Little, L.T and Kelly, M.L and Habing, R.J. and Millar, T.J. (1995) A study of carbon-monoxide and neutral carbon in the s106 molecular core. Monthly Notices of the Royal Astronomical Society, 277 (1). pp. 307-318. ISSN 0035-8711.
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Maps are presented of J=2-1 and J=3-2 (CO)-O-18 emission from the molecular environment of the bipolar nebula S106, together with complementary observations of the P-3(1)-P-3(0), C I emission. Line splitting observed extensively over the E molecular cloud suggests that it is best explained as the expanding remnant of a thick toroid surrounding the optical lobes. The poor correlation between the observed molecular line emission and dust continuum emission in the E cloud is probably due to a large temperature gradient. Strong C I emission from the protostellar candidate S106 FIR suggests the nearby presence of a powerful source of far-UV radiation, whose energy supply is unlikely to arise from gravitational contraction of a protostar. It is probable that this source is the star S106 LR, which also heats S106 FIR. There is evidence, in both C I and (CO)-O-18, for a predominantly blueshifted outflow from S106 IR, best interpreted as a stellar wind-driven shock into the toroidal remnant. (CO)-O-18 and (CO)-C-13 appear to be depleted, relative to canonical values for their abundances, in S106 FIR, despite its high optical extinction, which should discourage selective photodissociation. Elsewhere in the cloud the C I line profiles show a resemblance to those of (CO)-O-18, with intensity equivalent to a few photodissociation regions (PDRs) along the line of sight.
|Uncontrolled keywords:||line, profiles; ism, abundances; ism, clouds; ism, individual, s106; ism, molecules; radio lines, ism|
|Subjects:||Q Science > QB Astronomy
Q Science > QC Physics
|Divisions:||Faculties > Science Technology and Medical Studies > School of Physical Sciences|
|Depositing User:||O.O. Odanye|
|Date Deposited:||04 Jun 2009 14:07|
|Last Modified:||04 Jun 2009 14:07|
|Resource URI:||http://kar.kent.ac.uk/id/eprint/19354 (The current URI for this page, for reference purposes)|
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