2016A&A...588A..44Y


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.05CEST08:57:08

2016A&A...588A..44Y - Astronomy and Astrophysics, volume 588A, 44-44 (2016/4-1)

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

YSARD N., KOHLER M., JONES A., DARTOIS E., GODARD M. and GAVILAN L.

Abstract (from CDS):

Context. Many dense interstellar clouds are observable in emission in the near-IR (J, H, and K photometric bands), commonly referred to as "Cloudshine", and in the mid-IR (Spitzer IRAC 3.6 and 4.5µm bands), the so-called "Coreshine". These C-shine observations have usually been explained in terms of grain growth but no model has yet been able to self-consistently explain the dust spectral energy distribution from the near-IR to the submm.
Aims. Our new core/mantle evolutionary dust model, The Heterogeneous dust Evolution Model at the IaS (THEMIS), has been shown to be valid in the far-IR and submm. We want to demonstrate its ability to reproduce the C-shine observations.
Methods. Our starting point is a physically motivated core/mantle dust model. It consists of three dust populations: small poly-aromatic-rich carbon grains, bigger core/mantle grains with mantles of aromatic-rich carbon, and cores made of either amorphous aliphatic-rich carbon or amorphous silicate. Then, we assume an evolutionary path where these grains, when entering denser regions, may first form a second aliphatic-rich carbon mantle (coagulation of small grains, accretion of carbon from the gas phase), second coagulate together to form large aggregates, and third accrete gas phase molecules coating them with an ice mantle. To compute the corresponding dust emission and scattering, we use a 3D Monte Carlo radiative transfer code.
Results. We show that our global evolutionary dust modelling approach THEMIS allows us to reproduce C-shine observations towards dense starless clouds. Dust scattering and emission is most sensitive to the cloud central density and to the steepness of the cloud density profile. Varying these two parameters leads to changes that are stronger in the near-IR, in both the C-shine intensity and profile.
Conclusions. With a combination of aliphatic-rich mantle formation and low-level coagulation into aggregates, we can self-consistently explain the observed C-shine and far-IR/submm emission towards dense starless clouds.

Abstract Copyright: © ESO, 2016

Journal keyword(s): ISM: general - dust, extinction - evolution

Simbad objects: 14

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Number of rows : 14

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 LDN 1448 DNe 03 22.5 +30 35           ~ 466 0
2 LDN 1451 DNe 03 26.1 +30 10           ~ 42 0
3 LDN 1471 DNe 03 48.0 +32 54           ~ 280 0
4 LDN 1506 DNe 04 20.0 +25 17           ~ 70 0
5 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 3478 0
6 TMC-1N MoC 04 41 21.3 +25 48 07           ~ 10 0
7 TMC-1 MoC 04 41 45.9 +25 41 27           ~ 1359 0
8 NAME Ori Region reg 05 35 17.30 -05 23 28.0           ~ 480 0
9 NAME Cha Dark Cloud SFR 11 55 -78.0           ~ 556 1
10 NAME Musca Cld 12 23 -71.3           ~ 156 0
11 LDN 134 MoC 15 53 36.3 -04 35 26           ~ 194 0
12 LDN 183 MoC 15 54 12.2 -02 49 42           ~ 682 1
13 NAME Lupus IV MoC 16 03 12.4 -42 07 43           ~ 125 0
14 NAME Cep Cloud SFR 22 00.0 +76 30           ~ 99 0

    Equat.    Gal    SGal    Ecl

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2020.07.05-08:57:08

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