Dust Grains in the Comae and Tails of Sungrazing Comets: Modeling of Their Mineralogical and Morphological Properties

Kimura, Hiroshi; Mann, Ingrid; Biesecker, D. A.; Jeßberger, E. K.

doi:10.1006/icar.2002.6940

Cited by 91 publications

(126 citation statements)

References 88 publications

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“…The longer egress tails, in this picture, would naturally correspond to dust tails that trail the fragment due to radiation pressure (see, e.g., Rappaport et al 2014). However, as was shown in Sanchis-Ojeda et al (2015), dust tails can also lead the emitting object if the radiation pressure is low enough or if the dust particles have a small scattering cross section (see, e.g., Kimura et al 2002). Finally, in regard to the results in Fig.…”

Section: Discussionmentioning

confidence: 71%

Drifting asteroid fragments around WD 1145+017

Rappaport

Gary²,

Kaye

et al. 2016

Mon. Not. R. Astron. Soc.

135

155

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We have obtained extensive photometric observations of the polluted white dwarf WD 1145+017 which has been reported to be transited by at least one, and perhaps several, large asteroids with dust emission. Observation sessions on 37 nights spanning 2015 November to 2016 January with small to modest size telescopes have detected 237 significant dips in flux. Periodograms reveal a significant periodicity of 4.5004 hours consistent with the dominant ("A") period detected with K2. The folded light curve shows an hour-long depression in flux with a mean depth of nearly 10%. This depression is, in turn, comprised of a series of shorter and sometimes deeper dips which would be unresolvable with K2. We also find numerous dips in flux at other orbital phases. Nearly all of the dips associated with this activity appear to drift systematically in phase with respect to the "A" period by about 2.5 minutes per day with a dispersion of ∼0.5 min/d, corresponding to a mean drift period of 4.4928 hours. We are able to track ∼15 discrete drifting features. The "B"-"F" periods found with K2 are not detected, but we would not necessarily have expected to see them. We explain the drifting motion as due to smaller fragmented bodies that break off from the asteroid and go into a slightly smaller orbit. In this interpretation, we can use the drift rate to determine the mass of the asteroid, which we find to be ≈ 10 23 grams, or about 1/10th the mass of Ceres.

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Section: Discussionmentioning

confidence: 71%

Drifting asteroid fragments around WD 1145+017

Rappaport

Gary²,

Kaye

et al. 2016

Mon. Not. R. Astron. Soc.

135

155

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“…Gail & Sedlmayr (1999) have shown that compounds such as enstatite and forsterite (typically Mg-rich pyroxene and olivine) have their stability limits under equilibrium conditions in the temperature region between 800 K and 1100 K. These temperatures should be reached for distances R to the Sun below 0.3 AU (see e.g. Kimura et al 2002;Mann et al 2004). The degradation of silicate minerals in this region could explain the observed variation in the polarization.…”

Section: Discussionmentioning

confidence: 99%

Inferring the interplanetary dust properties

Lasue¹,

Levasseur-Regourd²,

Fray

et al. 2007

A&A

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Context. Since in situ studies and interplanetary dust collections only provide a spatially limited amount of information about the interplanetary dust properties, it is of major importance to complete these studies with properties inferred from remote observations of scattered and emitted light, with interpretation through simulations. Aims. Physical properties of the interplanetary dust in the near-ecliptic symmetry surface, such as the local polarization, temperature, and composition, together with their heliocentric variations, may be derived from scattered and emitted light observations, giving clues to the respective contribution of the particle sources. Methods. A model of light scattering by a cloud of solid particles constituted by spheroidal grains and aggregates thereof is used to interpret the local light-scattering data. Equilibrium temperature of the same particles allows us to interpret the temperature heliocentric variations. Results. A good fit of the local polarization phase curve, P α , near 1.5 AU from the Sun is obtained for a mixture of silicates and more absorbing organic material (≈40% in mass) and for a realistic size distribution typical of the interplanetary dust in the 0.2 µm to 200 µm size range. The contribution of dust particles of cometary origin is at least 20% in mass. The same size distribution of particles gives a dependence of the temperature with the solar distance, R, in R −0.45 that is different than the typical black body behavior. The heliocentric dependence of P α=90 • is interpreted as a progressive disappearance of solid organic (such as HCN polymers or amorphous carbon) towards the Sun. Conclusions.

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“…Most of the sungrazers dim below detection at around 7 R s and may be completely destroyed by 3 R s , as a handful of UVCS observations suggest (e.g., Bemborad et al 2005). Furthermore, Kimura et al (2002) have suggested that sungrazers should exhibit a second brightness peak at 4-6 R s due to the sublimation of crystalline and amorphous pyroxenes. WISPR will have the sensitivity, spatial coverage, and cadence to resolve these issues albeit based on a smaller sample of comets than LASCO or SECCHI due to the SPP orbit and operational restrictions.…”

Section: Science Question 9: 'What Is the Nature Of Dust-plasma Intermentioning

confidence: 99%

The Wide-Field Imager for Solar Probe Plus (WISPR)

et al. 2015

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mission designed to orbit as close as 7 million km (9.86 solar radii) from Sun center. WISPR employs a 95 • radial by 58 • transverse field of view to image the fine-scale structure of the solar corona, derive the 3D structure of the large-scale corona, and determine whether a dust-free zone exists near the Sun. WISPR is the smallest heliospheric imager to date yet it comprises two nested wide-field telescopes with large-format (2 K × 2 K) APS CMOS detectors to optimize the performance for their respective fields of view and to minimize the risk of dust damage, which may be considerable close to the Sun. The WISPR electronics are very flexible allowing the collection of individual images at cadences up to 1 second at perihelion or the summing of multiple images to increase the signal-to-noise when the spacecraft is further from the Sun. The dependency of the Thomson scattering emission of the corona on the imaging geometry dictates that WISPR will be very sensitive to the emission from plasma close to the spacecraft in contrast to the situation for imaging from Earth orbit. WISPR will be the first 'local' imager providing a crucial link between the large-scale corona and the in-situ measurements.

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Dust Grains in the Comae and Tails of Sungrazing Comets: Modeling of Their Mineralogical and Morphological Properties

Cited by 91 publications

References 88 publications

Drifting asteroid fragments around WD 1145+017

Drifting asteroid fragments around WD 1145+017

Inferring the interplanetary dust properties

The Wide-Field Imager for Solar Probe Plus (WISPR)

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