2002A&A...389..908J


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.02CEST13:22:59

2002A&A...389..908J - Astronomy and Astrophysics, volume 389, 908-930 (2002/7-3)

Physical structure and CO abundance of low-mass protostellar envelopes.

JORGENSEN J.K., SCHOEIER F.L. and VAN DISHOECK E.F.

Abstract (from CDS):

We present 1D radiative transfer modelling of the envelopes of a sample of 18 low-mass protostars and pre-stellar cores with the aim of setting up realistic physical models, for use in a chemical description of the sources. The density and temperature profiles of the envelopes are constrained from their radial profiles obtained from SCUBA maps at 450 and 850µm and from measurements of the source fluxes ranging from 60µm to 1.3mm. The densities of the envelopes within ∼10000AU can be described by single power-laws ρ∝r–α for the class 0 and I sources with α ranging from 1.3 to 1.9, with typical uncertainties of ±0.2. Four sources have flatter profiles, either due to asymmetries or to the presence of an outer constant density region. No significant difference is found between class 0 and I sources. The power-law fits fail for the pre-stellar cores, supporting recent results that such cores do not have a central source of heating. The derived physical models are used as input for Monte Carlo modelling of submillimeter C18O and C17O emission. It is found that class I objects typically show CO abundances close to those found in local molecular clouds, but that class 0 sources and pre-stellar cores show lower abundances by almost an order of magnitude implying that significant depletion occurs for the early phases of star formation. While the 2-1 and 3-2 isotopic lines can be fitted using a constant fractional CO abundance throughout the envelope, the 1-0 lines are significantly underestimated, possibly due to contribution of ambient molecular cloud material to the observed emission. The difference between the class 0 and I objects may be related to the properties of the CO ices.

Abstract Copyright:

Journal keyword(s): stars: formation - ISM: molecules - ISM: abundances - stars: circumstellar matter - radiative transfer - astrochemistry

Simbad objects: 29

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Number of rows : 29

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 LDN 1448 IRS 2 Y*O 03 25 22.32 +30 45 13.9           ~ 116 0
2 [SDA2014] West4 Y*O 03 25 38.83 +30 44 06.2           ~ 242 1
3 NAME LDN 1448-mm Y*O 03 25 38.83 +30 44 06.2           ~ 301 0
4 NAME [BM89] L1450D DNe 03 28 36.8 +31 15 20           ~ 51 0
5 IRAS 03258+3104 Y*O 03 28 55.30 +31 14 27.8           ~ 158 1
6 [JCC87] IRAS 2A Y*O 03 28 55.55 +31 14 36.7           ~ 390 3
7 [JCC87] IRAS 4A Y*O 03 29 10.49 +31 13 30.8           ~ 595 1
8 [JCC87] IRAS 4 FIR 03 29 10.9 +31 13 26           ~ 464 0
9 NGC 1333 OpC 03 29 11 +31 18.6           ~ 1218 1
10 [JCC87] IRAS 4B Y*O 03 29 12.058 +31 13 02.05           ~ 553 0
11 LDN 1450 DNe 03 29.6 +31 20           ~ 58 0
12 Ass Per OB 2 As* 03 42.2 +33 26           ~ 305 0
13 LDN 1489 DNe 04 04 47.5 +26 19 42           ~ 195 0
14 RAFGL 5123 FU* 04 31 34.07736 +18 08 04.9020           K3V/M3III 810 0
15 IRAS 04361+2547 Y*O 04 39 13.89767 +25 53 20.6340           ~ 185 1
16 IRAS 04365+2535 Y*O 04 39 35.19360 +25 41 44.7252           ~ 236 0
17 LDN 1527 DNe 04 39 53 +25 45.0           ~ 494 0
18 TMC-1 MoC 04 41 45.9 +25 41 27           ~ 1358 0
19 LDN 1544 DNe 05 04 16.6 +25 10 48           ~ 680 0
20 NAME [BM89] L1544 cor 05 04 22.5 +25 11 36           ~ 434 1
21 NAME VLA 1623-243 Y*O 16 26 26.42 -24 24 30.0           ~ 372 0
22 [SSG2006] MMS002 smm 16 26 26.50 -24 24 30.9           ~ 241 0
23 IRAS 16293-2422 cor 16 32 22.56 -24 28 31.8           ~ 1035 1
24 LDN 1689B DNe 16 34 42.1 -24 36 11           ~ 138 0
25 LDN 483 DNe 18 17 35 -04 39.8           ~ 209 0
26 LDN 723 DNe 19 18 12 +19 13.6           ~ 153 0
27 LDN 1157 DNe 20 39 06.4 +68 02 13           ~ 483 0
28 V* V1610 Cyg pA* 21 02 18.27 +36 41 37.0           F5Iae 829 1
29 LDN 1262 MoC 23 25 47 +74 17.6           ~ 130 0

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2020.07.02-13:22:59

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