Forbidden oxygen lines in Comets C/2006 W3 Christensen and C/2007 Q3 Siding Spring at large heliocentric distance: Implications for the sublimation of volatile ices

McKay, Adam; Chanover, N. J.; Morgenthaler, J. P.; Cochran, A. L.; Harris, Walter M.; Russo, N. Dello

doi:10.1016/j.icarus.2012.04.030

Cited by 35 publications

(33 citation statements)

References 32 publications

(36 reference statements)

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“…Those lines are produced by prompt emission following the photodissociation of various parent molecules (H 2 O, CO 2 , CO, but also O 2 ) into a shortlived excited oxygen atoms (Festou and Feldman 1981;Cessateur et al 2016). The combination of measurements of two forbidden lines O 1 D and O 1 S shows that is possible to even estimate the CO 2 /H 2 O ratio (McKay et al 2012;Decock et al 2013;Cessateur et al 2016). The 6300.304 Å line, which is the brightest of the three forbidden oxygen lines has been successfully used to derive water production rates (e.g., Spinrad 1982;McKay et al 2012).…”

Section: Uv/visible Emission Featuresmentioning

confidence: 99%

“…The combination of measurements of two forbidden lines O 1 D and O 1 S shows that is possible to even estimate the CO 2 /H 2 O ratio (McKay et al 2012;Decock et al 2013;Cessateur et al 2016). The 6300.304 Å line, which is the brightest of the three forbidden oxygen lines has been successfully used to derive water production rates (e.g., Spinrad 1982;McKay et al 2012). Observation of the forbidden oxygen lines require highresolution spectroscopy and a sufficient Doppler shift of the comet emission lines to be distinguished from telluric oxygen lines.…”

Section: Uv/visible Emission Featuresmentioning

confidence: 99%

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The Main Belt Comets and ice in the Solar System

Snodgrass

Agarwal

Combi

et al. 2017

Astron Astrophys Rev

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We review the evidence for buried ice in the asteroid belt; specifically the questions around the so-called Main Belt Comets (MBCs). We summarise the evidence for water throughout the Solar System, and describe the various methods for detecting it, including remote sensing from ultraviolet to radio wavelengths. We review progress in the first decade of study of MBCs, including observations, modelling of ice survival, and discussion on their origins. We then look at which methods will likely be most effective for further progress, including the key challenge of direct detection of (escaping) water in these bodies.

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Section: Uv/visible Emission Featuresmentioning

confidence: 99%

Section: Uv/visible Emission Featuresmentioning

confidence: 99%

The Main Belt Comets and ice in the Solar System

Snodgrass

Agarwal

Combi

et al. 2017

Astron Astrophys Rev

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“…Examples of the types of studies performed are 12 C/ 13 C (Danks et al 1974;Kleine et al 1995), 14 N/ 15 N (Arpigny et al 2003;Manfroid et al 2005Manfroid et al , 2009 and O ( 1 S/ 1 D) (Cochran and Cochran 2001;Festou and Feldman 1981;Capria et al 2005Capria et al , 2008McKay et al 2012Decock et al 2013Decock et al , 2015.…”

Section: Optical Observationsmentioning

confidence: 99%

“…McKay et al (2012 and Decock et al (2013Decock et al ( , 2015 have used discussions of branching ratios for the processes to produce [O I] (e.g. Festou and Feldman 1981) and have developed procedures and empirical release rates to use observations of the forbidden oxygen lines in the optical to infer the abundance of CO or CO 2 .…”

Section: Ir Observationsmentioning

confidence: 99%

The Composition of Comets

Cochran¹,

et al. 2015

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This paper is the result of the International Cometary Workshop, held in Toulouse, France in April 2014, where the participants came together to assess our knowledge of comets prior to the ESA Rosetta Mission. In this paper, we look at the composition of the gas and dust from the comae of comets. With the gas, we cover the various taxonomic studies that have broken comets into groups and compare what is seen at all wavelengths. We also discuss what has been learned from mass spectrometers during flybys. A few caveats for our interpretation are discussed. With dust, much of our information comes from flybys. They include {\it in situ} analyses as well as samples returned to Earth for laboratory measurements. Remote sensing IR observations and polarimetry are also discussed. For both gas and dust, we discuss what instruments the Rosetta spacecraft and Philae lander will bring to bear to improve our understanding of comet 67P/Churyumov-Gerasimenko as "ground-truth" for our previous comprehensive studies. Finally, we summarize some of the initial Rosetta Mission findings.Comment: To appear in Space Science Review

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“…The direct de-excitation of O( 1 S) yields a 2972 Å emission line, which has been observed in the cometary spectrum only once (Festou & Feldman 1981). Since there are other oxygen-bearing species, such as CO 2 and CO, which can also produce these metastable states via dissociative excitation reactions, the observed green to red-doublet emission intensity ratio (hereafter referred as the G/R ratio) has been used to confirm the parent source of these emission lines (Cochran 1984(Cochran , 2008Morrison et al 1997;Cochran & Cochran 2001;Zhang et al 2001;Capria et al 2005Capria et al , 2008Capria et al , 2010Furusho et al 2006;McKay et al 2012McKay et al , 2013McKay et al , 2015Decock et al 2013). Based on O( 1 S) and O( 1 D) photorates calculated by Festou & Feldman (1981), the observed high G/R ratio values (>0.1) were ascribed to large CO 2 and CO volume mixing ratios in the coma (Furusho et al 2006;Capria et al 2010;McKay et al 2012;Decock et al 2013).…”

Section: Introductionmentioning

confidence: 99%

Prediction of Forbidden Ultraviolet and Visible Emissions in Comet 67p/Churyumov–gerasimenko

Raghuram

Bhardwaj

Galand

2016

ApJ

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Remote observation of spectroscopic emissions is a potential tool for the identification and quantification of various species in comets. The CO Cameron band (to trace CO 2 ) and atomic oxygen emissions (to trace H 2 O and/ or CO 2 , CO) have been used to probe neutral composition in the cometary coma. Using a coupled-chemistryemission model, various excitation processes controlling the CO Cameron band and different atomic oxygen and atomic carbon emissions have been modeled in comet 67P/Churyumov-Gerasimenko at 1.29 AU (perihelion) and at 3 AU heliocentric distances, which is being explored by ESAʼs Rosetta mission. The intensities of the CO Cameron band, atomic oxygen, and atomic carbon emission lines as a function of projected distance are calculated for different CO and CO 2 volume mixing ratios relative to water. Contributions of different excitation processes controlling these emissions are quantified. We assess how CO 2 and/or CO volume mixing ratios with respect to H 2 O can be derived based on the observed intensities of the CO Cameron band, atomic oxygen, and atomic carbon emission lines. The results presented in this work serve as baseline calculations to understand the behavior of low out-gassing cometary coma and compare them with the higher gas production rate cases (e.g., comet Halley). Quantitative analysis of different excitation processes governing the spectroscopic emissions is essential to study the chemistry of inner coma and to derive neutral gas composition.

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Forbidden oxygen lines in Comets C/2006 W3 Christensen and C/2007 Q3 Siding Spring at large heliocentric distance: Implications for the sublimation of volatile ices

Cited by 35 publications

References 32 publications

The Main Belt Comets and ice in the Solar System

The Main Belt Comets and ice in the Solar System

The Composition of Comets

Prediction of Forbidden Ultraviolet and Visible Emissions in Comet 67p/Churyumov–gerasimenko

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