67P/C-G inner coma dust properties from 2.2 au inbound to 2.0 au outbound to the Sun

Corte, Vincenzo Della; Rotundi, A.; Fulle, M.; Ivanovski, S.; Green, Simon; Rietmeijer, Frans J. M.; Colangeli, L.; Palumbo, P.; Sordini, R.; Ferrari, M.; Accolla, M.; Захаров, Владимир; Epifani, E. Mazzotta; Weissman, P. R.; Grüen, E.; Moreno, J. J. Lopez; Rodriguez, J.; Bussoletti, E.; Crifo, J. F.; Esposito, F.; Lamy, Philippe; McDonnell, J. A. M.; Mennella, V.; Molina, A.; Morales, R.; Moreno, Fernando; Palomba, E.; Perrin, J. M.; Rodrigo, R.; Zarnecki, J. C.; Cosi, M.; Giovane, F.; Gustafson, B. Å. S.; Ortiz, J. L.; Jeronimo, J. M.; Leese, M. R.; Herranz, M.; Liuzzi, V.; López-Jiménez, A.

doi:10.1093/mnras/stw2529

Cited by 49 publications

(20 citation statements)

References 20 publications

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“…1). The experiments span a velocity range of 0.3 -6 m s −1 , which overlaps with the range measured on particles from 67P that entered the GIADA instrument (Fulle et al 2016;Della Corte et al 2016). A total of 110 dust particles in the size range 30-410 µm could be traced on the video images and their deposits subsequently identified on the target.…”

Section: Resultsmentioning

confidence: 93%

“…On one hand there are detections of 'compact' particles about 80-800 µm. These particles enter the instrument at velocities typically in the range 0.5 -15 m s −1 , with a few detections up to 35 m s −1 when the comet was near perihelion (Della Corte et al 2016). On the other hand, collections of intermittent showers of smaller particles are hypothesized to be the fragments of a low-density, fluffy component (Fulle et al 2015).…”

Section: Introductionmentioning

confidence: 99%

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The footprint of cometary dust analogues – I. Laboratory experiments of low-velocity impacts and comparison with Rosetta data

Ellerbroek

Gundlach

Landeck

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Cometary dust provides a unique window on dust growth mechanisms during the onset of planet formation. Measurements by the Rosetta spacecraft show that the dust in the coma of comet 67P/Churyumov-Gerasimenko has a granular structure at size scales from sub-µm up to several hundreds of µm, indicating hierarchical growth took place across these size scales. However, these dust particles may have been modified during their collection by the spacecraft instruments. Here we present the results of laboratory experiments that simulate the impact of dust on the collection surfaces of COSIMA and MIDAS, instruments onboard the Rosetta spacecraft. We map the size and structure of the footprints left by the dust particles as a function of their initial size (up to several hundred µm) and velocity (up to 6 m s −1 ). We find that in most collisions, only part of the dust particle is left on the target; velocity is the main driver of the appearance of these deposits. A boundary between sticking/bouncing and fragmentation as an outcome of the particle-target collision is found at v ∼ 2 m s −1 . For velocities below this value, particles either stick and leave a single deposit on the target plate, or bounce, leaving a shallow footprint of monomers. At velocities > 2 m s −1 and sizes > 80 µm, particles fragment upon collision, transferring up to 50 per cent of their mass in a rubble-pile-like deposit on the target plate. The amount of mass transferred increases with the impact velocity. The morphologies of the deposits are qualitatively similar to those found by the COSIMA instrument.

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Section: Resultsmentioning

confidence: 93%

Section: Introductionmentioning

confidence: 99%

The footprint of cometary dust analogues – I. Laboratory experiments of low-velocity impacts and comparison with Rosetta data

Ellerbroek

Gundlach

Landeck

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…Instruments onboard Rosetta have provided information on the physics of 67P dust in the coma, including dust size and velocity distribution. The Grain Impact Analyser and Dust Accumulator (GIADA, Della Corte et al, 2014)) measured sizes from 100 μm to millimetres and characterised the dust flux (Rotundi et al, 2015;Della Corte et al, 2016;Fulle et al, 2016b). The Cometary Secondary Ion Mass Analyser (COSIMA, Henkel et al, 2003) measured sizes from tens of micrometres to millimetres (Langevin et al, 2016;.…”

