Distribution and properties of fragments and debris from the split Comet 73P/Schwassmann-Wachmann 3 as revealed by Spitzer Space Telescope

Reach, W. T.; Vaubaillon, Jérémie; Kelley, Michael S. P.; Lisse, C. M.; Sykes, M. V.

doi:10.1016/j.icarus.2009.05.027

Cited by 51 publications

(54 citation statements)

References 42 publications

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“…Our 103P cumulative power-index is −2.7, which is significantly steeper than the distribution of cometary fragments presented in Table 5 of Reach et al (2009), indicating cumulative distributions slightly >−2.0. This seems to indicate that the processes of boulder formation on comets and comets breakups are different.…”

Section: The Comparison Between 103p Boulders and Split Fragments Frocontrasting

confidence: 66%

“…Nonetheless, in few cases, such size-frequency distributions have been identified. Reach et al (2009) studied the distribution and properties of fragments and debris from the split comet 73P/Schwassmann-Wachmann, hereafter 73P, via Spitzer data. Despite the difficulties in identifying the size-frequency distribution of 73P fragments, because many of them were actively emitting dust, Reach et al (2009) find that the cumulative distribution of flux for these fragments has a slope of −0.42 for the small and −0.78 for the large fragments.…”

Section: The Comparison Between 103p Boulders and Split Fragments Fromentioning

confidence: 99%

“…Reach et al (2009) studied the distribution and properties of fragments and debris from the split comet 73P/Schwassmann-Wachmann, hereafter 73P, via Spitzer data. Despite the difficulties in identifying the size-frequency distribution of 73P fragments, because many of them were actively emitting dust, Reach et al (2009) find that the cumulative distribution of flux for these fragments has a slope of −0.42 for the small and −0.78 for the large fragments. As it is the flux proportional to the area, the size-frequency distribution of fragments has slopes of −0.84 and −1.56, respectively, i.e., significantly lower with respect to 103P −2.7 power-index.…”

Section: The Comparison Between 103p Boulders and Split Fragments Fromentioning

confidence: 99%

“…As it is the flux proportional to the area, the size-frequency distribution of fragments has slopes of −0.84 and −1.56, respectively, i.e., significantly lower with respect to 103P −2.7 power-index. By switching to differential size-frequency distributions of −1.84 on 73P small fragments and −2.56 on 73P large fragments, Reach et al (2009) compare 73P results with fragments of comet C/1999 S4 LINEAR (−2.72, as from Mäkinen et al 2001), as well as with fragments derived from the Kreutz group of cometary Sungrazers (−2.7 to −3.0, as from Sekanina 2003), indicating how 73P fragments presents the shallowest power-index slope. Nevertheless, Ishiguro et al (2009) used Subaru/Suprime-Cam data to derive a power-law index of the differential size distribution for 73P of −3.34, which is particularly higher with respect to Reach et al (2009) measurements.…”

Section: The Comparison Between 103p Boulders and Split Fragments Fromentioning

confidence: 99%

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Size-frequency distribution of boulders ≥10 m on comet 103P/Hartley 2

Pajola

Lucchetti

Bertini

et al. 2015

A&A

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Aims. We derive the size-frequency distribution of boulders on comet 103P/Hartley 2, which are computed from the images taken by the Deep Impact/HRI-V imaging system. We indicate the possible physical processes that lead to these boulder size distributions. Methods. We used images acquired by the High Resolution Imager-Visible CCD camera on 4 November 2010. Boulders ≥10 m were identified and manually extracted from the datasets with the software ArcGIS. We derived the global size-frequency distribution of the illuminated side of the comet (∼50%) and identified the power-law indexes characterizing the two lobes of 103P. The three-pixel sampling detection, together with the shadowing of the surface, enables unequivocally detection of boulders scattered all over the illuminated surface. Results. We identify 332 boulders ≥10 m on the imaged surface of the comet, with a global number density of nearly 140/km 2 and a cumulative size-frequency distribution represented by a power law with index of −2.7 ± 0.2. The two lobes of 103P show similar indexes, i.e., −2.7 ± 0.2 for the bigger lobe (called L1) and −2.6 +0.2/ − 0.5 for the smaller lobe (called L2). The similar power-law indexes and similar maximum boulder sizes derived for the two lobes both point toward a similar fracturing/disintegration phenomena of the boulders as well as similar lifting processes that may occur in L1 and L2. The difference in the number of boulders per km 2 between L1 and L2 suggests that the more diffuse H 2 O sublimation on L1 produce twice the boulders per km 2 with respect to those produced on L2 (primary activity CO 2 driven). The 103P comet has a lower global power-law index (−2.7 vs. −3.6) with respect to 67P. The global differences between the two comets' activities, coupled with a completely different surface geomorphology, make 103P hardly comparable to 67P. A shape distribution analysis of boulders ≥30 m performed on 103P suggests that the cometary boulders show more elongated shapes when compared to collisional laboratory fragments as well as to the boulders present on the surfaces of 25 143 Itokawa and 433 Eros asteroids. Consequently, this supports the interpretation that cometary boulders have different origins with respect to the impact-related asteroidal boulders.

