Kuiper Belt Dust Grains as a Source of Interplanetary Dust Particles

Liou, J.‐C.; Zook, H. A.; Dermott, S. F.

doi:10.1006/icar.1996.0220

Cited by 98 publications

(89 citation statements)

References 28 publications

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“…If there is a planet in the disk, the particles reach locations of exterior mean-motion resonances (MMRs) with the planet and get trapped, yielding characteristic density patterns. Liou et al (1996) and Liou & Zook (1999) applied this idea to the solar system. By modeling perturbations induced by jovian planets on the Edgeworth-Kuiper Belt dust disk, they found efficient resonant trapping of dust by Neptune (which produces arcs of dust co-orbital with the planet) and efficient ejection of dust out of the solar system by Jupiter and Saturn.…”

Section: Statement Of the Problemmentioning

confidence: 99%

On the nature of clumps in debris disks

Krivov¹,

Queck²,

Löhne³

et al. 2006

A&A

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The azimuthal substructure observed in some debris disks, as exemplified by Eridani, is usually attributed to resonances with embedded planets. In a standard scenario, the Poynting-Robertson force, possibly enhanced by the stellar wind drag, is responsible for the delivery of dust from outer regions of the disk to locations of external mean-motion planetary resonances; the captured particles then create characteristic "clumps". Alternatively, it has been suggested that the observed features in systems like Eri may stem from populations of planetesimals that have been captured in resonances with the planet, such as Plutinos and Trojans in the solar system. A large fraction of dust produced by these bodies would stay locked in the same resonance, creating the dusty clumps. To investigate both scenarios and their applicability limits for a wide range of stars, planets, disk densities, and planetesimal families we construct simple analytic models for both scenarios. In particular, we show that the first scenario works for disks with the pole-on optical depths below about ∼10 −4 −10 −5 . Above this optical depth level, the first scenario will generate a narrow resonant ring with a hardly visible azimuthal structure, rather than clumps. It is slightly more efficient for more luminous/massive stars, more massive planets, and planets with smaller orbital radii, but all these dependencies are weak. The efficiency of the second scenario is proportional to the mass of the resonant planetesimal family, as example, a family with a total mass of ∼0.01 to 0.1 Earth masses could be sufficient to account for the clumps of Eridani. The brightness of the clumps produced by the second scenario increases with the decreasing luminosity of the star, increasing planetary mass, and decreasing orbital radius of the planet. All these dependencies are much stronger than in the first scenario. Models of the second scenario are quantitatively more uncertain than those of the first one, because they are very sensitive to poorly known properties of the collisional grinding process.

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Section: Statement Of the Problemmentioning

confidence: 99%

On the nature of clumps in debris disks

Krivov¹,

Queck²,

Löhne³

et al. 2006

A&A

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show abstract

“…Particles of this size are continuously being lost in the system by Poynting-Robertson (PR) drag and momentum exchange with the solar wind that causes them to spiral into the Sun (Burns, Lamy, & Soter 1979). Sources of dust particles required to maintain the cloud include comets Cremonese et al 1997) and collisions between larger bodies in the asteroid (Mann, Grü n, & Wilck 1996) or Kuiper belt (Liou, Zook, & Dermott 1996). By calculating the lifetime of the particles in the main ZD cloud we calculate the required rate of dust injection and compare it to the different dust sources.…”

Section: Introductionmentioning

confidence: 99%

The Zodiacal Emission Spectrum as Determined byCOBEand Its Implications

Fixsen

Dwek

2002

ApJ

100

120

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We combine observations from the DIRBE and FIRAS instruments on the COBE satellite to derive an annually averaged spectrum of the zodiacal cloud in the 10-1000 lm wavelength region. The spectrum exhibits a break at $150 lm that indicates a sharp break in the dust size distribution at a radius of about 30 lm. The spectrum can be fitted with a single blackbody with a À2 emissivity law beyond 150 lm and a temperature of 240 K. We also used a more realistic characterization of the cloud to fit the spectrum, including a distribution of dust temperatures representing different dust compositions and distances from the Sun, as well as a realistic representation of the spatial distribution of the dust. We show that amorphous carbon and silicate dust with respective temperatures of 280 and 274 K at 1 AU, and size distributions with a break at grain radii of 14 and 32 lm, can provide a good fit to the average zodiacal dust spectrum. The total mass of the zodiacal cloud is 2-11 Eg (Eg ¼ 10 18 g), depending on the grain composition.

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“…Because Voyager 1/2 mainly measured dust fluxes beyond Saturn's orbit, the effect of gravitational scattering on the flux measured by Voyager 1/2 may be much smaller than those by Pioneer 10/11. Although the ejection efficiency due to the gravitational scattering of Neptune is only 5%, that of Jupiter and Saturn is about 80% for dust with size as large as the Pioneer threshold (Liou et al, 1996). The model flux with Pioneer threshold from 14 to 4 AU gradually decreases with decreasing distance (Landgraf et al, 2002;Moro-Martín and Malhotra, 2003).…”

Section: Discussionmentioning

confidence: 98%

“…EKBOs are thought to produce dust particles through mutual collisions between EKBOs and/or erosion of EKBO surfaces by impacts of interstellar dust streaming into the solar system (Stern, 1996;Yamamoto and Mukai, 1998). Theoretical studies indicate that timescales for dust particles released from EKBOs to drift inward by the Poynting-Robertson (P-R) effect are shorter than their timescales against collisional destruction in the outer solar system if their radii are smaller than ∼10 µm (Liou et al, 1996). Therefore, EKB dust particles in orbit around the sun must drift inward by the P-R effect.…”

Section: Introductionmentioning

confidence: 99%

Ice sublimation of dust particles and their detection in the outer solar system

et al. 2010

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The flux of interplanetary dust beyond the Jupiter's orbit, which supposedly originates from Edgeworth-Kuiper belt, has been measured in situ by instruments on board Voyager and Pioneer spacecraft. The measured flux shows a nearly flat radial profile at 10-50 AU for Voyager and at 5-15 AU for Pioneer. Because the orbital evolution of dust particles controlled by radiation forces results in the flux that is inversely proportional to distance from the sun, dust particles detected by spacecraft should have suffered from other dynamical effects. We calculate model fluxes on the spacecraft taking into account the effect of ice sublimation as well as radiation forces on the orbital evolution of dust particles. Our results show that the radial profile of the model flux becomes relatively flat near the outer edge of the sublimation zone, where ice substantially sublimes. The expected location of the flat radial profile, which depends on the detection threshold of instruments, is 15-40 AU for Voyager and 5-20 AU for Pioneer. Because our model fluxes are comparable with the measured ones, we conclude that the flat radial profiles of the dust flux derived from in-situ dust impacts may be caused by ice sublimation.

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Kuiper Belt Dust Grains as a Source of Interplanetary Dust Particles

Cited by 98 publications

References 28 publications

On the nature of clumps in debris disks

On the nature of clumps in debris disks

The Zodiacal Emission Spectrum as Determined byCOBEand Its Implications

Ice sublimation of dust particles and their detection in the outer solar system

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