J/A+A/291/943 Protostellar cores (Ossenkopf+, 1994)
Dust opacities for protostellar cores
Ossenkopf V., Henning T.
<Astron. Astrophys. 291, 943 (1994)>
=1994A&A...291..943O 1994A&A...291..943O
ADC_Keywords: Protostars ; Extinction ; Interstellar medium
Keywords: ISM: dust, extinction - infrared: interstellar: continuum -
radio continuum: interstellar - stars: formation
Abstract:
Basing on the coagulation model of Ossenkopf (1993A&A...280..617O 1993A&A...280..617O),
we systematically computed and tabulated the opacity of dust in dense
protostellar cores between 1 micrometers and 1.3 mm. The possible
physical conditions were varied especially considering the influence
of different gas densities and molecular depletion ratios. In
comparison to the dust opacity in the diffuse interstellar medium, we
found nowhere changes by more than the factor 5 for ice-covered dust
grains. Possible uncertainties and deviations in environments with
different physical conditions are discussed. Although one may imagine
very special situations in which the dust opacity is changed by more
than a factor 10, for physically reasonable conditions in dense
protostellar cores, all possible deviations from the tabulated values
may not sum up to more than a factor of 2. Using these tables of dust
opacities, the submm continuum radiation of cold dust in protostellar
cores is a good tracer of their total mass.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 68 335 *Mass absorption coefficients for the particles
produced in the coagulation of an MRN distribution
(Mathis+Rumpl+Nordsieck, 1977ApJ...217..425M 1977ApJ...217..425M)
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Note on table1.dat: the file represents all dust opacities plotted in Fig. 5
of the paper. It is an expansion of Table 1 of the paper in the sense
that additional opacity files are given for the intermediate gas densities
n(H)=10^5 cm^-3 and 10^7 cm^-3.
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 5 E5.1 cm-3 n(H) Gas density (1)
8- 16 E9.3 um Lambda0 Vacuum wavelength of light
18- 26 E9.3 cm2/g Kappa0 Mass absorption coefficient of the whole
distribution of dust grains
29- 37 E9.3 um Lambda1 Vacuum wavelength of light with
thick ice mantles
39- 47 E9.3 cm2/g Kappa1 Mass absorption coefficient of the whole
distribution of dust grains with
thick ice mantles
50- 58 E9.3 um Lambda2 Vacuum wavelength of light with
thin ice mantles
60- 68 E9.3 cm2/g Kappa2 Mass absorption coefficient of the whole
distribution of dust grains with
thin ice mantles
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Note (1): n(H)=0 corresponds to initial MRN size distribution of grains
(see Mathis, Rumpl and Nordsieck, 1977ApJ...217..425M 1977ApJ...217..425M)
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History:
* 31-Aug-1994: Original version
* 12-Aug-2006: Gas density corrected in table1.
(End) Patricia Bauer [CDS] 31-Aug-1994