Highly Depleted Ethane and Slightly Depleted Methanol in Comet 21P/Giacobini-Zinner: Application of Empirical g-factors for CH3OH near 50 K

Details Highly Depleted Ethane and Slightly Depleted Methanol in Comet 21P/Giacobini-Zinner: Application of Empirical g-factors for CH3OH near 50 K Highly Depleted Ethane and Slightly Depleted Methanol in Comet 21P/Giacobini-Zinner: Application of Empirical g-factors for CH3OH near 50 K

Oct 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010dps....42.0307d&link_type=abstract

American Astronomical Society, DPS meeting #42, #3.07; Bulletin of the American Astronomical Society, Vol. 42, p.946

Astronomy and Astrophysics

Astrophysics

Scientific paper

We report high resolution (λ/Δλ 24,000) observations of Comet 21P/Giacobini-Zinner (21P) between 2.85 - 3.54 µm, obtained with NIRSPEC at Keck 2 on UT 2005 June 03 (Rh = 1.12 AU, Δ = 1.45 AU). These simultaneously sampled multiple emissions from the ν7 band of C2H6 and the ν2 and ν3 bands of CH3OH, together with several hot bands of H2O, permitting a direct measure of parent volatile abundances in 21P. Our spectra reveal highly depleted C2H6 (0.13-0.14 percent relative to H2O) and CH3OH/C2H6 10, consistent with previously published abundances from observations in the IR [1,2] and millimeter/sub-mm (reporting CH3OH/H2O [3]) during its previous apparition in 1998.
We observed similarly high CH3OH/C2H6, and also similar rotational temperature to that measured for 21P, in Comet 8P/Tuttle [4,5]. We used our (higher signal-to-noise) NIRSPEC observations of 8P to produce effective (empirical) CH3OH g-factors for several lines in the ν2 band. These will be presented together with interpretation of our results, including constraints on the spin temperature of water. We acknowledge support from the NASA Planetary Atmospheres, Planetary Astronomy, and Astrobiology Programs and from the NSF Astronomy and Astrophysics Research Grants Program.
References: [1] Weaver et al. 1999 Icarus 142:482; [2] Mumma et al. 2000 ApJ 531:L155; [3] Biver et al. 2002 EMP 90:323; [4] Bonev et al. 2008 ApJ 680:L61; [5] Boehnhardt et al. 2008 ApJ 683:L71

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