Large Aperture [O I] 6300 Å Observations of Comet Hyakutake: Implications for the Photochemistry of...
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Transcript of Large Aperture [O I] 6300 Å Observations of Comet Hyakutake: Implications for the Photochemistry of...
![Page 1: Large Aperture [O I] 6300 Å Observations of Comet Hyakutake: Implications for the Photochemistry of OH and [O I] Production in Comet Hale-Bopp Jeffrey.](https://reader036.fdocuments.net/reader036/viewer/2022062421/56649d1f5503460f949f3a38/html5/thumbnails/1.jpg)
Large Aperture [O I] 6300 Å Observations of Comet
Hyakutake: Implications for the Photochemistry of OH and [O I] Production in Comet Hale-Bopp
Jeffrey P. Morgenthaler, Walter M. Harris (U. Washington), Michael
R. Combi (U. Michigan)
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What is [O I] 6300 Å?
• Emission line from a metastable state of oxygen
• O(1D) difficult to get to with photon excitation
• Product of electron excitation or molecular dissociation
• 110 s lifetime
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Hale-Bopp had “too much” [O I]
• By a factor of 3—4 – Assuming standard H2O and OH
photochemistry
• 4 instruments on 3 telescopes
• Morgenthaler et al., Ap.J., 2001 asked: is photochemistry correct?– OH in particular
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Likely Answer
• Glinski et al. (2004): Hale-Bopp coma dense enough for gas phase chemistry:
O + OH → O2 + H
– Simple coma model with 14 concentric shells– Complex chemical model with 55 reactions
– O2 efficient at producing [O I]
• OH → [O I] branching ratio still needed to be raised to match Hale-Bopp data
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Do [O I] observations of other comets support any change in OH
branching ratios?• Uwe Fink [O I] profiles of many comets
consistent with standard H2O and OH photochemistry– Fink et al. do not cleanly separate airglow and NH2
– Sensitivity of long-slit spectrometers to extended sources is low compared to wide-field Fabry-Pérots
– OH does dominates [O I] >104 km
• Fink sensitivity to [O I] from OH may be too low to address this issue
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Fabry-Pérot Observations
• Solar minimum comets: – Hale-Bopp (Morgenthaler et al. 2001)
• “Too much” [O I]
– Halley (Magee-Sauer et al. 1988, 1990), Hyakutake (this work)
• Highly variable production rates
• Solar max comet: Austin– Good agreement with standard
photochemistry (Schultz et al. 1993)
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Comet Austin [O I] Profile (Schultz et al. 1993)
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Hyakutake (2006 March 23)
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Hyakutake (2006 March 23)
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Hyakutake (2006 March 23)
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Hyakutake (2006 March 23)
• Time-varying Haser model based on Combi et al. (2005) Q(H2O) values
• Glinski et al. (2004) modified OH → [O I] branching ratio (BR3G) not compatible
• Model fits data best with standard photochemistry
• Let’s stick with standard H2O and OH photochemistry
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Halley measured profiles steeper than model
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Halley measured profiles steeper than model
• Hyakutake model based on actual Q(H2O) values (Combi et al. 2005) fits well
• Halley time-varying model based on Q(C2) values (Schleicher et al. 1990)– CN and NH2 profiles match C2 well (Combi et
al. 1993)
• Does H2O have a different inner coma or outgassing or behavior than CN, NH2, and C2?