Radiatively induced star formation

Abstract

view Abstract Citations (23) References (9) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Radiatively induced star formation Larosa, T. N. Abstract A model is presented for the compression of molecular-cloud clumps subjected to ionizing radiation and the pressure of the associated hot gas. This model is applicable to clumps of arbitrary mass. They are taken to be spherical, and are characterized by supersonic, turbulent, internal velocities that scale with the clump radii. For a significant range of clump radii, these clumps implode when subjected even for short times to pressures likely to be produced by H II regions. The occurrence of implosion depends primarily on the ratio of external to internal pressures. The effect of self-gravity was included but was not found to be important. Since the internal velocities increase with the clump radii, smaller clumps are more likely to implode. It is found that implosion is inevitable for clumps with radii less than 1 pc and densities greater than 1000/cu cm. (Lower-density clumps would evaporate.) Such a result indicates that this process may be an important star formation mechanism. Publication: The Astrophysical Journal Pub Date: November 1983 DOI: 10.1086/161494 Bibcode: 1983ApJ...274..815L Keywords: Molecular Clouds; Nebulae; Radiative Transfer; Star Formation; Astronomical Models; Clumps; H Ii Regions; Implosions; Shock Waves; Astrophysics full text sources ADS |