C/2002 VQ94 (LINEAR) and 29P/Schwassmann–Wachmann 1 — CO+ and N+2 rich comets

Корсун, П. П.; Ivanova, Oleksandra; Afanasiev, V. L.

doi:10.1016/j.icarus.2008.08.010

Cited by 49 publications

(70 citation statements)

References 34 publications

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“…This requires several assumptions about the physical characteristics of dust particles in the coma. To calculate the dust production rate, we considered the radii of dust grains falling into the intervals 0.1-100 µm and 0.1-600 µm for data obtained in /2007and 2008/2009, respectively (de Val-Borro et al 2014. The differential size distribution of grains was described by a differential power law of index −3.6 (Bockelée-Morvan et al 2010).…”

Section: Resultsmentioning

confidence: 99%

“…At large heliocentric distances, emissions of CO + have so far only been detected in a few comets: C/1961 R1 (Humason) (Dossin 1966), 29P/Schwassmann-Wachmann 1 (Cochran et al 1980(Cochran et al , 1982(Cochran et al , 1992Cochran & Cochran 1991;Korsun et al 2008), C/1995 O1 Hale-Bopp (Jockers et al 1996), and C/2002 VQ94 (LINEAR) (Korsun et al 2006. Analysis of CO + coma and estimation of column density of CO + at large heliocentric distances are rare in the cometary history and performed only for comet 29P/Schwassmann-Wachmann 1 (Jockers et al 1992) and for comet C/2002 VQ94 (LINEAR) (Ivanova et al 2009;Korsun et al 2008), when the comets were at heliocentric distances of 5.8 and 7.3 au, respectively.…”

Section: Discussionmentioning

confidence: 99%

“…Analysis of CO + coma and estimation of column density of CO + at large heliocentric distances are rare in the cometary history and performed only for comet 29P/Schwassmann-Wachmann 1 (Jockers et al 1992) and for comet C/2002 VQ94 (LINEAR) (Ivanova et al 2009;Korsun et al 2008), when the comets were at heliocentric distances of 5.8 and 7.3 au, respectively. Production rates of NH 2 are often used to derive NH 3 abundance in comets (Tegler & Wyckoff 1989).…”

Section: Discussionmentioning

confidence: 99%

“…2, the contour line equal to 1.99 × 10 −17 erg cm −2 s −1 Å −1 corresponds to a column density of 3 × 10 7 particles per cm 2 at a cometocentric distance of 25 000 km. The column density equal to 6 × 10 10 particles per cm 2 at a distance of approximately 100 000 km from the comet nucleus was derived for comet 29P/SchwassmannWachmann 1, which was at a distance of 5.77 au from the Sun (Jockers et al 1992); and 1.3 × 10 7 particles per cm 2 at a cometocentric distance of 72 000 km were obtained for comet C/2002 VQ94 (LINEAR), which was observed at a heliocentric distance of 7.34 au (Korsun et al 2008).…”

Section: Co + Morphology Of the Cometmentioning

confidence: 97%

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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: Resultsmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Section: Co + Morphology Of the Cometmentioning

confidence: 97%

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

Корсун

Kulyk

Ivanova

et al. 2016

A&A

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“…To eliminate the false details from the images prepared for interpretation, each of the filters was separately applied to each of the images. Such a technique of selecting the structures in the coma was successfully used by Manzini et al (2007) for comet C/2002 C1 Ikeya-Zhang and by Korsun et al (2008; for comets Schwassmann-Wach mann and C/2003 WT42 (LINEAR). Figure 2 shows that the application of the digital fil ters to the images of comet SW1 obtained in Decem ber 2008, allows two jets to be distinguished, and these jets are observed during the whole period of record.…”

Section: Selection Of Jets In the Coma Imagesmentioning

confidence: 99%

The rotation period of comet 29P/Schwassmann-Wachmann 1 determined from the dust structures (Jets) in the coma

et al. 2012

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The results of the photometric observations of comet 29P/Schwassmann-Wachmann 1 are ana lyzed. The comet demonstrates substantial activity at heliocentric distances larger than 5 AU, i.e., outside the water ice sublimation zone. The CCD images of the comet were obtained in wideband R filters at the 6 meter telescope of the Special Astrophysical Observatory of the Russian Academy of Sciences (SAO RAS) and at the 2 meter Zeiss 2000 telescope of the Peak Terskol Observatory. The processing of the images with special digital filters allowed the active structures (jets) to be distinguished in the dust coma of the comet. With the cross correlation method, the rotation period of the cometary nucleus was determined as 12.1 ± 1.2 and 11.7 ± 1.5 days for the observations taken in December 2008, and February 2009, respectively. The probable causes of the difference in the estimates of the rotation period of the cometary nucleus obtained by different authors are discussed.

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Cosmogenic nuclide enhancement via deposition from long-period comets as a test of the Younger Dryas impact hypothesis

Overholt

Melott

2013

Earth and Planetary Science Letters

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We explore the idea that detectable excursions in 26 Al may arise from direct deposition by any bolide, and excursions in 14 C and 10 Be abundances in the atmosphere may result from long-period comet impacts. This is very different from the usual processes of production by cosmic rays within Earth's atmosphere. Long-period comets experience greatly increased cosmic ray flux beyond the protection of the sun's magnetic field. We report the computed amount of 14 C, 10 Be, and 26 Al present on long-period comets as a function of comet mass. We find that the amount of nuclide mass on large long-period comets entering the Earth's atmosphere may be sufficient for creating anomalies in the records of 14 C and 10 Be from past impacts. In particular, the estimated mass of the proposed Younger Dryas comet is consistent with its having deposited sufficient isotopes to account for recorded 14 C and 10

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C/2002 VQ94 (LINEAR) and 29P/Schwassmann–Wachmann 1 — CO+ and N+2 rich comets

Cited by 49 publications

References 34 publications

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

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

The rotation period of comet 29P/Schwassmann-Wachmann 1 determined from the dust structures (Jets) in the coma

Cosmogenic nuclide enhancement via deposition from long-period comets as a test of the Younger Dryas impact hypothesis

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