Long-term optical spectrophotometric monitoring of comet C/1995 O1 (Hale-Bopp)

Rauer, H.; Helbert, J.; Arpigny, C.; Benkhoff, J.; Bockelée‐Morvan, Dominique; Boehnhardt, H.; Colas, François; Crovisier, J.; Hainaut, O.; Jordá, L.; Kueppers, M.; Manfroid, Jean; Thomas, N.

doi:10.1051/0004-6361:20021550

Cited by 62 publications

(70 citation statements)

References 37 publications

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“…Any differences between the shapes of the profiles obtained using a Haser model and the corresponding column density profiles of this work are caused by the different assumptions about the chemical reactions and their rates. The Haser model column densities of Rauer et al (2003) quantitatively differ, i.e. differ in absolute value, from the data presented by H05.…”

Section: Comparison Of the Outputs Of The Two Modelscontrasting

confidence: 71%

“…The reason for the difference in absolute units between the modelled column density profiles, when using the same input parameters, remains unknown. Rauer et al (2003) present Haser production rates for C 3 and C 2 , together with the assumed scale lengths and gas expansion velocities, that were derived from the same data used in H05. The corresponding Haser column density profiles of C 3 and C 2 are also presented in Fig.…”

Section: Comparison Of the Outputs Of The Two Modelsmentioning

confidence: 99%

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The chemistry of C₃and C₂in cometary comae

Weiler

2012

A&A

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Context. It is widely accepted that C 3 and in particular C 2 play an important role in the compositional classification of comets, and the most well-established classification scheme to date is indeed based on the Haser production rates of these two radicals. A link between both C 3 and C 2 and their actual parent molecules would therefore be desirable to allow both a physical and chemical interpretation of the compositional classification of comets. A first detailed study was performed by Helbert and collaborators for comet C/1995 O1 (Hale-Bopp), which suggested a link between these two radicals and the parent species C 2 H 2 , C 2 H 6 , and C 3 H 4 . Aims. We extend previous studies of the formation of C 3 and C 2 to other comets at smaller heliocentric distances. The proposed model for the formation of these two radicals is tested for these comets. Methods. We compare the observed radial column densities of C 3 and C 2 in the comae of the comets C/2001 Q4 (NEAT), C/2002 T7 (LINEAR), and 9P/Tempel 1 with the results of a one-dimensional multi-fluid coma chemistry model. The shape of the modelled radial column density profiles are compared with the observed profiles, and the production rates of the parent species are computed by fitting the observational data with the model. Results. We do not find that C 2 H 6 is a significant parent species of the observed cometary C 2 . Furthermore, electron impact reactions do not play an important role in the formation of C 3 . The model for the formation of C 3 and C 2 derived from comet Hale-Bopp is inconsistent with observations of these radicals in other comets.

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Section: Comparison Of the Outputs Of The Two Modelscontrasting

confidence: 71%

Section: Comparison Of the Outputs Of The Two Modelsmentioning

confidence: 99%

The chemistry of C₃and C₂in cometary comae

Weiler

2012

A&A

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“…The (0-0) band at 3883 Å is one of the most prominent feature of comet optical spectra. It has been detected at up to almost 10 au for comet Hale-Bopp (Rauer et al 2003) and it is usually one of the first gas emissions detected in comets from the ground. The CN radical can also be used as a proxy of water production.…”

Section: Outgassing From Mbcsmentioning

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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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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“…We used a lifetime which agrees with both pre-impact data and data from the impact ejecta cloud. h Rauer et al (2003). i Combi et al (2004).…”

Section: Water Andmentioning

confidence: 99%

Observations of Comet 9P/Tempel 1 around the Deep Impact event by the OSIRIS cameras onboard Rosetta

Keller

Küppers

Fornasier

et al. 2007

Icarus

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The OSIRIS cameras on the Rosetta spacecraft observed Comet 9P/Tempel 1 from 5 days before to 10 days after it was hit by the Deep Impact projectile. The Narrow Angle Camera (NAC) monitored the cometary dust in 5 different filters. The Wide Angle Camera (WAC) observed through filters sensitive to emissions from OH, CN, Na, and OI together with the associated continuum. Before and after the impact the comet showed regular variations in intensity. The period of the brightness changes is consistent with the rotation period of Tempel 1. The overall brightness of Tempel 1 decreased by about 10% during the OSIRIS observations. The analysis of the impact ejecta shows that no new permanent coma structures were created by the impact. Most of the material moved with ~200 ms -1 . Much of it left the comet in the form of icy grains which sublimated and fragmented within the first hour after the impact. The light curve of the comet after the impact and the amount of material leaving the comet (4.5-9 x 10 6 kg of water ice and a presumably larger amount of dust) suggest that the impact ejecta were quickly accelerated by collisions with gas molecules. Therefore, the motion of the bulk of the ejecta cannot be described by ballistic trajectories, and the validity of determinations of the density and tensile strength of the nucleus of Tempel 1 with models using ballistic ejection of particles is uncertain.

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Long-term optical spectrophotometric monitoring of comet C/1995 O1 (Hale-Bopp)

Cited by 62 publications

References 37 publications

The chemistry of C₃and C₂in cometary comae

The chemistry of C₃and C₂in cometary comae

The Main Belt Comets and ice in the Solar System

Observations of Comet 9P/Tempel 1 around the Deep Impact event by the OSIRIS cameras onboard Rosetta

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Long-term optical spectrophotometric monitoring of comet C/1995 O1 (Hale-Bopp)

Cited by 62 publications

References 37 publications

The chemistry of C3and C2in cometary comae

The chemistry of C3and C2in cometary comae

The Main Belt Comets and ice in the Solar System

Observations of Comet 9P/Tempel 1 around the Deep Impact event by the OSIRIS cameras onboard Rosetta

Contact Info

Product

Resources

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The chemistry of C₃and C₂in cometary comae

The chemistry of C₃and C₂in cometary comae