Large Aperture [O I] 6300 Å Observations Of Comet Hyakutake: Implications For The Photochemistry Of OH And [O I] Production In Comet Hale-Bopp

Details Large Aperture [O I] 6300 Å Observations Of Comet Hyakutake: Implications For The Photochemistry Of OH And [O I] Production In Comet Hale-Bopp Large Aperture [O I] 6300 Å Observations Of Comet Hyakutake: Implications For The Photochemistry Of OH And [O I] Production In Comet Hale-Bopp

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006dps....38.2007m&link_type=abstract

American Astronomical Society, DPS meeting #38, #20.07; Bulletin of the American Astronomical Society, Vol. 38, p.517

Astronomy and Astrophysics

Astronomy

Scientific paper

In previous work (Morgenthaler et al. 2001, Glinski et al. 2004), we proposed a revision to the standard OH photochemistry of van Dishoeck & Dalgarno (1984) in order to explain the anomalously bright [O I] 6300 Å emission observed by several instruments in comet C/1995 O1 (Hale-Bopp). In order to test the validity of revisions to the OH photochemistry, we present wide-field Fabry-Pérot [O I] 6300 Å observations of comet C/1996 B2 (Hyakutake) recorded with the Wisconsin H-alpha Mapper (WHAM), one of the instruments that detected the [O I] excess in comet Hale-Bopp. Hyakutake was shown to have highly variable Q(H2O) values (Schleicher et al. 2002, Combi et al. 2005), so we used a time-varying Haser model with Q(H2O) values from Combi et al. to fit radial profiles formed from the WHAM image-mode data. Only the standard OH photochemistry resulted in satisfactory fits: modified OH photochemistry results in model profiles that are too flat. Radial profiles of Fabry-Pérot [O I] images of comet 1989 c1 (Austin), were well fit by a Haser model with standard OH photochemistry (Schultz et al. 1993). Comet 1P/Halley [O I] images, recorded with a Fabry-Pérot similar to that used in the Austin campaign (Magee-Sauer et al. 1988), however, were not well fit by static or variable Haser models using standard or modified photochemistry: the models are too flat in all cases. The bulk of the evidence suggests that the OH photochemical rates of van Dishoeck & Dalgarno (1984) are, on the whole, correct, and that the bright [O I] emission observed in Hale-Bopp, particularly at cometocentric distances beyond 3 x 104 km, was unique to that comet, or possibly any comet with such a large production rate.
This work has been supported by NASA and NSF.

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