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Title:
Radio OH observations of 9P/Tempel 1 before and after Deep Impact
Authors:
Howell, Ellen S.; Lovell, Amy J.; Butler, Bryan; Schloerb, F. Peter
Affiliation:
AA(NAIC/Arecibo Observatory, HC3 Box 53995, Arecibo 00612, Puerto Rico), AB(Agnes Scott College, 141 E. College Ave., Decatur, GA 30030, USA), AC(National Radio Astronomy Observatory, 1003 Lopezville Rd., Socorro, NM 87801-0387, USA), AD(Five College Radio Astronomy Observatory, University of Massachusetts Amherst, Amherst, MA 01003, USA)
Publication:
Icarus, Volume 187, Issue 1, p. 228-239. (Icarus Homepage)
Publication Date:
03/2007
Origin:
ELSEVIER
DOI:
10.1016/j.icarus.2006.10.005
Bibliographic Code:
2007Icar..187..228H

Abstract

We observed 18-cm OH emission in Comet 9P/Tempel 1 before and after Deep Impact. Observations using the Arecibo Observatory 305 m telescope took place between 8 April and 9 June, 2005, followed by post-impact observations using the National Radio Astronomy Observatory 100 m Green Bank Telescope 4 12 July, 2005. The resulting spectra were analyzed with a kinematic Monte Carlo model which allows estimation of the OH production rate, neutral gas outflow velocity, and distribution of the out-gassing from the nucleus. We detected typically 24% variability from the overall OH production rate trend in the two months leading up to the impact, and no dramatic increase in OH production in the days post-impact. Generally, the coma is well-described, within uncertainties, by a symmetric model with OH production rates from 1.6 to 7.4×10 mols, and mean water outflow velocity of 0.75±0.03 kms. At these low production rates, collisional quenching is expected to occur only within 20,000 km of the nucleus. However, our best-fit average quenching radius is 64,200 ± 22,000 km in April and May.

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