2013A&A...558A..62J


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.04CEST01:09:07

2013A&A...558A..62J - Astronomy and Astrophysics, volume 558A, 62-62 (2013/10-1)

The evolution of amorphous hydrocarbons in the ISM: dust modelling from a new vantage point.

JONES A.P., FANCIULLO L., KOEHLER M., VERSTRAETE L., GUILLET V., BOCCHIO M. and YSARD N.

Abstract (from CDS):

The evolution of amorphous hydrocarbon materials, a-C(:H), principally resulting from ultraviolet (UV) photon absorption-induced processing, are likely at the heart of the variations in the observed properties of dust in the interstellar medium. The consequences of the size-dependent and compositional variations in a-C(:H), from aliphatic-rich a-C:H to aromatic-rich a-C, are studied within the context of the interstellar dust extinction and emission. Newly-derived optical property data for a-C(:H) materials, combined with that for an amorphous forsterite-type silicate with iron nano-particle inclusions, a-SilFe, are used to explore dust evolution in the interstellar medium. We present a new dust model that consists of a power-law distribution of small a-C grains and log-normal distributions of large a-SilFe and a-C(:H) grains. The model, which is firmly anchored by laboratory-data, is shown to quite naturally explain the variations in the infrared (IR) to far-ultraviolet (FUV) extinction, the 217nm UV bump, the IR absorption and emission bands and the IR-mm dust emission. The major strengths of the new model are its inherent simplicity and built-in capacity to follow dust evolution in interstellar media. We show that mantle accretion in molecular clouds and UV photo-processing in photo-dominated regions are likely the major drivers of dust evolution.

Abstract Copyright:

Journal keyword(s): dust, extinction - photon-dominated region - ISM: molecules

Simbad objects: 12

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Number of rows : 12

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 3478 0
2 NAME Trapezium Cluster As* 05 35 16.5 -05 23 14           ~ 1466 1
3 NAME Orion Bright Bar reg 05 35 22.30 -05 24 33.0           ~ 716 0
4 NAME Horsehead Nebula DNe 05 40 59.0 -02 27 30           ~ 445 0
5 NGC 2023 RNe 05 41 37.9 -02 15 52           ~ 570 1
6 M 82 IG 09 55 52.430 +69 40 46.93 9.61 9.30 8.41     ~ 5331 6
7 GCIRS 7 * 17 45 39.987 -29 00 22.24           M2 344 0
8 NAME Sgr A* X 17 45 40.03599 -29 00 28.1699           ~ 3446 3
9 NAME Gal Center reg 17 45 40.04 -29 00 28.1           ~ 11533 0
10 LHO 75 WR* 17 46 14.11 -28 49 36.7           WC9?d 20 0
11 WR 102dc WR* 17 46 14.69 -28 49 40.7           WC9d+OB 50 0
12 NAME M 17 SW SFR 18 20 23.1 -16 11 43           ~ 249 0

    Equat.    Gal    SGal    Ecl

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2020.07.04-01:09:07

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