The gas production rate and coma structure of comet C/1995 O1 (Hale-Bopp)

Jeffrey P. Morgenthaler, Walter M Harris, Frederick L. Roesler, Frank Scherb, Christopher M. Anderson, Nathaniel E. Doane, Ronald J. Oliversen

Research output: Contribution to journalArticle

3 Citations (Scopus)

Abstract

The University of Wisconsin-Madison and NASA-Goddard conducted a comprehensive multi-wavelength observing campaign of coma emissions from comet Hale-Bopp, including OH 3080 Å, [O I] 6300 Å, H2O+ 6158 Å, H Balmer-α 6563 Å, NH2 6330 Å, [C I] 9850 Å CN 3879 Å, C2 5141 Å, C3 4062 Å, C I 1657 Å, and the UV and optical continua. In this work, we concentrate on the results of the H2O daughter studies. Our wide-field OH 3080 Å measured flux agrees with other, similar observations and the expected value calculated from published water production rates using standard H2O and OH photochemistry. However, the total [O I] 6300 Å flux determined spectroscopically over a similar field-of-view was a factor of 3 - 4 higher than expected. Narrow-band [O I] images show this excess came from beyond the H2O scale length, suggesting either a previously unknown source of [O I] or an error in the standard OH + v → O(1D) + H branching ratio. The Hale-Bopp OH and [O I] distributions, both of which were imaged to cometocentric distances > 1 × 106 km. were more spatially extended than those of comet Halley (after correcting for brightness differences), suggesting a higher bulk outflow velocity. Evidence of the driving mechanism for this outflow is found in the Hα line profile, which was narrower than in comet Halley (though likely because of opacity effects, not as narrow as predicted by Monte-Carlo models). This is consistent with greater collisional coupling between the suprathermal H photodissociation products and Hale-Bopp's dense coma. Presumably because of mass loading of the solar wind by ions and ions by the neutrals, the measured acceleration of H2O+ down the ion tail was much smaller than in comet Halley. Tailward extensions in the azimuthal distributions of OH 3080 Å, [O I], and [C I], as well as a Doppler asymmetry in the [O I] line profile, suggest ion-neutral coupling. While the tailward extension in the OH can be explained by increased neutral acceleration, the [O I] 6300 Å and [C I] 9850 Å emissions show 13% and > 200% excesses in this direction (respectively), suggesting a non-negligible contribution from dissociative recombination of CO+ and/or electron collisional excitation. Thus, models including the effects of photo- and collisional chemistry are necessary for the full interpretation of these data.

Original languageEnglish (US)
Pages (from-to)77-87
Number of pages11
JournalEarth, Moon and Planets
Volume90
Issue number1-4
DOIs
StatePublished - Mar 2002
Externally publishedYes

Fingerprint

Hale-Bopp
coma
comets
Halley's comet
gas production
comet
ion
gases
ions
outflow
Hale-Bopp comet
H lines
photochemistry
profiles
field of view
opacity
photochemical reactions
photodissociation
recombination
solar wind

Keywords

  • C/1995 O1 (hale-bopp)
  • Carbon monoxide
  • Comets
  • Dissociative recombination
  • Electron collisional excitation
  • Hydrogen Balmer-α coma
  • Hydroxyl radical photodissociation
  • Metastable oxygen coma
  • Water photochemistry
  • Water production rate

ASJC Scopus subject areas

  • Earth and Planetary Sciences (miscellaneous)
  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Morgenthaler, J. P., Harris, W. M., Roesler, F. L., Scherb, F., Anderson, C. M., Doane, N. E., & Oliversen, R. J. (2002). The gas production rate and coma structure of comet C/1995 O1 (Hale-Bopp). Earth, Moon and Planets, 90(1-4), 77-87. https://doi.org/10.1023/A:1021564301815

The gas production rate and coma structure of comet C/1995 O1 (Hale-Bopp). / Morgenthaler, Jeffrey P.; Harris, Walter M; Roesler, Frederick L.; Scherb, Frank; Anderson, Christopher M.; Doane, Nathaniel E.; Oliversen, Ronald J.

