Composition of comet Halley dust particles from Giotto observations

Kissel, J.; Brownlee, D. E.; Büchler, K.; Clark, B. C.; Fechtig, H.; Grün, E.; Hornung, Klaus; Igenbergs, E.; Jeßberger, E. K.; Krueger, F. R.; Kuczera, H.; McDonnell, J. A. M.; Morfill, G. E.; Rahe, J.; Schwehm, G.; Sekanina, Z.; Utterback, N. G.; Völk, H. J.; Zook, H. A.

doi:10.1038/321336a0

Cited by 312 publications

(73 citation statements)

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“…The first was ESA's Giotto mission, which flew by Halley's comet in 1985, and took the first image of a cometary nucleus (Reinhard 1986). One of the most significant findings of this mission was that the comet was richer in organics relative to ice than had been expected (Kissel et al 1986). ESA followed up the success of the Giotto mission with the Rosetta mission (Ferri & Schwehm 2005).…”

Section: Comets and The Stardust Missionmentioning

confidence: 99%

UV-Vis spectroscopy of stardust

Fernandes¹,

Johnson²,

Bridges

et al. 2006

International Journal of Astrobiology

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: NASA's Stardust mission flew through the coma of comet Wild 2 in January 2004, capturing dust grains as it did so. The grains were returned safely to Earth in January 2006, and are in the process of being distributed to investigators. As members of the Spectroscopy Preliminary Examination Team, we are preparing to analyse Stardust grains. Our contribution is to measure the spectrum of the grains between 200 nm (in the near ultraviolet) and 800 nm (near infrared). The purpose of the measurement is to provide an additional technique for characterizing the grains, one that is complementary to other spectroscopic techniques and one that produces results that can be matched directly with spectra acquired remotely (with telescope or spacecraft instrumentation). As part of the preparation for analysis of Stardust materials, we are producing a database of spectra from appropriate minerals, and are honing the technique through analysis of primitive meteorites.

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Section: Comets and The Stardust Missionmentioning

confidence: 99%

UV-Vis spectroscopy of stardust

Fernandes¹,

Johnson²,

Bridges

et al. 2006

International Journal of Astrobiology

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“…The temperature of pure silicate grains will be much colder than a blackbody. However, the grains are most likely associated with absorbing material (Kissel et al 1986; Li & Greenberg 1998) sufficient to make them warm. We have left the temperature of the silicate grains as a free parameter, to be determined by the observed flux ratio between the 10 and 25 µm silicate features.…”

Section: Dust Modelsmentioning

confidence: 99%

Broadband infrared photometry of comet Hale-Bopp with ISOPHOT

Grün

Hanner

Peschke

et al. 2001

A&A

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Abstract. Comet Hale-Bopp was observed five times with ISOPHOT, the photometer on board ESA's Infrared Space Observatory (ISO) between 4.6 and 2.8 AU. Each time, broadband photometry was performed using 4 different detectors, 5 apertures and 10 filters covering the range between 3.6 and 170 µm. Background observations were performed with identical instrument settings at the same positions on the sky several days after the comet observations. The observation strategy and the data reduction steps are described in some detail, including the techniques to correct for variable detector responsivity. The resulting inband power values of the Hale-Bopp observations and their uncertainties are given. The mean uncertainty is 25%. The final fluxes were computed, taking into account the zodiacal background, possible offset of the comet's position from the center of the aperture, the brightness distribution within the coma, and the spectral energy distribution of the comet's emission. Strong thermal emission from a broad size distribution of dust particles was detected in all of the data sets, even at r = 4.6-4.9 AU pre-perihelion and 3.9 AU post-perihelion; the total thermal energy varied as r −3 . The 7.3-12.8 µm color temperature was ∼1.5 times the blackbody temperature, higher than that observed in any other comet. Silicate features at 10 and 25 µm were prominent in all 5 data sets, the largest heliocentric distances that silicate emission has been detected in a comet. The presence of crystalline water ice grains is suggested from the 60 µm excess emission at 4.6-4.9 AU, consistent with the observed QOH if the icy grains were slightly warmer than an equilibrium blackbody. The average albedo of the dust is higher than that of comet P/Halley, but lower than other albedo measurements for Hale-Bopp nearer perihelion. There is no evidence for a component of cold, bright icy grains enhancing the scattered light at 4.6 AU. Simple models for a mixture of silicate and absorbing grains were fit to the ISO spectra and photometry at 2.8 AU. The observed flux at λ > 100 µm requires a size distribution in which most of the mass is concentrated in large particles. Dust production rates of order 1.5 × 10 5 kg s −1 at 2.8 AU and 3 × 10 4 kg s −1 at 4.6 AU have been found. They correspond to dust to gas mass ratios of 6 to 10. † Deceased.Article published by EDP Sciences and available at http://www.aanda.org or http://dx

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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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Composition of comet Halley dust particles from Giotto observations

Cited by 312 publications

References 4 publications

UV-Vis spectroscopy of stardust

UV-Vis spectroscopy of stardust

Broadband infrared photometry of comet Hale-Bopp with ISOPHOT

Polarization studies of comet C/2000 WM1 (LINEAR)

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