Regular ArticleOrbital Evolution of Retrograde Interplanetary Dust Particles and Their Distribution in the Solar System
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Student Dust Counter: Status report at 38 AU
2019, IcarusCitation Excerpt :Dust is continually produced from EKBOs due to mutual collisions (Stern, 1996) and bombardment of interstellar and interplanetary dust (Yamamoto and Mukai, 1998; Poppe, 2015). Dust particles generated in the EKB slowly migrate towards the Sun due to Poynting-Robertson drag, and their fate is determined by possible close encounters with planets, trapping in mean motion orbital resonances (Liou et al., 1996; 1999; Moro-Martín and Malhotra, 2002; 2003), and grain-grain collisions (Kuchner and Stark, 2010) Recent models have detailed the sources, sinks, and transport of dust particles in the outer solar system allowing for direct comparisons with SDC observations (Vitense et al., 2012; 2014; Poppe, 2016).
Space weathering and the color-color diagram of Plutinos and Jupiter Trojans
2015, IcarusCitation Excerpt :To estimate the amount of dust particles that impact on a Jupiter-Trojan asteroid or on a Plutino we scale the estimated mass of dust that fall on the Earth. It is estimated to be between 20,000 tons and 40,000 tons of 1 mm – 1 μm dust particles per year (Liou et al., 1999). The model we are going to discuss, is based on many laboratory experiments that have been conducted in the last 10 years by the group at the Laboratorio di Astrofisica Sperimentale in Catania (LASP-Catania) (e.g. Strazzulla et al., 2005) and by other groups (see e.g., Sasaki et al., 2001; Loeffler et al., 2008, 2009).
Migration of small bodies and dust to near-Earth space
2006, Advances in Space ResearchCitation Excerpt :The spatial density of 1.4–10 μm particles obtained with Voyager 1 data was constant from 30 to 51 AU. Liou et al. (1999) and Liou and Zook (1999) concluded that dust grains released by Halley-type comets cannot account for this observed distribution, but trans-Neptunian dust particles can. Based on our runs, we made plots of distribution of spatial density ns (i.e., the number of particles per unit of volume) near ecliptic over distance R from the Sun (Fig. 1).
Impact-generated dust clouds around planetary satellites: Model versus Galileo data
2005, Planetary and Space ScienceCitation Excerpt :The first two classes of particles can be further subdivided into several populations with different sources and clearly discernible properties. IDPs are expected to comprise a classical population in prograde (low-eccentricity, low-inclination) orbits coming from short-period comets and the Edgeworth-Kuiper Belt; the “Oort cloud” population (Cuzzi and Durisen, 1990; Colwell and Horányi, 1996) which is thought to come from long-period comets and is characterized by highly eccentric, randomly inclined orbits; a population of IDPs in retrograde orbits supplied by comets in retrograde orbits (Liou et al., 1999). The planetary impactors in the Jovian case may include several populations as well.
The new ESA meteoroid model
2005, Advances in Space ResearchCitation Excerpt :By simulating the orbital dynamics of particles from comet Encke, Liou et al. (1995) demonstrated that the comets are necessary to account for the full thickness of the zodiacal cloud, with the dust from asteroids being confined close to the ecliptic plane. Liou et al. (1999) computed the trajectories of meteoroids of several sizes from comet Halley and its imaginary prograde clone. Cremonese et al. (1997) studied numerically the contributions of dust from comets Schwassmann-Wachmann 1 and Griegg-Skjellerup to the inner zodiacal cloud.