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J/A+A/291/943       Protostellar cores                        (Ossenkopf+, 1994)
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Dust opacities for protostellar cores
       Ossenkopf V., Henning T.
      <Astron. Astrophys. 291, 943 (1994)>
      =1994A&A...291..943O      (SIMBAD/NED Reference)
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ADC_Keywords: Protostars; Extinction
Keywords: ISM: dust, extinction - infrared: interstellar: continuum -
          radio continuum: interstellar - stars: formation

Abstract:
    Basing on the coagulation model of Ossenkopf (1993), 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          68        335   *Mass absorption coefficients for the particles
                                  produced in the coagulation of an MRN
                                  distribution
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Note on table1: table1 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
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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
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(End)                                       Patricia Bauer   [CDS]   31-Aug-1994