In: Earth, Moon and Planets, Vol. 90, No. 1-4, 03.2002, p. 77-87.

Research output: Contribution to journalArticle

Morgenthaler, JP, Harris, WM, Roesler, FL, Scherb, F, Anderson, CM, Doane, NE & Oliversen, RJ 2002, 'The gas production rate and coma structure of comet C/1995 O1 (Hale-Bopp)', Earth, Moon and Planets, vol. 90, no. 1-4, pp. 77-87. https://doi.org/10.1023/A:1021564301815
Morgenthaler, Jeffrey P. ; Harris, Walter M ; Roesler, Frederick L. ; Scherb, Frank ; Anderson, Christopher M. ; Doane, Nathaniel E. ; Oliversen, Ronald J. / The gas production rate and coma structure of comet C/1995 O1 (Hale-Bopp). In: Earth, Moon and Planets. 2002 ; Vol. 90, No. 1-4. pp. 77-87.
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abstract = "The University of Wisconsin-Madison and NASA-Goddard conducted a comprehensive multi-wavelength observing campaign of coma emissions from comet Hale-Bopp, including OH 3080 {\AA}, [O I] 6300 {\AA}, H2O+ 6158 {\AA}, H Balmer-α 6563 {\AA}, NH2 6330 {\AA}, [C I] 9850 {\AA} CN 3879 {\AA}, C2 5141 {\AA}, C3 4062 {\AA}, C I 1657 {\AA}, and the UV and optical continua. In this work, we concentrate on the results of the H2O daughter studies. Our wide-field OH 3080 {\AA} measured flux agrees with other, similar observations and the expected value calculated from published water production rates using standard H2O and OH photochemistry. However, the total [O I] 6300 {\AA} flux determined spectroscopically over a similar field-of-view was a factor of 3 - 4 higher than expected. Narrow-band [O I] images show this excess came from beyond the H2O scale length, suggesting either a previously unknown source of [O I] or an error in the standard OH + v → O(1D) + H branching ratio. The Hale-Bopp OH and [O I] distributions, both of which were imaged to cometocentric distances > 1 × 106 km. were more spatially extended than those of comet Halley (after correcting for brightness differences), suggesting a higher bulk outflow velocity. Evidence of the driving mechanism for this outflow is found in the Hα line profile, which was narrower than in comet Halley (though likely because of opacity effects, not as narrow as predicted by Monte-Carlo models). This is consistent with greater collisional coupling between the suprathermal H photodissociation products and Hale-Bopp's dense coma. Presumably because of mass loading of the solar wind by ions and ions by the neutrals, the measured acceleration of H2O+ down the ion tail was much smaller than in comet Halley. Tailward extensions in the azimuthal distributions of OH 3080 {\AA}, [O I], and [C I], as well as a Doppler asymmetry in the [O I] line profile, suggest ion-neutral coupling. While the tailward extension in the OH can be explained by increased neutral acceleration, the [O I] 6300 {\AA} and [C I] 9850 {\AA} emissions show 13{\%} and > 200{\%} excesses in this direction (respectively), suggesting a non-negligible contribution from dissociative recombination of CO+ and/or electron collisional excitation. Thus, models including the effects of photo- and collisional chemistry are necessary for the full interpretation of these data.",
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AU - Morgenthaler, Jeffrey P.

AU - Harris, Walter M

AU - Roesler, Frederick L.

AU - Scherb, Frank

AU - Anderson, Christopher M.

AU - Doane, Nathaniel E.

AU - Oliversen, Ronald J.

