A Solar System dust ring with the Earth as its shepherd

Jackson, A. A.; Zook, H. A.

doi:10.1038/337629a0

Cited by 126 publications

(65 citation statements)

References 18 publications

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“…While the large-scale clumps on the outskirts of the solar system still escape observational detection, there is one, so far the only, case where scenario I is observed at work: the asymmetric resonant ring of asteroidal dust around the Earth orbit. Predicted by Jackson & Zook (1989), it was identified in IRAS (Dermott et al 1994) and COBE/DIRBE data (Reach et al 1995). Search of a similar ring around the Mars orbit was not successful, however (Kuchner et al 2000).…”

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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“…Dermott et al (1994) also carried out orbital calculations for asteroidal dust particles with s = 6 µm and ρ s = 2.7 g/cm 3 (corresponding to β = 0.037) and empirically derived the relative probability of capture into and the average trapping time in p : (p + 1) MMRs outside the orbit of the Earth. Dermott et al (1994) made a model "image" of a circumsolar ring in the zodiacal dust cloud using these empirical data and showed that the leading-trailing brightness asymmetry observed by IRAS is caused by the circumsolar ring composed of asteroidal dust (see also Jackson & Zook 1989). However, Dermott et al (1994) carried out these simulations only for asteroidal particles with β = 0.037.…”

Section: Introductionmentioning

confidence: 99%

Size Dependence of Dust Distribution around the Earth Orbit

Ueda

Kobayashi

Takeuchi

et al. 2017

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In the Solar System, interplanetary dust particles (IDPs) originating mainly from asteroid collisions and cometary activities drift to the Earth orbit due to the Poynting-Robertson drag. We analyzed the thermal emission from IDPs that was observed by the first Japanese infrared astronomical satellite, AKARI.The observed surface brightness in the trailing direction of the Earth orbit is 3.7% greater than that in the leading direction in the 9 µm band and 3.0% in the 18 µm band. In order to reveal dust properties causing the leading-trailing surface brightness asymmetry, we numerically integrated orbits of the Sun, the Earth, and a dust particle as a restricted three-body problem including radiation from the Sun. The initial orbits of particles are determined according to the orbits of main-belt asteroids or Jupiter-family comets. The orbital trapping in mean motion resonances results in a significant leading-trailing asymmetry so that intermediate sized dust (∼ 10-100 µm) produces a greater asymmetry than the zodiacal light has. The leading-trailing surface brightness difference integrated over the size distribution of the asteroidal dust is obtained to be the values of 27.7% and 25.3% in the 9 µm and 18 µm bands, respectively. In contrast, the brightness difference for cometary dust is calculated as the values of 3.6% and 3.1% in the 9 µm and 18 µm bands, respectively, if the maximum dust radius is set to be s max = 3000 µm. Taking into account these values and their errors, we conclude that the contribution of asteroidal dust to the zodiacal infrared emission is less than ∼ 10%, while cometary dust of the order of 1 mm mainly accounts for the zodiacal light in infrared.

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“…Orbital motion of dust particles in the zones of mean-motion orbital resonances with a planet is intensively discussed since the paper by Jackson and Zook (1989) was published.…”

Section: Introductionmentioning

confidence: 99%

“…Besides important gravitational attraction of the Sun and the planet, moving usually in circular orbit, also the effect of solar electromagnetic radiation on the particle is considered. Standardly, dust particle is considered to be spherically symmetric and, correspondingly, the effect of solar electromagnetic radiation is considered in the form of the Poynting-Robertson (P-R) effect: e. g., Jackson and Zook (1989), Šidlichovský and Nesvorný (1994), Beaugé and Ferraz-Mello (1994), Marzari and Vanzani (1994), , , Liou and Zook (1997). Observations confirming the existence of dust ring around the Sun in resonant lock with the Earth are discussed in Brownlee (1994), Dermott et al (1994), Reach et al (1995).…”

Section: Introductionmentioning

confidence: 99%

Motion of dust in mean motion resonances with planets

Pástor

Klačka

Kómar

2009

Celest Mech Dyn Astr

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Abstract. Effect of stellar electromagnetic radiation on motion of spherical dust particle in mean-motion orbital resonances with a planet is investigated. Planar circular restricted three-body problem with the Poynting-Robertson (P-R) effect yields monotonous secular evolution of eccentricity when the particle is trapped in the resonance. Elliptically restricted three-body problem with the P-R effect enables nonmonotonous secular evolution of eccentricity and the evolution of eccentricity is qualitatively consistent with the published results for the complicated case of interaction of electromagnetic radiation with nonspherical dust grain. Thus, it is sufficient to allow either nonzero eccentricity of the planet or nonsphericity of the grain and the orbital evolutions in the resonances are qualitatively equal for the two cases. This holds both for exterior and interior mean-motion orbital resonances. Evolutions of longitude of pericenter in the planar circular and elliptical restricted three-body problems are shown. Our numerical integrations suggest that any analytic expression for secular time derivative of the particle's longitude of pericenter does not exist, if a dependence on semi-major axis, eccentricity and longitude of pericenter is considered (the P-R effect and mean-motion resonance with the planet in circular orbit is taken into account).Change of optical properties of the spherical grain with the heliocentric distance is also considered. The change of the optical properties: i) does not have any significant influence on secular evolution of eccentricity, ii) causes that the shift of pericenter is mainly in the same direction/orientation as the particle motion around the Sun. The statements hold both for circular and noncircular planetary orbits.

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A Solar System dust ring with the Earth as its shepherd

Cited by 126 publications

References 18 publications

On the nature of clumps in debris disks

On the nature of clumps in debris disks

Size Dependence of Dust Distribution around the Earth Orbit

Motion of dust in mean motion resonances with planets

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