Spectral energy of first protostellar cores: Detecting 'class -I' protostars with ISO and SIRTF

Details Spectral energy of first protostellar cores: Detecting 'class -I' protostars with ISO and SIRTF Spectral energy of first protostellar cores: Detecting 'class -I' protostars with ISO and SIRTF

Feb 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995apj...439l..55b&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 439, no. 2, p. L55-L58

Astronomy and Astrophysics

Astronomy

56

Far Infrared Radiation, Hydrodynamic Equations, Mathematical Models, Protostars, Spectral Energy Distribution, Star Formation, Stellar Cores, Computerized Simulation, Infrared Astronomy, Infrared Astronomy Satellite, Infrared Space Observatory (Iso), Space Infrared Telescope Facility

Scientific paper

Radiative hydrodynamical models of protostellar collapse are used to calculate the spectral energy distributions of single and binary protostars at the phase of formation of the first (outer) protostellar core. In accordance with the established nomenclature, where classes 0, I, II, and III form a sequence in time, we term these pre-class 0 objects to be class-I ('class minus one') objects. These class -I objects are characterized by central core temperatures of approximately 200 K, envelope temperatures of approximately 10 K, and substantial far-infrared and submillimeter-wave fluxes. While undetectable by IRAS, these objects should be detectable by Infrared Space Observatory (ISO) and Space Infrared Telescope Facility (SITF) at 60 micrometer and longer wavelengths. First protostellar cores exist for times on the order of a few percent of the total collapse time, implying that a small fraction of all protostellar objects should be class -I objects.

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