Observations of Comet 19P/Borrelly by the Miniature Integrated Camera and Spectrometer Aboard Deep Space 1

Soderblom, Laurence A.; Becker, T. L.; Bennett, Glenn E.; Boice, D. C.; Britt, D. T.; Brown, R. H.; Buratti, B. J.; Isbell, C. E.; Giese, B.; Hare, T. M.; Hicks, Michael; Howington-Kraus, E.; Kirk, Randolph L.; Lee, Meemong; Nelson, Robert M.; Oberst, J.; Owen, Tobias; Rayman, Marc D.; Sandel, B. R.; Stern, S. A.; Thomas, N.; Yelle, R. V.

doi:10.1126/science.1069527

Cited by 213 publications

(129 citation statements)

References 16 publications

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“…Several considerations suggest that hemispheric albedo variations are not an important source of error. In the cases of 1P/Halley (Keller et al 1987) and 19P/Borrelly (Soderblom et al 2002), we possess in situ, high-resolution images that confirm the geometric interpretation of the light curve. For comets 10P/ Tempel 2, 28P/Neujmin 1, and 49P/Arend-Rigaux, we possess time-resolved measurements of the albedo that show no significant variation with rotational phase (A'Hearn et al 1989;Campins, A'Hearn, & McFadden 1987;Millis, A'Hearn, & Campins 1988).…”

Section: Albedo Variationsmentioning

confidence: 71%

143P/Kowal-Mrkos and the Shapes of Cometary Nuclei

Jewitt¹,

Sheppard²,

Fernández³

2003

Astron J

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We add 143P/Kowal-Mrkos to the small but growing sample of well-observed cometary nuclei. Photometric observations from 3.4 to 4.0 AU heliocentric distance reveal a pointlike object with no detectable outgassing. Periodic modulation of the scattered light (Dm R = 0.45 AE 0.05) is attributed to rotation of the bare nucleus with a double-peaked period 17.21 AE 0.10 hr and a projected ratio of the shortest to longest axis of about 0.67/1. We also measured the phase coefficient (0.043 AE 0.014 mag deg À1 ), the BVRI colors (VÀR = 0.58 AE 0.02), and the absolute red magnitude [m R (1, 1, 0) = 13.49 AE 0.20]. The effective circular radius is 5.7 AE 0.6 km (geometric albedo 0.04 assumed). We study the properties of 11 well-observed Jupiterfamily comet (JFC) nuclei. On average, the nuclei are systematically more elongated (average photometric range Dm R = 0.54 AE 0.07) than main-belt asteroids of comparable size (Dm R = 0.32 AE 0.05) and more elongated than fragments produced in laboratory impact experiments. We attribute the elongation of the nuclei to an evolutionary effect, most likely driven by sublimation-induced mass loss. However, we find no evidence for any relation between the nucleus shape and the sublimation timescale. This may be because the timescale for evolution of the nucleus shape is very short compared with the dynamical timescale for the JFCs, meaning that most nuclei in our sample are already highly physically evolved.

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Section: Albedo Variationsmentioning

confidence: 71%

143P/Kowal-Mrkos and the Shapes of Cometary Nuclei

Jewitt¹,

Sheppard²,

Fernández³

2003

Astron J

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“…The detection of POM in the coma of Halley by means of mass spectrometry, with mass differences between peaks of 15 ± 1 amu (Huebner & Boice 1987), leaves room for a POM structure including NH groups; it was argued, however, that the observed mass spectrum could be due to a CHON molecule and not necessarily a polymer (Mitchell et al 1992). The infrared feature of comet Borrelly ascribed to POM is far too noisy to draw any conclusions (Soderblom et al 2002).…”

Section: Astrophysical Implicationsmentioning

confidence: 99%

UV-photoprocessing of interstellar ice analogs: New infrared spectroscopic results