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Section: The Comparison Between 103p Boulders and Split Fragments Frocontrasting

confidence: 66%

Section: The Comparison Between 103p Boulders and Split Fragments Fromentioning

confidence: 99%

Section: The Comparison Between 103p Boulders and Split Fragments Fromentioning

confidence: 99%

Section: The Comparison Between 103p Boulders and Split Fragments Fromentioning

confidence: 99%

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Size-frequency distribution of boulders ≥10 m on comet 103P/Hartley 2

Pajola

Lucchetti

Bertini

et al. 2015

A&A

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“…3 Some of the brightest comets ever seen were large Kreutz sungrazers. But a steady stream of smaller fragments also arrive more or less continuously with estimated radii 3 between about 10 m and 1000 m. 4,5 Before the sightings of C/2011 N3 and Lovejoy, though, none had been observed to fly through the solar corona.…”

Section: Sungrazing Cometsmentioning

confidence: 99%

Comets as solar probes

Schrijver¹,

Lisse²,

Downs³

2013

Physics Today

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The Science of Sungrazers, Sunskirters, and Other Near-Sun Comets

et al. 2017

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This review addresses our current understanding of comets that venture close to the Sun, and are hence exposed to much more extreme conditions than comets that are typically studied from Earth. The extreme solar heating and plasma environments that these objects encounter change many aspects of their behaviour, thus yielding valuable information on both the comets themselves that complements other data we have on primitive solar system bodies, as well as on the near-solar environment which they traverse. We propose clear definitions for these comets: We use the term near-Sun comets to encompass all ob- jects that pass sunward of the perihelion distance of planet Mercury (0.307 AU). Sunskirters are defined as objects that pass within 33 solar radii of the Sun's centre, equal to half of Mercury's perihelion distance, and the commonly-used phrase sungrazers to be objects that reach perihelion within 3.45 solar radii, i.e. the fluid Roche limit. Finally, comets with orbits that intersect the solar photosphere are termed sundivers. We summarize past studies of these objects, as well as the instruments and facilities used to study them, including space-based platforms that have led to a recent revolution in the quantity and quality of relevant observations. Relevant comet populations are described, including the Kreutz, Marsden, Kracht, and Meyer groups, near-Sun asteroids, and a brief discussion of their origins. The importance of light curves and the clues they provide on cometary composition are emphasized, together with what information has been gleaned about nucleus parameters, including the sizes and masses of objects and their families, and their tensile strengths. The physical processes occurring at these objects are considered in some detail, including the disruption of nuclei, sublimation, and ionisation, and we consider the mass, momentum, and energy loss of comets in the corona and those that venture to lower altitudes. The different components of comae and tails are described, including dust, neutral and ionised gases, their chemical reactions, and their contributions to the near-Sun environment. Comet-solar wind interactions are discussed, including the use of comets as probes of solar wind and coronal conditions in their vicinities. We address the relevance of work on comets near the Sun to similar objects orbiting other stars, and conclude with a discussion of future directions for the field and the planned ground-and space-based facilities that will allow us to address those science topics.

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Distribution and properties of fragments and debris from the split Comet 73P/Schwassmann-Wachmann 3 as revealed by Spitzer Space Telescope

Cited by 51 publications

References 42 publications

Size-frequency distribution of boulders ≥10 m on comet 103P/Hartley 2

Size-frequency distribution of boulders ≥10 m on comet 103P/Hartley 2

Comets as solar probes

The Science of Sungrazers, Sunskirters, and Other Near-Sun Comets

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