IMEM2: a meteoroid environment model for the inner solar system

Soja, R.; Grün, E.; Strub, Peter; Sommer, Maximilian; Millinger, Mark; Vaubaillon, Jérémie; Alius, W.; Camodeca, G.; Hein, F.; Laskar, Jacques; Fienga, A.; Schwarzkopf, Gabriel Jörg; Herzog, J.; Gutsche, K.; Skuppin, Nikolai; Srama, R.

doi:10.1051/0004-6361/201834892

Cited by 28 publications

(29 citation statements)

References 57 publications

(100 reference statements)

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“…In order to identify time intervals when the Helios spacecraft traversed cometary meteoroid trails, we use the IMEX dust streams in space model developed by Soja et al (2015bSoja et al ( ,a, 2019. The model generates trails for 362 Jupiter-family, 40 Halley-type, and 18 Encke-type comets available in the JPL Small Body Database (SBDB) as of 1 August 2013, which have perihelion distances q < 3 AU, semimajor axes a < 30 AU, and defined total visual magnitudes.…”

Section: Imex Cometary Trails Modelmentioning

confidence: 99%

“…Recently, the Interplanetary Meteoroid Environment for eXploration (IMEX) dust streams in space model was developed by Soja et al (2015bSoja et al ( ,a, 2019 under contract by the European Space Agency. IMEX is a new universal and physical model for dust dynamics and orbital evolution that simulates recently created cometary dust trails in the inner Solar System.…”

Section: Introductionmentioning

confidence: 99%

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Helios spacecraft data revisited: detection of cometary meteoroid trails by following in situ dust impacts

Krüger

Strub

Sommer

et al. 2020

A&A

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Context. Cometary meteoroid trails exist in the vicinity of comets, forming a fine structure of the interplanetary dust cloud. The trails consist predominantly of the largest cometary particles (with sizes of approximately 0.1 mm-1 cm), which are ejected at low speeds and remain very close to the comet orbit for several revolutions around the Sun. In the 1970s, two Helios spacecraft were launched towards the inner Solar System. The spacecraft were equipped with in situ dust sensors which measured the distribution of interplanetary dust in the inner Solar System for the first time. Recently, when re-analysing the Helios data, a clustering of seven impacts was found, detected by Helios in a very narrow region of space at a true anomaly angle of 135 ± 1 • , which the authors considered as potential cometary trail particles. However, at the time, this hypothesis could not be studied further. Aims. We re-analyse these candidate cometary trail particles in the Helios dust data to investigate the possibility that some or all of them indeed originate from cometary trails and we constrain their source comets. Methods. The Interplanetary Meteoroid Environment for eXploration (IMEX) dust streams in space model is a new and recently published universal model for cometary meteoroid streams in the inner Solar System. We use IMEX to study the traverses of cometary trails made by Helios. Results. During ten revolutions around the Sun, the Helios spacecraft intersected 13 cometary trails. For the majority of these traverses the predicted dust fluxes are very low. In the narrow region of space where Helios detected the candidate dust particles, the spacecraft repeatedly traversed the trails of comets 45P/Honda-Mrkos-Pajdušáková and 72P/Denning-Fujikawa with relatively high predicted dust fluxes. The analysis of the detection times and particle impact directions shows that four detected particles are compatible with an origin from these two comets. By combining measurements and simulations we find a dust spatial density in these trails of approximately 10 −8-10 −7 m −3. Conclusions. The identification of potential cometary trail particles in the Helios data greatly benefited from the clustering of trail traverses in a rather narrow region of space. The in situ detection and analysis of meteoroid trail particles which can be traced back to their source bodies by spacecraft-based dust analysers provides a new opportunity for remote compositional analysis of comets and asteroids without the necessity to fly a spacecraft to or even land on those celestial bodies. This provides new science opportunities for future missions like DESTINY + (Demonstration and Experiment of Space Technology for INterplanetary voYage with Phaethon fLyby and dUst Science), Europa Clipper, and the Interstellar Mapping and Acceleration Probe.

