Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006dps....38.0304s&link_type=abstract
American Astronomical Society, DPS meeting #38, #03.04; Bulletin of the American Astronomical Society, Vol. 38, p.485
Astronomy and Astrophysics
Astronomy
9
Scientific paper
We present analyses and results from multi-apparition narrowband photometry of Comet 73P/Schwassmann-Wachmann 3. Observations were obtained on 7 nights during the comet's current apparition from 2006 February 25 to May 18 (r = 1.65-0.99 AU) using Lowell Observatory's 42-inch (1.1-m) Hall telescope. Due to the comet's very close passage by the Earth and occasional outbursts, a total of 4 components were successfully measured, including the apparent primary body (C) and 3 fragments (B, G, and R), thus permitting us to probe the composition of the interior of Schwassmann-Wachmann 3's nucleus. Abundances of carbon-chain molecules yield a classification of strongly "depleted” in the A'Hearn et al. (1995, Icarus 118, 223) database, with the Q(C2)-to-Q(CN) ratio depleted by factors of between 7 and 8 for components C, B, and G, and a comparable upper limit for component R. Measured from Perth Observatory, S-W 3 also exhibited strong depletion in 1995, about 1-2 months after its original outburst and fragmentation. In 1990, prior to any fragmentation, Fink and Hicks (1996, Ap.J. 459, 729) identified Schwassmann-Wachmann 3 as being strongly depleted, with an upper limit on Q(C2) corresponding to a C2 depletion of a factor of 6.4 or greater. With the material released from the interior of S-W 3 yielding comparable depletions of carbon-chain molecules as with the original surface of the nucleus, we can conclusively state that carbon-chain depletion is not caused by evolution of the surface, and so must instead reflect the primordial composition at the time and location that the comet accreted.
A comparison of production rates for CN implies that component C in 2006 had returned to nearly the same rate of gas vaporization as it had at similar heliocentric distances in 1990. These and other results will be presented. This research is supported by NASA's Planetary Astronomy Program.
Bair Allison N.
Birch Peter V.
Schleicher David G.
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