Section: Introductionmentioning

confidence: 99%

Refractory and semi-volatile organics at the surface of comet 67P/Churyumov-Gerasimenko: Insights from the VIRTIS/Rosetta imaging spectrometer

Quirico

Moroz

Schmitt

et al. 2016

Icarus

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Laboratory spectral measurements of relevant analogue materials were performed in the framework of the Rosetta mission in order to explain the surface spectral properties of comet 67P. Fine powders of coal, iron sulphides, silicates and their mixtures were prepared and their spectra measured in the Vis-IR range. These spectra are compared to a reference spectrum of 67P nucleus obtained with the VIRTIS/Rosetta instrument up to 2.7 μm, excluding the organics band centred at 3.2 μm. The species used are known to be chemical analogues for cometary materials which could be present at the surface of 67P. Grain sizes of the powders range from tens of nanometres to hundreds of micrometres. Some of the mixtures studied here actually reach the very low reflectance level observed by VIRTIS on 67P. The best match is provided by a mixture of sub-micron coal, pyrrhotite, and silicates. Grain sizes are in agreement with the sizes of the dust particles detected by the GIADA, MIDAS and COSIMA instruments on board Rosetta. The coal used in the experiment is responsible for the spectral slope in the visible and infrared ranges. Pyrrhotite, which is strongly absorbing, is responsible for the low albedo observed in the NIR. The darkest components dominate the spectra, especially within intimate mixtures. Depending on sample preparation, pyrrhotite can coat the coal and silicate aggregates. Such coating effects can affect the spectra as much as particle size. In contrast, silicates seem to play a minor role.

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“…In order to study the temporal variation of dust ejection, we defined six periods, corresponding to the different orbital stages of comet 67P and characterized by different altitudes of the Rosetta spacecraft above the surface. The periods' definition is the same as the one proposed by Della Corte et al (2016a) and is summarized in Table 1, together with the number of GIADA individual particles detected during each period.…”

Section: Datamentioning

confidence: 99%

67P/Churyumov–Gerasimenko’s dust activity from pre- to post-perihelion as detected by Rosetta/GIADA

Longobardo

Corte

Rotundi

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We characterized the 67P/Churyumov–Gerasimenko’s dust activity, by analysing individual dust particle velocity and momentum measurements of Grain Impact Analyser and Dust Accumulator (GIADA), the dust detector onboard the ESA/Rosetta spacecraft, collecting dust from tens to hundreds of kilometres from the nucleus. Specifically, we developed a procedure to trace back the motion of dust particles down to the nucleus, identifying the surface’s region ejecting each dust particle. This procedure has been developed and validated for the first part of the mission by Longobardo et al. and was extended to the entire GIADA data set in this work. The results based on this technique allowed us to investigate the link between the dust porosity (fluffy/compact) and the morphology of the ejecting surface (rough/smooth). We found that fluffy and compact particles, despite the lack of correlation in their coma spatial distribution (at large nucleocentric distances) induced by their different velocities, have common ejection regions. In particular, the correlation between the distributions of fluffy and compact particles is maintained up to an altitude of about 10 km. Fluffy particles are more abundant in rough terrains. This could be the result of past cometary activity that resurfaced the smooth terrains and/or of the comet formation process that stored the fluffy particles inside the voids between the pebbles. The variation of fluffy particle concentration between rough and smooth terrains agrees with predictions of comet formation models. Finally, no correlation between dust distribution on the nucleus and surface thermal properties was found.

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67P/C-G inner coma dust properties from 2.2 au inbound to 2.0 au outbound to the Sun

Cited by 49 publications

References 20 publications

The footprint of cometary dust analogues – I. Laboratory experiments of low-velocity impacts and comparison with Rosetta data

The footprint of cometary dust analogues – I. Laboratory experiments of low-velocity impacts and comparison with Rosetta data

Refractory and semi-volatile organics at the surface of comet 67P/Churyumov-Gerasimenko: Insights from the VIRTIS/Rosetta imaging spectrometer

67P/Churyumov–Gerasimenko’s dust activity from pre- to post-perihelion as detected by Rosetta/GIADA

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