Abstract
We investigate the physical conditions of the material around massive protostars by modelling the so-called hot molecular cores. We present a model for the spectral energy distribution (SED) as well as the ammonia line emission of the G31.41+0.31 hot core. We find that the best fit to the SED is achieved by assuming a density distribution corresponding to the collapse of a magnetized logatropic sphere. On the other hand, the line emission is reproduced by adopting a gas phase ammonia abundance increasing towards the center of the core, as a result of the release of the ammonia molecules trapped in ice grain mantles.
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Osorio, M., Anglada, G., Lizano, S. et al. A Model to Test the Internal Structure of the G31.41+0.31 Hot Molecular Core. Astrophysics and Space Science 292, 369–374 (2004). https://doi.org/10.1023/B:ASTR.0000045040.16017.e3
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DOI: https://doi.org/10.1023/B:ASTR.0000045040.16017.e3