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Section: Imex Cometary Trails Modelmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Helios spacecraft data revisited: detection of cometary meteoroid trails by following in situ dust impacts

Krüger

Strub

Sommer

et al. 2020

A&A

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“…To test if the cauliflower-like structures may be a result of spallation and compaction of micrometeoroid bombardment into a highly porous and low strength rock, we assume that a hypervelocity impact into a highly porous material can be assumed to be 10 times larger than the impactor (Tedeschi et al 1995), thus a 250 µm particle would cause a 2.5 mm impact feature. Based on the Interplanetary Meteoroid Environment Model 2 by Soja et al (2019), the mean impact speed of a 250 µm dust particle in a near Earth orbit is approximately 16 km/s and has an flux of ∼8•10 −9 −2 −1 . Assuming that the rock imaged by MasCam has been exposed at the surface since Ryugu's formation (approximately 10 7 years ago (Arakawa et al 2020)), this flux results in about 1.6•10 5 accumulated impacts in the imaged 25 cm × 25 cm scene or 250 impacts per cm 2 .…”

Section: Roughness Caused By Micrometeoroid Impactsmentioning

confidence: 99%

Surface roughness of asteroid (162173) Ryugu and comet 67P/Churyumov–Gerasimenko inferred fromin situobservations

Otto

Matz

Schröder

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Alteration processes on asteroid and comet surfaces, such as thermal fracturing, (micrometeorite) impacts or volatile outgassing, are complex mechanisms that form diverse surface morphologies and roughness on various scales. These mechanisms and their interaction may differ on the surfaces of different bodies. Asteroid Ryugu and comet 67P/Churyumov-Gerasimenko, both, have been visited by landers which imaged the surfaces in high spatial resolution. We investigate the surface morphology and roughness of Ryugu and 67P/Churyumov-Gerasimenko based on high resolution in situ images of 0.2 mm and 0.8 mm pixel resolution over an approximately 25 cm and 80 cm wide scene, respectively. To maintain comparability and reproducibility, we introduce a method to extract surface roughness descriptors (fractal dimension, Hurst exponent, joint roughness coefficient, root mean square slope, hemispherical crater density, small scale roughness parameter and Hapke mean slope angle) from in situ planetary images illuminated by LEDs. We validate our method and choose adequate parameters for an analysis of the roughness of the surfaces. We also derive the roughness descriptors from 3-dimensional shape models of Ryugu and orbiter camera images and show that the higher spatially resolved images results in a higher roughness. We find that 67P/Churyumov-Gerasimenko is up to 6% rougher than Ryugu depending on the descriptor used and attribute this difference to the different intrinsic properties of the materials imaged and the erosive processes altering them. On 67P/Churyumov-Gerasimenko sublimation appears to be the main cause for roughness, while on Ryugu micrometeoroid bombardment as well as thermal fatigue and solar weathering may play a significant role in shaping the surface.

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“…Collisional lifetimes derived by Grün et al (1985) indicate that the particle size range studied here (D 100 µm) should not be particularly collisionally dominated. These lifetimes, however, have been the subject of much debate due to an incompatibility with the distribution of orbital elements of dust grains in the millimetre size range observed by ground-based meteor radars (Nesvorný et al 2010(Nesvorný et al , 2011Pokorný et al 2014;Soja et al 2019). The derived particle dynamics require considerable evolution under PR drag and thus collisional lifetimes up to orders of magnitude higher than those derived by Grün et al (1985).…”

Section: Discussionmentioning

confidence: 99%

Effects of neighbouring planets on the formation of resonant dust rings in the inner Solar System

Sommer

Yano

Srama

2020

A&A

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Context. Findings by the Helios and STEREO mission have indicated the presence of a resonant circumsolar ring of dust associated with Venus. Attempts to model this phenomenon as an analogue to the resonant ring of Earth -as a result of migrating dust trapped in external mean-motion resonances (MMRs) -have so far been unable to reproduce the observed dust feature. Other theories of origin have recently been put forward. However, the reason for the low trapping efficiency of Venus's external MMRs remains unclear. Aims. Here we look into the nature of the dust trapping resonant phenomena that arise from the multi-planet configuration of the inner Solar System, aiming to add to the existent understanding of resonant dust rings in single planet systems. Methods. We numerically modelled resonant dust features associated with the inner planets and specifically looked into the dependency of these structures and the trapping efficiency of particular resonances on the configuration of planets. Results. Besides Mercury showing no resonant interaction with the migrating dust cloud, we find Venus, Earth, and Mars to considerably interfere with each other's resonances, influencing their ability to form circumsolar rings. We find that the single most important reason for the weakness of Venus's external MMR ring is the perturbing influence of its outer neighbour -Earth. In addition, we find Mercury and Mars to produce crescent-shaped density features, caused by a directed apsidal precession occurring in particles traversing their orbital region.

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IMEM2: a meteoroid environment model for the inner solar system

Cited by 28 publications

References 57 publications

Helios spacecraft data revisited: detection of cometary meteoroid trails by following in situ dust impacts

Helios spacecraft data revisited: detection of cometary meteoroid trails by following in situ dust impacts

Surface roughness of asteroid (162173) Ryugu and comet 67P/Churyumov–Gerasimenko inferred fromin situobservations

Effects of neighbouring planets on the formation of resonant dust rings in the inner Solar System

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