The dust distribution within the inner coma of comet P/Halley 1982i: encounter by Giotto’s impact detectors

McDonnell, J. A. M.; Alexander, W. M.; Burton, W. M.; Bussoletti, E.; Evans, G. C.; Evans, S. T.; Firth, J. G.; Grard, R.; Green, S. F.; Grün, E.; Hanner, M. S.; Hughes, David W.; Igenbergs, E.; Kissel, J.; Kuczera, H.; Lindblad, B. A.; Langevin, Y.; Mandeville, J. C.; Nappo, S.; Pankiewicz, G. S.; Perry, C. H.; Schwehm, G.; Sekanina, Z.; Stevenson, T.; Turner, R. F.; Weishaupt, U.; Wallis, M. K.; Zarnecki, J. C.

doi:10.1007/978-3-642-82971-0_127

Cited by 69 publications

(54 citation statements)

References 25 publications

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“…In situ dust analysis performed during the Halley flyby missions [55,61] has revealed a very broad dust mass spectrum, covering at least the range of 10" 17 to 10~3 g. To allow for this fact, models use the "discrete approximation" by which the dust is represented by a certain number of single-size elementary fluids.…”

Section: 3 Size Distributionmentioning

confidence: 99%

“…Notice, however, that small grains (< 10" 14 g) remain velocity-accommodated to the gas up to [18]. The expansion of a mixture of water and of amorphous carbon grains with a density of 0.3 g-cm-3 an d vvith the in situ measured size distribution [55,61] is computed. Dusty ice sublimation boundary conditions are assumed.…”

Section: 3 Size Distributionmentioning

confidence: 99%

“…There is no universal answer to such a question. However, in the case of the in situ measured Halley dust distribution (as described in the interim assessment [55]), it has been shown, using the results of an hydrodynamic model incorporating 44 different grain mass intervals [22], that:…”

Section: 3 Size Distributionmentioning

confidence: 99%

“…Indeed, preliminary investigation reveals that this is probably not circumstantial: rotational cooling operates as a feedback mechanism that of use, available at https://www.cambridge.org/core/terms. https://doi.org/10.1017/S0252921100012781 [55,61], water recondensation [21] and water radiative losses computed from a realistic excitation model [6]. Photochemical heating is approximated by an analytic expression [7].…”

Section: Radiative Budget Of the Water Molecule Ignoring The Dust Anmentioning

confidence: 99%

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Hydrodynamic Models of the Collisional Coma

Crifo

1991

International Astronomical Union Colloquium

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ABSTRACT. The hydrodynamic approach to the modeling of the coUisional regions of the cometary atmospheres is reviewed. A concise account of the existing Monte Carlo simulations is also incorporated. Emphasis is placed on works stimulated by the Halley flyby missions. The basic physical processes are described, based on the analogy with the physics of underexpanded jets. The general structure of the governing equations is presented and their legacy discussed. A detailed intercomparison is made of the application of these methods to the modeling of the comas. The reliability of the conclusions brought forward by existing models is discussed. . IntroductionIn view of the extreme rarity of past and foreseeable in situ cometary missions, remote sensing of comets has been and will continue to be the essential tool of cometary investigation. Therefore, most properties (and, in particular, the statistical properties) of the solid nucleus of all comets have been and will continue to be inferred from observations of the cometary atmosphere-the coma. With the refinements of the observational techniques, a detailed and reliable understanding of the formation of the coma has emerged as a key objective of cometary physics.The application of gas-dynamic methods to the formation of the coma seems to date only back to the year 1965. Fluid equations were first used in order to account for the acceleration of cometary dust and for the formation of many minor molecules. It is not a simple problem to delineate the precise extent of the collision-dominated part of a coma, i.e., that region where hydrostatic or hydrodynamic methods provide satisfactory results (see Sections 3.3 to 3.5). Primitive considerations, based on evaluations of the ratio of the local collision mean free path (m.f.p.) to the cometocentric distance, suggest that a waterdominated coma has a very small collision zone beyond an heliocentric distance = 3 AU, while that zone covers the whole water survival zone within = 0.5 AU (see, e.g., [13,17]). The essential point, however, is that the distribution of matter in the coma, the dynamical properties of all constituents, and the chemical composition of the gas phase are 937

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Section: 3 Size Distributionmentioning

confidence: 99%

Section: 3 Size Distributionmentioning

confidence: 99%

Section: 3 Size Distributionmentioning

confidence: 99%

Section: Radiative Budget Of the Water Molecule Ignoring The Dust Anmentioning

confidence: 99%

See 2 more Smart Citations

Hydrodynamic Models of the Collisional Coma

Crifo

1991

International Astronomical Union Colloquium

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“…Therefore we should look at the adjusted values as parameters needed to compare the results derived from the different observations, but should not interpret them in terms of scattering properties of the cometary dust grains. (Mazets et al, 1986;McDonnell et al, 1987). Therefore particle size distributions significantly different from a power law like those generated by particle size orders > 1 do not appear realistic (Fulle, 2004).…”

Section: Application Of the Model 431 The Calculated Inverse Solutimentioning

confidence: 99%

A dynamical model with a new inversion technique applied to observations of Comet C/2000 WM1 (LINEAR)☆

Bonev

Jockers

Karpov

2008

Icarus

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A database of interplanetary and interstellar dust detected by the Wind spacecraft

Malaspina

Wilson

2016

JGR Space Physics

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It was recently discovered that the WAVES instrument on the Wind spacecraft has been detecting, in situ, interplanetary and interstellar dust of approximately 1 μm radius for the past 22 years. These data have the potential to enable advances in the study of cosmic dust and dust‐plasma coupling within the heliosphere due to several unique properties: the Wind dust database spans two full solar cycles; it contains over 107,000 dust detections; it contains information about dust grain direction of motion; it contains data exclusively from the space environment within 350 Earth radii of Earth; and it overlaps by 12 years with the Ulysses dust database. Further, changes to the WAVES antenna response and the plasma environment traversed by Wind over the lifetime of the Wind mission create an opportunity for these data to inform investigations of the physics governing the coupling of dust impacts on spacecraft surfaces to electric field antennas. A Wind dust database has been created to make the Wind dust data easily accessible to the heliophysics community and other researchers. This work describes the motivation, methodology, contents, and accessibility of the Wind dust database.

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The dust distribution within the inner coma of comet P/Halley 1982i: encounter by Giotto’s impact detectors

Cited by 69 publications

References 25 publications

Hydrodynamic Models of the Collisional Coma

Hydrodynamic Models of the Collisional Coma

A dynamical model with a new inversion technique applied to observations of Comet C/2000 WM1 (LINEAR)☆

A database of interplanetary and interstellar dust detected by the Wind spacecraft

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