# 2010A&A...516A.102C

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 Query : 2010A&A...516A.102C

2010A&A...516A.102C - Astronomy and Astrophysics, volume 516, A102-102 (2010/6-3)

Physical structure of the envelopes of intermediate-mass protostars.

CRIMIER N., CECCARELLI C., ALONSO-ALBI T., CASELLI P., FUENTE A., JOHNSTONE D., KAHANE C., LEFLOCH B., MARET S., PLUME R., RIZZO J.R., TAFALLA M., VAN DISHOECK E. and WYROWSKI F.

Abstract (from CDS):

Intermediate mass protostars provide a bridge between low- and high-mass protostars. Furthermore, they are an important component of the UV interstellar radiation field. Despite their relevance, little is known about their formation process. We present a systematic study of the physical structure of five intermediate mass, candidate Class 0 protostars. Our two goals are to shed light on the first phase of intermediate mass star formation and to compare these protostars with low- and high-mass sources. We derived the dust and gas temperature and density profiles of the sample. We analysed all existing continuum data on each source and modelled the resulting SED with the 1D radiative transfer code DUSTY. The gas temperature was then predicted by means of a modified version of the code CHT96. We found that the density profiles of five out of six studied intermediate mass envelopes are consistent with the predictions of the inside-out'' collapse theory. We compared several physical parameters, like the power law index of the density profile, the size, the mass, the average density, the density at 1000 AU and the density at 10 K of the envelopes of low-, intermediate, and high-mass protostars. When considering these various physical parameters, the transition between the three groups appears smooth, suggesting that the formation processes and triggers do not substantially differ.

Journal keyword(s): stars: formation

Full paper

 Number of rows : 18
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 [CB88] 3-1 MoC 00 28 42.17 +56 41 57.4           ~ 6 0
2 LBN 119.83-06.05 MoC 00 28 43.5075 +56 41 56.868           ~ 69 0
3 NAME Per Arm PoG 03 30 +45.0           ~ 1442 0
4 V* V2457 Ori Or* 05 35 26.97000 -05 09 54.4644         18.858 ~ 145 0
5 HH 212 HH 05 43 51.41 -01 02 53.1           ~ 364 1
6 IRAS 16293-2422 cor 16 32 22.56 -24 28 31.8           ~ 1201 1
7 NAME Serpens Cloud SFR 18 29 49 +01 14.8           ~ 1059 2
8 NAME SH 2-68 FIR 1 cor 18 29 49.63 +01 15 21.9           ~ 262 2
9 HD 206267 SB* 21 38 57.6195772032 +57 29 20.554016280 5.09 5.83 5.62   5.56 O6.0V((f))+O9:V 487 0
10 IC 1396 OpC 21 38 59 +57 30.8           ~ 479 1
11 [BGE2002] BIMA 1 Y*O 21 40 39.67 +58 16 06.2           ~ 17 0
12 [BGE2002] BIMA 2 Y*O 21 40 42.36 +58 16 09.7           ~ 118 0
13 NAME IC 1396 North CGb 21 40 42.6537 +58 16 01.882           ~ 188 1
14 [BGE2002] BIMA 3 Y*O 21 40 42.77 +58 16 01.1           ~ 18 0
15 NGC 7129 OpC 21 42 58 +66 06.8     11.5     ~ 255 0
16 NAME NGC 7129 FIR 2 IR 21 44 01.5 +66 03 40           ~ 94 0
17 NAME Cep E HII 23 03 12.779 +61 42 25.75           ~ 166 0
18 NAME III CEP ASSOC As* 23 04.2 +63 24           ~ 316 0

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2023.03.21-00:16:50