Dust density and mass distribution near comet Halley from Giotto observations

McDonnell, J. A. M.; Alexander, W. M.; Burton, W. M.; Bussoletti, E.; Clark, David H.; Grard, R.; Grün, E.; Hanner, M. S.; Hughes, David W.; Igenbergs, E.; Kuczera, H.; Lindblad, B. A.; Mandeville, J. C.; Minafra, A.; Schwehm, G.; Sekanina, Z.; Wallis, M. K.; Zarnecki, J. C.; Chakaveh, S.; Evans, G. C.; Evans, S. T.; Firth, J. G.; Littler, A. N.; Massonne, L.; Olearczyk, R. E.; Pankiewicz, G. S.; Stevenson, T.; Turner, R. F.

doi:10.1038/321338a0

Cited by 122 publications

(20 citation statements)

References 9 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Moreno et al (2008) studied the morphology of the dust cloud in terms of the dynamics of the particles, and found that >600 μm particles, which are much less sensitive to radiation pressure than micrometersized or smaller particles, could be ejected by the outburst. Evidence of such large particles is found to be ubiquitous in in situ observations (McDonnell et al 1986;Tuzzolino et al 2003), by the remote sensing observations of dust tail (Fulle 2004;Moreno 2009;Watanabe et al 1990) and dust trail Ishiguro 2008;Sarugaku et al 2007;Reach et al 2000Reach et al , 2007Kelley et al 2008), sub-millimeter and millimeter observations (Jewitt & Matthews 1997;Altenhoff et al 1999). As a result of these studies, we found that the power index of the size distribution of almost all comets would be in the range of −4 and −3 (Fulle 2004).…”

Section: Mass Erosionmentioning

confidence: 97%

2007 Outburst of 17p/Holmes: The Albedo and the Temperature of the Dust Grains

Ishiguro¹,

Watanabe²,

Sarugaku³

et al. 2010

ApJ

View full text Add to dashboard Cite

Based on optical and infrared observations, we study the albedo and the temperature of the dust grains associated with the spectacular 2007 outburst of Jupiter-family comet 17P/Holmes. We found that the albedo at the solar phase angle ∼16 • was 0.03-0.12. While the color temperature around 3-4 μm was 360 ± 40 K, the color temperature at 12.4 μm and 24.5 μm was ∼200 K, which is consistent with that of a blackbody. We studied the equilibrium temperature of the dust grains at 2.44 AU and found that the big discrepancy in the temperature was caused by the heterogeneity in particle size, that is, hotter components consist of submicron absorbing grains whereas colder components consist of large ( 1 μm) grains. The contemporaneous optical and mid-infrared observations suggest that the albedo and the temperature could decrease within ∼ 3 days after the outburst and stabilized at typical values of the other comets. We estimated the total mass injected into the coma by the outburst on the basis of the derived albedo and the optical magnitude for the entire dust cloud, and found that at least 4 × 10 10 kg (equivalent to a few meter surface layer) was removed by the initial outburst event. The derived mass suggests that the outburst is explainable by neither the exogenetic asteroidal impact nor water ice sublimation driven by solar irradiation, but by an endogenic energy source. We conclude that the outburst was triggered by the energy sources several meters or more below the nuclear surface.

show abstract

Section: Mass Erosionmentioning

confidence: 97%

2007 Outburst of 17p/Holmes: The Albedo and the Temperature of the Dust Grains

Ishiguro¹,

Watanabe²,

Sarugaku³

et al. 2010

ApJ

View full text Add to dashboard Cite

show abstract

“…(3). By using a 1 = 0.01 μm, corresponding to the radius of small refractory particle found in cometary grain (e.g., McDonnell et al, 1986), we reexamined the thermal radiation from EKB dust cloud. We found that the change of a 1 from 0.1 μm to 0.01 μm leads to a decrease of the total thermal radiation one third of that for a 1 = 0.1 μm.…”

