Physical conditions for dust grain alignment in Class 0 protostellar cores - II. The role of the radiation field in models that align and disrupt dust grains

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Table 1

Radiative transfer calculation details.

	Set I	Set II	Set III	Set VI	Set V	Set VI
f_high−J	1.0	0.0, 0.25, 0.5, 0.75, 1.0	1.0	0.25	1.0	0.2
Luminosity (L_⊙)	20	20	1, 5, 20, 50, 100	20	1, 5, 20, 50, 100	1, 5, 20, 50, 100
a_max (µm)	0.5, 2, 10, 30, 50	10	10	0.5, 2, 10, 30, 50	2	10

Notes. The values of the parameters we vary in the POLARIS radiative transfer calculations, i.e., fraction of aligned grains at the high-J attractor point f_high−J, luminosity of the central object, and maximum dust grain size a_max (µm). Each set gathers five radiative transfer runs where only one parameter varies. Each radiative transfer run produces synthetic observations at 0.87, 1.3, and 3 mm, and assumes that the RAT mechanism is responsible for aligning the dust grains with respect to the magnetic field.

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