A study of carbon-monoxide and neutral carbon in the s106 molecular core

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. (The full text of this publication is not currently available from this repository. You may be able to access a copy if URLs are provided)

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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.

Item Type: Article
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: 11 Jul 2014 09:05
Resource URI: https://kar.kent.ac.uk/id/eprint/19354 (The current URI for this page, for reference purposes)
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