Section: Thermal Emission From Ekb Dust Cloudmentioning

confidence: 99%

Thermal radiation from dust grains in Edgeworth-Kuiper Belt

Yamamoto

Mukai

2014

Earth Planet Sp

View full text Add to dashboard Cite

We calculate the temperature of dust grains produced in Edgeworth-Kuiper Belt (EKB) based on the grain model for water-ice and silicate mixtures. The dust grains with radii ranging from 0.1 μm to 1 mm have low temperatures of about 20 K to 50 K in EKB, depending on their size, solar distance, and a volume mixing ratio of silicate to water-ice. We also estimate the thermal radiation from dust cloud in EKB. The result of thermal emission shows the spectral feature of water-ice at the wavelength of about 60 μm. Although it is difficult to estimate the possibility to detect the thermal emission spectrum of EKB dust cloud, due to large uncertainties in its spatial density, we found that the thermal emission of dust cloud in EKB lies below the IRAS data of foreground zodiacal emission. The maximum value of the thermal emission derived from the acceptable dust cloud model in EKB, however, becomes to be comparable to that of foreground zodiacal emission in far-infrared and submillimeter wavelength domains. Since the EKB dust cloud seems to concentrate near the ecliptic plane, a scanning of infrared observation along a line perpendicular to the ecliptic plane may reveal the presence of such dust cloud in the future.

show abstract

“…We thus assumed in this model that the molar fraction of the volatile x released by the clathrate structure is the average over the layer of the volatile References. (a) Kossacki & Szutowicz (2006), (b) Carman (1956), Mekler et al (1990), (c) McDonnell et al (1986), Huebner et al (2006).…”

Section: Composition Of Volatile Molecules Both Trapped and Released mentioning

confidence: 99%

“…In this work, we assume a power of order −3.5 for the size distribution of dust grains (McDonnell et al 1986;Huebner et al 2006) with a cut-off at a radius of 1 cm (Prialnik 1997). The initial temperature is assumed to be equal to 30 K. Davidsson & Gutierrez (2005) give a density of 100−600 kg m −3 for the comet 67P/Churyumov-Gerasimenko, leading to porosities greater than 60%.…”

Section: Orbital and Physical Parameters Adoptedmentioning

confidence: 99%

A cometary nucleus model taking into account all phase changes of water ice: amorphous, crystalline, and clathrate

Marboeuf

Schmitt

Petit

et al. 2012

A&A

View full text Add to dashboard Cite

Context. Current theories, models of cometary nuclei and of ice formation in the protoplanetary disk, and laboratory studies suggest that cometary materials could be formed of pure crystalline water ice, amorphous water ice, clathrate hydrate, or a mixture of these structures of water ice. However, current models of cometary nuclei consider only two forms of ice during the thermodynamic evolution of comets: amorphous and crystalline water ices. Aims. In this work, we have developed a model of cometary nucleus that takes into account all water ice structures and phase changes in order to predict the outgassing profile of volatile molecules that could be measured by the Rosetta mission and can be used to constrain the structural type of ice existing in the interior of the Comet 67P/Churyumov-Gerasimenko, the target comet of the Rosetta mission, and, hopefully, its initial composition. Methods. We added the physic of formation/dissociation of clathrate hydrates in addition to others physical processes that are taken into account in models without clathrate hydrates. All thermal changes, as well as the release and trapping of gas with water phase changes are taken into account. Results. This model describes heat transmission, latent heat exchanges, all water ices structures and transitions (amorphous-to-pure crystalline, amorphous-to-clathrate hydrates and pure crystalline-to-clathrate hydrates and vise versa), sublimation/recondensation of volatile molecules in the nucleus, gas diffusion, gas released and trapped by crystallization and clathrate formation/dissociation processes, as well as gas and dust release and mantle formation at the surface. Applying this model to the comet 67P/ChuryumovGerasimenko, results show different outgassing profiles of volatiles molecules from the nucleus depending on the water ice structure, the distribution of volatile molecules between the "trapped" and "condensed" states in the nucleus and the thermal inertia of its porous matrix. Conclusions. Given these results, we pretend that this model is able to constrain the water ice structure and chemical composition in comets from outgassing profiles of volatile molecules, and especially those of the target comet of the Rosetta mission.

show abstract

Dust density and mass distribution near comet Halley from Giotto observations

Cited by 122 publications

References 9 publications

2007 Outburst of 17p/Holmes: The Albedo and the Temperature of the Dust Grains

2007 Outburst of 17p/Holmes: The Albedo and the Temperature of the Dust Grains

Thermal radiation from dust grains in Edgeworth-Kuiper Belt

A cometary nucleus model taking into account all phase changes of water ice: amorphous, crystalline, and clathrate

Contact Info

Product

Resources

About