Phillips, J. P.; White, Glenn J.; Ade, P. A. R.; Cunningham, C. T.; Richardson, K. J.; Robson, E. I. and Watt, Graeme D.
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We present CO J=3→2 molecular line spectra, and submillimetre photometry at wavelengths λλ377 μm, 811 μm, and 1136 μm for the sources L1551 and IRC+10216. Detailed analysis of the L1551 spectra indicates the presence of strong velocity gradients in the CO emission zones, implying low optical depths and relatively high densities. The central source IRS 5 displays an infrared excess wihich cannot be explained in terms of a single temperature continuum. The emission zone is probably compact with respect to the instrumental beam size at the wavelength of peak emission (λ~50 μm), and may represent an accretion disc responsible for collimation of the high velocity gas. The far-infrared continuum of IRC+10216 has been synthesised by assuming a distribution of optically thin grains whose emissivity varies as εα λ-1, and the CO J=3→2 spectrum for this source supports earlier J=2→1 observations, implying a variable mass-loss rate
|Item Type:||Journal Article|
|Copyright Holders:||1982 European Southern Observatory|
|Keywords:||carbon monoxide; electron transitions; molecular spectra; stellar evolution; stellar mass ejection; variable stars; interstellar gas; late stars; line spectra; stellar winds; velocity distribution|
|Academic Unit/Department:||Science > Physical Sciences
|Interdisciplinary Research Centre:||Centre for Earth, Planetary, Space and Astronomical Research (CEPSAR)|
|Depositing User:||G. J. White|
|Date Deposited:||07 Jun 2012 08:40|
|Last Modified:||24 Feb 2016 02:30|
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