Open AccessModelling submillimetre spectra of the protostellar infall candidates NGC 1333–IRAS 2 and Serpens SMM4
Author(s) -
WardThompson D.,
Buckley H.D.
Publication year - 2001
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1046/j.1365-8711.2001.04782.x
Subject(s) - physics , radiative transfer , astrophysics , protostar , serpens , line (geometry) , envelope (radar) , velocity dispersion , turbulence , rotation (mathematics) , star formation , atmospheric radiative transfer codes , stars , galaxy , mechanics , optics , geometry , telecommunications , radar , mathematics , computer science
We present a radiative transfer model, which is applicable to the study of submillimetre spectral line observations of protostellar envelopes. The model uses an exact, non‐LTE, spherically symmetric radiative transfer ‘Stenholm’ method, which numerically solves the radiative transfer problem by the process of ‘Λ‐iteration’. We also present submillimetre spectral line data of the Class 0 protostars NGC 1333–IRAS 2 and Serpens SMM4. We model the data using the Stenholm code. We examine the physical constraints which can be used to limit the number and range of parameters used in protostellar envelope models, and identify the turbulent velocity and tracer molecule abundance as the principal sources of uncertainty in the radiative transfer modelling. We explore the trends in the appearance of the predicted line profiles as key parameters in the models are varied, such as infall velocity profile, turbulence and rotation. The formation of the characteristic asymmetric double‐peaked line profile in infalling envelopes is discussed. We find that the separation of the two peaks of a typical infall profile is dependent not on the evolutionary status of the collapsing protostar, but on the turbulent velocity dispersion in the envelope . We also find that the line shapes can be significantly altered by rotation. Fits are found for the observed line profiles of IRAS 2 and SMM4 using plausible infall model parameters. The density and velocity profiles in our best‐fitting models are inconsistent with a singular isothermal sphere model (SIS), since for both objects modelled, the infall velocities appear further advanced than a SIS model would predict, given the density profile. We find better agreement with a form of collapse which assumes non‐static initial conditions, in agreement with other recent findings. We also find some evidence that the infall velocities are retarded from free‐fall towards the centre of the cloud, probably by rotation, and that the envelope of SMM4 is rotationally flattened.