OF-SIGHT TEMPERATURE VARIATION AND NOISE ON DUST CONTINUUM OBSERVATIONS (2009, methodology): “Published data of sources in Taurus and Orion by Stepnik et al. (2003) and Dupac et al. (2001), respectively, show these apparent trends, but an isothermal description with no systematic variations in β still cannot be strictly ruled out, due to the uncertainties.”
Far-infrared to millimeter astrophysical dust emission. I. A model based on physical properties of a (2007, methodology): “…1995; Finkbeiner et al. 1999; Galliano et al. 2003) or for substantial modifications of dust properties in the submillimeter with respect to predictions of standard dust models (e.g. Ristorcelli et al. 1998; Bernard et al. 1999; Stepnik et al. 2003a; Dupac et al. 2001; Dupac et al. 2002, 2003a).”
Determination of the gas-to-dust ratio in nearby dense clouds using X-ray absorption measurements (2003, background): “In particular,RV is expected to increase in cold, dense molecular clouds (Cardelli et al. 1989) where grain coagulation probably occurs (Stepnik et al. 2003).”