Dust From the Solar System and Beyond

Rotundi, A.; Fulle, M.; Corte, Vincenzo Della

doi:10.1016/b978-0-12-409548-9.11988-8

Cited by 8 publications

(12 citation statements)

References 32 publications

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“…Furthermore, they are mostly perpendicular to the surface where they first emerge. In the coma images of OSIRIS, the dust sizes should be on the order of 0.1-1 mm according to Rotundi et al (2015). This estimate is consistent with the model calculation of the curved jets by Lin et al (2016).…”

Section: Methodssupporting

confidence: 85%

Seasonal variations in source regions of the dust jets on comet 67P/Churyumov-Gerasimenko

Lai

Lee

et al. 2019

A&A

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Aims. We investigate the surface distribution of the source regions of dust jets on comet 67P/Churyumov-Gerasimenko as a function of time. Methods. The dust jet source regions were traced by the comprehensive imaging data set provided by the OSIRIS scientific camera. Results. We show in detail how the projected footpoints of the dust jets and hence the outgassing zone would move in consonance with the sunlit belt. Furthermore, a number of source regions characterized by repeated jet activity might be the result of local topographical variations or compositional heterogeneities. Conclusions. The spatial and temporal variations in source regions of the dust jets are influenced significantly by the seasonal effect. The strong dependence on the solar zenith angle and local time could be related to the gas sublimation process driven by solar insolation on a surface layer of low thermal inertia.

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Section: Methodssupporting

confidence: 85%

Seasonal variations in source regions of the dust jets on comet 67P/Churyumov-Gerasimenko

Lai

Lee

et al. 2019

A&A

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“…The targets were exposed on movable target holders that could be placed in front of a funnel in such a way that the cometary dust that entered the instrument was focused onto the collection target. The impact velocity of the particles was not higher than 10 m s −1 (Rotundi et al 2015), which is much lower than the collection velocity of 6 km s −1 during the Stardust mission (Brownlee et al 2006) and the encounter speeds of about 78 and 68 km s −1 estimated for the Vega (Sagdeev et al 1986) and Giotto (Reinhard 1986) spacecrafts, respectively. Considering this low capture velocity, the chemical composition of particles of 67P is very probably not altered by the capture process.…”

Section: Cosima Instrumentmentioning

confidence: 64%

H/C elemental ratio of the refractory organic matter in cometary particles of 67P/Churyumov-Gerasimenko

Isnard

Bardyn

Fray

et al. 2019

A&A

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Context. Because comets are part of the most primitive bodies of our solar system, establishing their chemical composition and comparing them to other astrophysical bodies gives new constraints on the formation and evolution of organic matter throughout the solar system. For two years, the time-of-flight secondary ion mass spectrometer COmetary Secondary Ion Mass Analyzer (COSIMA) on board the Rosetta orbiter performed in situ analyses of the dust particles ejected from comet 67P/Churyumov-Gerasimenko (67P). Aims. The aim is to determine the H/C elemental ratio of the refractory organic component contained in cometary particles of 67P. Methods. We analyzed terrestrial and extraterrestrial calibration samples using the COSIMA ground-reference model. Exploiting these calibration samples, we provide calibration lines in both positive and negative ion registration modes. Thus, we are now able to measure the cometary H/C elemental ratio. Results. The mean H/C value is 1.04 ± 0.16 based on 33 different cometary particles. Consequently, the H/C atomic ratio is on average higher in cometary particles of 67P than in even the most primitive insoluble organic matter extracted from meteorites. Conclusions. These results imply that the refractory organic matter detected in dust particles of 67P is less unsaturated than the material in meteorites.

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“…However, this distribution varies from differential size distributions derived from cometary trail observations: for example, modelling of the dust emission of 67P/Churyumov-Gerasimenko by Agarwal et al (2010) to match Spitzer infrared observations of the trail requires D mid ≈ 2 µm, α = 3.7, and β = 1.8. Measurements at this comet suggest similar slopes, but a different knee of the distribution: Rotundi et al (2015) report a size distribution from the GIADA instrument with a slope of −4 for particles >1 mm and a slope of −2 for smaller particles. However, Fulle et al (2016) report that the size distribution of dust emitted by 67P/Chruyumov-Gerasimenko also varies with heliocentric distance.…”

Section: Discussionmentioning

confidence: 81%

IMEM2: a meteoroid environment model for the inner solar system

Soja

Grün

Strub

et al. 2019

A&A

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Context. The interplanetary dust complex is currently understood to be largely the result of dust production from Jupiter-family comets, with contributions also from longer-period comets (Halley- and Oort-type) and collisionally produced asteroidal dust. Aims. Here we develop a dynamical model of the interplanetary dust cloud from these source populations in order to develop a risk and hazard assessment tool for interplanetary meteoroids in the inner solar system. Methods. The long-duration (1 Myr) integrations of dust grains from Jupiter-family and Halley-type comets and main belt asteroids were used to generate simulated distributions that were compared to COBE infrared data, meteor data, and the diameter distribution of lunar microcraters. This allowed the constraint of various model parameters. Results. We present here the first attempt at generating a model that can simultaneously describe these sets of observations. Extended collisional lifetimes are found to be necessary for larger (radius ≥ 150 μm) particles. The observations are best fit with a differential size distribution that is steep (slope = 5) for radii ≥ 150 μm, and shallower (slope = 2) for smaller particles. At the Earth the model results in ~ 90–98% Jupiter-family comet meteoroids, and small contributions from asteroidal and Halley-type comet particles. In COBE data we find an approximately 80% contribution from Jupiter-family comet meteoroids and 20% from asteroidal particles. The resulting flux at the Earth is mostly within a factor of about two to three of published measurements.

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Dust From the Solar System and Beyond

Cited by 8 publications

References 32 publications

Seasonal variations in source regions of the dust jets on comet 67P/Churyumov-Gerasimenko

Seasonal variations in source regions of the dust jets on comet 67P/Churyumov-Gerasimenko

H/C elemental ratio of the refractory organic matter in cometary particles of 67P/Churyumov-Gerasimenko

IMEM2: a meteoroid environment model for the inner solar system

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