Evolutionary Models of the Formation of Protostars out of Low-Mass, Dense Cores: Towards Reconciling Models and Observations

Details Evolutionary Models of the Formation of Protostars out of Low-Mass, Dense Cores: Towards Reconciling Models and Observations Evolutionary Models of the Formation of Protostars out of Low-Mass, Dense Cores: Towards Reconciling Models and Observations

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21535502d&link_type=abstract

American Astronomical Society, AAS Meeting #215, #355.02; Bulletin of the American Astronomical Society, Vol. 42, p.538

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We present a set of evolutionary models describing the collapse of low-mass, dense cores into protostars. We use as our starting point the evolutionary model following the inside-out collapse of a singular isothermal sphere as presented by Young & Evans 2005. We calculate the radiative transfer of the collapsing core throughout the full duration of the collapse in two dimensions, and from the results we calculate evolutionary indicators to directly compare to observations. We incorporate several modifications and additions to the original Young & Evans model in an effort to better match observations with model predictions: (1) we include the opacity from scattering in the radiative transfer, (2) we include a circumstellar disk directly in the two-dimensional radiative transfer, (3) we include a two-dimensional envelope structure, taking into account the effects of rotation, (4) we include mass-loss and the opening of outflow cavities, and (5) we include a simple treatment of episodic accretion. We find that two-dimensional geometry, mass-loss, and outflow cavities all affect the model predictions, as expected, but none resolve the discrepancies between model predictions and observations, specifically the long-standing luminosity problem whereby the models fail to capture all but the upper end of the distribution of observed sources in luminosity. On the other hand, we find that a cycle of episodic mass accretion similar to that predicted by recent theoretical work can resolve this luminosity problem and bring the model predictions in better agreement with observations.

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