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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
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), 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:
FileName Lrecl Records Explanations
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)
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.
Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
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
Note (1): n(H)=0 corresponds to initial MRN size distribution of grains (see Mathis, Rumpl and Nordsieck, 1977ApJ...217..425M)
History: * 31-Aug-1994: Original version * 12-Aug-2006: Gas density corrected in table1.
(End) Patricia Bauer [CDS] 31-Aug-1994
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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