Activity of Comet C/2006 W3 Christensen

Kossacki, Konrad J.; Szutowicz, S.

doi:10.1016/j.icarus.2014.12.019

Cited by 4 publications

(2 citation statements)

References 24 publications

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“…When normalized to HCN, abundance ratios of the species observed with the IRAM telescope was HCN:CO:CH 3 OH:H 2 S:CS = 1:240:9:6:0.3 indicating that W3 is CO-rich. Kossacki & Szutowicz (2015), using available observations, carried out theoretical modeling and found that the nucleus of the comet should be very porous, composed of moderately fine grains that were about 10 µm in diameter with a tensile strength of about 10 kPa, as was estimated for comet 9P/Tempel 1.…”

Section: Introductionmentioning

confidence: 99%

Optical spectrophotometric monitoring of comet C/2006 W3 (Christensen) before perihelion

Корсун

Kulyk

Ivanova

et al. 2016

A&A

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Context. Long period distant comet C/2006 W3 (Christensen) was discovered in 2006 and passed perihelion at 3.13 au in July 2009. It was a target for the Herschel Space Observatory, Spitzer Space Telescope, and ground-based radio telescopes. We enlarge the observational database with optical spectrophotometric ground base data. Aims. We performed optical monitoring of cometary activity and searched for possible emission lines in the C/2006 W3 (Christensen) spectrum in a wide range of heliocentric distances. Methods. We carried out pre-perihelion observations of the comet at heliocentric distances from 8.49 to 3.13 au with the 2 m and 6 m telescopes, both in imaging and spectroscopic modes, during the period 2006 to 2009. Results. No emissions were detected in the spectra at heliocentric distances of 8.49 and 6.25 au. Rich molecular emission spectra were obtained, when the comet was at a distance of 3.74 au from the Sun. The CN, C 3 , C 2 , CH, NH 2 , CO + , and, probably, CH + emissions were assigned in the 3800-6800 Å spectral range. Gas production rates or corresponding upper limits in the emissionless case were calculated using a Haser model. We derived the gas production rates of 1.03 × 10 26 mol s −1 for CN, 4.12 × 10 24 mol s −1 for C 3 , 6.54 × 10 25 mol s −1 for C 2 , and 3.12 × 10 25 mol s −1 for NH 2 , which is matched with the CN:C 3 :C 2 :NH 2 = 1.0:0.04:0.63:0.30 gas production ratios at a heliocentric distance of 3.74 au. The CO + production rate of the comet, which was equal to 2 × 10 24 mol s −1 , was also obtained. We quantified the evolution of the comet activity in a wide range of heliocentric distances with the A f ρ technique. Heliocentric dependence of the A f ρ parameters indicates that steep growth of the comet activity occurred around 3.96 au, almost simultaneously with the appearance of molecular emissions in the comet spectrum. The dust production rate was estimated from the A f ρ reaching a maximal value of 380 kg s −1 at a distance of 3.13 au before perihelion passage.

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Section: Introductionmentioning

confidence: 99%

Optical spectrophotometric monitoring of comet C/2006 W3 (Christensen) before perihelion

Корсун

Kulyk

Ivanova

et al. 2016

A&A

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“…It should be noted that the rate of sublimation

Ż

and the cometary gas velocity v g that occur in Equation 2 are functions of the temperature T s of the surface of the cometary nucleus. This important parameter has been calculated on the basis of the well‐known energy balance equation for the surface of the cometary nucleus (for more details, see, e.g., Capria et al ; Gronkowski, ; Keller, ; Kossacki & Szutowicz S., ; Kossacki et al ; Marboeuf et al ). We emphasize that in our discussion, we assume the tensile strength of the cometary nucleus as 10 kPa according to Reach et al ().…”

Section: Emission Of Grains From the Surface Of An Ellipsoidal Cometamentioning

confidence: 99%

Ejection of large particles from cometary nuclei in the shape of prolate ellipsoids

Gronkowski

Wesołowski

2017

Astron Nachr

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The ejection of cometary grains from comets is examined. It is assumed that cometary grains are chunks of ice-dust material. We focus on cometary nuclei in the shape of prolate ellipsoids. Two mechanisms are considered. The first one is the drag acting on the motionless grains lying on the surface of a comet's nucleus. It is a consequence of the cometary ice's gentle sublimation. The second one is related to the cometary jet-like phenomenon. This mechanism is associated with the rapid flow of gas streams into space from subsurface cavities in a comet's nucleus through narrow gaps and channels. The different elongations of ellipsoidal nuclei are examined. The formula for the maximum radius of grain that can be lifted up from the comet's nucleus is derived. The obtained algorithm takes into account the different cometo-centric latitudes of places from which the cometary grains are ejected. We show that for a fixed mass of nucleus the maximum size of grains is an increasing function of nuclear flattening. Numerical simulation is carried out for a large range of assumed cometary parameters. The obtained results are in good agreement with the observations of the Comet 103P/Hartley carried out by the Deep Impact spacecraft.

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Sintering and sublimation of micrometre-sized water-ice particles: the formation of surface crusts on icy Solar System bodies

Gundlach

Ratte

Blum

et al. 2018

Monthly Notices of the Royal Astronomical Society

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Activity of Comet C/2006 W3 Christensen

Cited by 4 publications

References 24 publications

Optical spectrophotometric monitoring of comet C/2006 W3 (Christensen) before perihelion

Optical spectrophotometric monitoring of comet C/2006 W3 (Christensen) before perihelion

Ejection of large particles from cometary nuclei in the shape of prolate ellipsoids

Sintering and sublimation of micrometre-sized water-ice particles: the formation of surface crusts on icy Solar System bodies

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