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N2 - The University of Wisconsin-Madison and NASA-Goddard conducted a comprehensive multi-wavelength observing campaign of coma emissions from comet Hale-Bopp, including OH 3080 Å, [O I] 6300 Å, H2O+ 6158 Å, H Balmer-α 6563 Å, NH2 6330 Å, [C I] 9850 Å CN 3879 Å, C2 5141 Å, C3 4062 Å, C I 1657 Å, and the UV and optical continua. In this work, we concentrate on the results of the H2O daughter studies. Our wide-field OH 3080 Å measured flux agrees with other, similar observations and the expected value calculated from published water production rates using standard H2O and OH photochemistry. However, the total [O I] 6300 Å flux determined spectroscopically over a similar field-of-view was a factor of 3 - 4 higher than expected. Narrow-band [O I] images show this excess came from beyond the H2O scale length, suggesting either a previously unknown source of [O I] or an error in the standard OH + v → O(1D) + H branching ratio. The Hale-Bopp OH and [O I] distributions, both of which were imaged to cometocentric distances > 1 × 106 km. were more spatially extended than those of comet Halley (after correcting for brightness differences), suggesting a higher bulk outflow velocity. Evidence of the driving mechanism for this outflow is found in the Hα line profile, which was narrower than in comet Halley (though likely because of opacity effects, not as narrow as predicted by Monte-Carlo models). This is consistent with greater collisional coupling between the suprathermal H photodissociation products and Hale-Bopp's dense coma. Presumably because of mass loading of the solar wind by ions and ions by the neutrals, the measured acceleration of H2O+ down the ion tail was much smaller than in comet Halley. Tailward extensions in the azimuthal distributions of OH 3080 Å, [O I], and [C I], as well as a Doppler asymmetry in the [O I] line profile, suggest ion-neutral coupling. While the tailward extension in the OH can be explained by increased neutral acceleration, the [O I] 6300 Å and [C I] 9850 Å emissions show 13% and > 200% excesses in this direction (respectively), suggesting a non-negligible contribution from dissociative recombination of CO+ and/or electron collisional excitation. Thus, models including the effects of photo- and collisional chemistry are necessary for the full interpretation of these data.

AB - The University of Wisconsin-Madison and NASA-Goddard conducted a comprehensive multi-wavelength observing campaign of coma emissions from comet Hale-Bopp, including OH 3080 Å, [O I] 6300 Å, H2O+ 6158 Å, H Balmer-α 6563 Å, NH2 6330 Å, [C I] 9850 Å CN 3879 Å, C2 5141 Å, C3 4062 Å, C I 1657 Å, and the UV and optical continua. In this work, we concentrate on the results of the H2O daughter studies. Our wide-field OH 3080 Å measured flux agrees with other, similar observations and the expected value calculated from published water production rates using standard H2O and OH photochemistry. However, the total [O I] 6300 Å flux determined spectroscopically over a similar field-of-view was a factor of 3 - 4 higher than expected. Narrow-band [O I] images show this excess came from beyond the H2O scale length, suggesting either a previously unknown source of [O I] or an error in the standard OH + v → O(1D) + H branching ratio. The Hale-Bopp OH and [O I] distributions, both of which were imaged to cometocentric distances > 1 × 106 km. were more spatially extended than those of comet Halley (after correcting for brightness differences), suggesting a higher bulk outflow velocity. Evidence of the driving mechanism for this outflow is found in the Hα line profile, which was narrower than in comet Halley (though likely because of opacity effects, not as narrow as predicted by Monte-Carlo models). This is consistent with greater collisional coupling between the suprathermal H photodissociation products and Hale-Bopp's dense coma. Presumably because of mass loading of the solar wind by ions and ions by the neutrals, the measured acceleration of H2O+ down the ion tail was much smaller than in comet Halley. Tailward extensions in the azimuthal distributions of OH 3080 Å, [O I], and [C I], as well as a Doppler asymmetry in the [O I] line profile, suggest ion-neutral coupling. While the tailward extension in the OH can be explained by increased neutral acceleration, the [O I] 6300 Å and [C I] 9850 Å emissions show 13% and > 200% excesses in this direction (respectively), suggesting a non-negligible contribution from dissociative recombination of CO+ and/or electron collisional excitation. Thus, models including the effects of photo- and collisional chemistry are necessary for the full interpretation of these data.

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KW - Electron collisional excitation

KW - Hydrogen Balmer-α coma

KW - Hydroxyl radical photodissociation

KW - Metastable oxygen coma

KW - Water photochemistry

KW - Water production rate

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