Optical probing of comet Halley from the Giotto spacecraft

Levasseur-Regourd, A. C.; Bertaux, Jean-Loup; Dumont, René; Festou, M. C.; Giese, R. H.; Giovane, F.; Lamy, Philippe; Blanc, Jean-Jacques; Llebaria, A.; Weinberg, J. L.

doi:10.1038/321341a0

Cited by 57 publications

(10 citation statements)

References 4 publications

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“…The deduced gradient of the overall coma profile (−1.1) is consistent with the expected value (−1) and with other observations for P/Halley (e.g. Levasseur-Regourd et al 1986;Gammelgaard & Thomson 1988). The gradient of the tailward profile (−.86) is consistent with the ρ −1 law, too, whereas the sunward gradient (−1.6) shows a significant deviation.…”

Section: Intensity and Column Density Profilessupporting

confidence: 91%

Spatial distribution of neutral and ionic constituents in comet P/Halley

Umbach

Jockers

Geyer

1998

Astron. Astrophys. Suppl. Ser.

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Abstract. Multislit spectra of comet P/Halley were obtained on April 10, 1986, using a focal reducer with a field of ≈ 0.5• angular diameter. The number and arrangement of the slits allowed a reconstruction of the spatial distribution of principal neutral and ionic coma constituents within a frame of about 4 10 5 × 4 10 5 km 2 at the comet. Radial profiles and two-dimensional maps for the dust continuum, CN, C 3 , CH, CO + , and especially CO + 2 , are presented in absolute intensity and column density units, respectively. Scale lengths and production rates for the radicals were determined within the Haser model. The molecular ions are not only restricted to the plasma tail but are also present in the sunward coma. Instead of forming a peak at the nucleus like the neutral radicals the ion column densities decrease rapidly in the solar direction and form a plateau extending from the nucleus into the antisolar direction. The distribution of CO + 2 shows a stronger decrease in the tailward direction than that of CO + .

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Section: Intensity and Column Density Profilessupporting

confidence: 91%

Spatial distribution of neutral and ionic constituents in comet P/Halley

Umbach

Jockers

Geyer

1998

Astron. Astrophys. Suppl. Ser.

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“…The study of the dust grains in comets has been an active area of investigation for quite some time but the exact nature and composition of the cometary grains are still not well understood. Dollfus (1989) pointed out the Send offprint requests to: U. C. Joshi, e-mail: joshi@prl.ernet.in possibility of the grains giving rise to the polarization being large, rough and dark, resembling fluffy aggregates such as Brownlee particles.The space mission to Comet Halley made some in-situ measurements and have contributed new information on the nature of grains in that comet (Kissel et al 1986;Mazets et al 1986;Levasseur-Regourd et al 1986). However, ground based observations have indicated that the detailed behaviour of grains differs in different comets.…”

Section: Introductionmentioning

confidence: 99%

Polarization studies of comet C/2000 WM1 (LINEAR)

Joshi

Baliyan

Ganesh

2003

A&A

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• ) when the polarization is negative and where the data for most of the comets are rather meager. The observations during March were made when the phase angle was ∼47• . Observations were conducted through the IHW narrow band and BVR broad band filters. Based on these polarization observations we infer that the comet C/2000 WM1 belongs to high polarization class i.e. the dusty comet family.

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“…Other polarimetric observations on P/Halley suitable for dust characterization were recorded by Bastien et al (1986Bastien et al ( , 1987, Kikuchi et al (1987), Kiselev et al (1986), Le Borgne et al (1987), Brooke et al (1987) and Vrba (1987). The instrument HOPE on-board spacecraft GIOTTO recorded in situ data (Levasseur-Regourd et al, 1986). All those measurements pertaining to the dust characterization have been analysed jointly in a workshop study in Paris on April 2-3, 1987, and synthetic linear polarization phase variation curves have been derived (Dollfus et al, 1988).…”

Section: Characterization Of the Coma Grains By Telescopic Photopolarmentioning

confidence: 99%

Cometary Dust and Zodiacal Light Connection

Dollfus

1989

Highlights astron.

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Photopolarimetry of P/Halley coma characterizes, in the cloud of dust grains released by the nucleus, the presence of a significant population of large flakes, made of aggregated small and very dark grains. These globules are subsequently transported toward the Sun, with some modifications in texture, and concentrate in the inner part of the Solar System. Comets appear to be the source for the fluffy grains which are observed in the zodiacal light.

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Optical probing of comet Halley from the Giotto spacecraft

Cited by 57 publications

References 4 publications

Spatial distribution of neutral and ionic constituents in comet P/Halley

Spatial distribution of neutral and ionic constituents in comet P/Halley

Polarization studies of comet C/2000 WM1 (LINEAR)

Cometary Dust and Zodiacal Light Connection

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