Dynamics of Interplanetary Dust

Belton, M. J. S.

doi:10.1126/science.151.3706.35

Cited by 52 publications

(24 citation statements)

References 14 publications

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“…Since the orbital eccentricities are close to zero for dust particles at small distances from the Sun, the radial drift of particles under the P-R effect will cause a radial number density variation proportional to 1/r . The interplay between the P-R drag and the radiation pressure force, increasing due to sublimation, may yield an enhancement of number density of the dust grains ("a dust ring") in the region just exterior to the dustfree zone (Belton 1966(Belton , 1967. Mukai et al (1974) calculated the dust number density for 1-µm-sized graphite grains initially on near-circular orbits to obtain an enhancement of the number density over the r −1 law by factors of 30 and 20 for e = 0 and e = 0.02, respectively.…”

Section: Radial Structurementioning

confidence: 99%

Dust Cloud near the Sun

Mann

Krivov

Kimura

2000

Icarus

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Section: Radial Structurementioning

confidence: 99%

Dust Cloud near the Sun

Mann

Krivov

Kimura

2000

Icarus

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“…On the basis of theoretical studies concerning the orbital evolution of circumsolar dust grains, Belton (1966Belton ( , 1967 has found that the orbital evolution of dust particles is stabilized at the edge of the dust-free zone. Subsequently, Mukai and Yamamoto (1979) have constructed a model of the near-solar dust rings consisting of spherical silicate and carbon grains to explain the observed infrared brightness.…”

Section: The Configuration Of the Dust Cloud Near The Sunmentioning

confidence: 99%

Brightness of the solar F-corona

Kimura

Mann

2014

Earth Planet Sp

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We discuss our present knowledge about the brightness of the solar F-corona in the wavelength range from the visible to the middle infrared. From the general trend of the observational data, the F-corona is regarded as the continuous extension of the zodiacal light at smaller elongation of the line of sight. A contribution of thermal emission from dust is indicated by the increasing F-coronal brightness in comparison to the solar spectrum towards longer wavelength. As compared with the F-coronal brightness, the polarization and color in the visible regime are not well determined due to the high sensitivity of these quantities to the observational accuracy. Aside from observational problems, our present interpretation of the F-coronal brightness is also limited due to ambiguities in the inversion of the line of sight integral. Nevertheless, the measurements and model calculations of the brightness can be used to deduce some physical properties of dust grains. We show that the hump of the near-infrared brightness at 4 solar radii, which was sometimes observed in the corona, is related rather to the physical properties of dust grains along the line of sight than to the existence of a dust ring as previously discussed. We also show that the appearance or disappearance of the near-infrared peak in the coronal brightness cannot be described in any periodic cycle for each wavelength range.

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“…An accumulation of interplanetary dust grains at their sublimation zone proposed by Belton (1966) is now known as a mechanism to form a dust ring. Refractory dust grains drift toward the Sun by the Poynting-Robertson drag (hereafter P-R drag) and sublime in the immediate vicinity of the Sun.…”

Section: Introductionmentioning

confidence: 99%

Dust ring formation due to sublimation of dust grains drifting radially inward by the Poynting–Robertson drag: An analytical model

Kobayashi

Watanabe

Kimura

et al. 2009

Icarus

107

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Dust particles exposed to the stellar radiation and wind drift radially inward by the Poynting-Robertson (P-R) drag and pile up at the zone where they begin to sublime substantially. The reason they pile up or form a ring is that their inward drifts due to the P-R drag are suppressed by stellar radiation pressure when the ratio of radiation pressure to stellar gravity on them increases during their sublimation phases. We present analytic solutions to the orbital and mass evolution of such subliming dust particles, and find their drift velocities at the pileup zone are almost independent of their initial semimajor axes and masses. We derive analytically an enhancement factor of the number density of the particles from their drift velocities at the outer edge of the sublimation zone.We show that the formula of the enhancement factor reproduces well numerical simulations in the previous studies. The enhancement factor for spherical dust particles of silicate and carbon extends from 3 to more than 20 at stellar luminosities L = 0.8-500L , where L is solar luminosity. Although the enhancement factor for fluffy dust particles is smaller than that for spherical particles, sublimating particles inevitably form a dust ring as long as their masses decrease faster than their surface areas during sublimation. The formulation is applicable to dust ring formation for arbitrary shape and material of dust in dust-debris disks as well as in the Solar System.-4 -

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Dynamics of Interplanetary Dust

Cited by 52 publications

References 14 publications

Dust Cloud near the Sun

Dust Cloud near the Sun

Brightness of the solar F-corona

Dust ring formation due to sublimation of dust grains drifting radially inward by the Poynting–Robertson drag: An analytical model

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