Tracing the physical and chemical evolution of low-mass protostars Jørgensen, J.K.

nificantly underestimated by such models, similar to the trend seen for CO in Chapter 2. Varying freeze-out timescales in the regions of the en- velopes corresponding to

The left column gives the temperature and density as functions of radius (black solid and grey dashed lines, respectively) for three archetypical low-mass pre- and protostellar

The identical fits to the line intensities and continuum observations and success of both collapse and power-law density models illustrates the low age inferred for IRAS2: the

The detailed modeling of the continuum emission performed in §7.3 reveals that there is compact emission in both IRAS 16293–2422 and L1448–C that can- not be explained by the

The dip seen in the single-dish CS spectra at the rest velocity of the cloud is a result of self-absorption, while for the interferometry observations it is caused by the

The derived abundances do not depend on the velocity field as long as integrated intensities of optically thin lines are considered (Jørgensen et al. 2004d), but this may not be

Through observations with, e.g., the Spitzer Space Telescope and infrared cameras on 8 m class telescopes, the inner radius of the envelopes, as well as the spectral energy

Het gas rondom lage massa protosterren kan bijvoorbeeld door waarnemingen van moleculaire lijnen in het millime- ter golflengtegebied bestudeerd worden en de stofdeeltjes kunnen