Muñoz

Schütte

2003

A&A

165

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Abstract. We simulate experimentally the physical conditions present in dense clouds by means of a high vacuum experimental setup at low temperature T ≈ 12 K. The accretion and photoprocessing of ices on grain surfaces is simulated in the following way: an ice layer with composition analogous to that of interstellar ices is deposited on a substrate window, while being irradiated by ultraviolet (UV) photons. Subsequently the sample is slowly warmed up to room temperature; a residue remains containing the most refractory products of photo-and thermal processing. In this paper we report on the Fourier transform-infrared (FT-IR) spectroscopy of the refractory organic material formed under a wide variety of initial conditions (ice composition, UV spectrum, UV dose and sample temperature). The refractory products obtained in these experiments are identified and the corresponding efficiencies of formation are given. The first evidence for carboxylic acid salts as part of the refractory products is shown. The features in the IR spectrum of the refractory material are attributed to hexamethylenetetramine (HMT, [(CH 2 ) 6 N 4 ]), ammonium salts of carboxylic acids [(R-COO − )(NH + )], amides [H 2 NC(=O)-R], esters [R-C(=O)-O-R ] and species related to polyoxymethylene (POM, [(-CH 2 O-) n ]). Furthermore, evidence is presented for the formation of HMT at room temperature, and the important role of H 2 O ice as a catalyst for the formation of complex organic molecules. These species might also be present in the interstellar medium (ISM) and form part of comets. Ongoing and future cometary missions, such as Stardust and Rosetta, will allow a comparison with the laboratory results, providing new insight into the physico-chemical conditions present during the formation of our solar system.

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“…It is a welldocumented comet observed at many of its returns. It was the target of Deep Space 1 mission in 2001 (Soderblom et al 2002).…”

Section: Application To Comet 19p/borrellymentioning

confidence: 99%

CONGO, model of cometary non-gravitational forces combining astrometric and production rate data

Maquet

Colas

Jordá

et al. 2012

A&A

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The gravitational orbit of a comet is affected by the sublimation of water molecules by the nucleus when the comet approaches perihelion. This outgassing triggers a non-gravitational force (NGF) that significantly modifies the orbit of the comet. Up to now, modelling of this effect is mostly based on an empirical model defined in the early 70s that uses a simplified outgassing model. Attempts have been made to use advanced anisotropic thermal models both to calculate the NGF taking several observational constraints into account and to retrieve the nucleus's mass and density, but (i) this approach is restricted to a handful of cometary nuclei that are sufficiently well known to allow this type of modelling, and (ii) the authors usually do not fit the astrometric measurements directly but rather non-gravitational parameters calculated with the above-mentioned empirical model. We present a new model for non-gravitational forces with the aim of revisiting the problem of NGF calculation and nucleus density determination. Our model is closer to the nucleus outgassing physics with only a few free parameters. The amplitude of the perturbation depends on several parameters describing the comet activity that can be constrained by visible, infrared, and radio observations of the coma and the nucleus of the comet. It also depends on the nucleus mass, which can in turn be determined by modelling the effect of the NGF on the orbit of a comet. The method is based on the decomposition of the surface of the nucleus in several elements located at different latitudes. The contribution of each surface element to the overall NGF is fitted from the astrometric measurements, together with the density of the nucleus. This method is the only one available so far to estimate the density of cometary nuclei from ground-based observations. This method is tested on the well-known comet 19P/Borrelly. The density found for these comet is between 150 and 600 kg m −3 .

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Observations of Comet 19P/Borrelly by the Miniature Integrated Camera and Spectrometer Aboard Deep Space 1

Cited by 213 publications

References 16 publications

143P/Kowal-Mrkos and the Shapes of Cometary Nuclei

143P/Kowal-Mrkos and the Shapes of Cometary Nuclei

UV-photoprocessing of interstellar ice analogs: New infrared spectroscopic results

CONGO, model of cometary non-gravitational forces combining astrometric and production rate data

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