2-D Radiative Transfer in Protostellar Envelopes: II. An Evolutionary Sequence

Details 2-D Radiative Transfer in Protostellar Envelopes: II. An Evolutionary Sequence 2-D Radiative Transfer in Protostellar Envelopes: II. An Evolutionary Sequence

2003-08-30

arxiv.org/abs/astro-ph/0309007v1

Astrophys.J.598:1079-1099,2003

Astronomy and Astrophysics

Astrophysics

A version with high-resolution images is available at http://www.astro.wisc.edu/glimpse/glimpsepubs.html

Scientific paper

10.1086/379068

We present model spectral energy distributions, colors, polarization, and images for an evolutionary sequence of a low-mass protostar from the early collapse stage (Class 0) to the remnant disk stage (Class III). We find a substantial overlap in colors and SEDs between protostars embedded in envelopes (Class 0-I) and T Tauri disks (Class II), especially at mid-IR wavelengths. Edge-on Class I-II sources show double-peaked spectral energy distributions, with a short-wavelength hump due to scattered light and the long-wavelength hump due to thermal emission. These are the bluest sources in mid-IR color-color diagrams. Since Class 0 and I sources are diffuse, the size of the aperture over which fluxes are integrated has a substantial effect on the computed colors, with larger aperture results showing significantly bluer colors. This causes overlap in color-color diagrams between all evolutionary states, especially in the mid-IR. However the near-IR polarization of the Class 0 sources is much higher than the Class I-II sources, providing a means to separate these evolutionary states. We varied the grain properties in the circumstellar envelope, allowing for larger grains in the disk midplane and smaller in the envelope. We find that grain growth in disks of Class I sources can be detected at wavelengths greater than 100 $\mu$m. Our image calculations predict that the diffuse emission from edge-on Class I and II sources should be detectable in the mid-IR with the Space Infrared Telescope Facility (SIRTF) in nearby star forming regions (out to several hundred parsecs).

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