The size dependence of sublimation rates for interplanetary ice particles

Patashnick, H.; Rupprecht, Georg

doi:10.1086/181783

Cited by 32 publications

(12 citation statements)

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“…The model parameters including the maximum modeled grain sizes are summarized in Table 1. Two different models of grains were used: pure icy grains (Patashnick and Ruprecht, 1975) and ''dirty'' icy grains (Lien, 1990) -the principal difference being the amount of silicate material contained in the grain (pure = nil dirty = 10%). While pure icy grains absorb in the UV and in the IR, ''dirty'' icy grains absorb well in the visible.…”

Section: Direct Simulation Monte Carlo (Dsmc) Kinetic Model Of Cometamentioning

confidence: 99%

Understanding measured water rotational temperatures and column densities in the very innermost coma of Comet 73P/Schwassmann–Wachmann 3 B

Fougere

Combi

Tenishev

et al. 2012

Icarus

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Section: Direct Simulation Monte Carlo (Dsmc) Kinetic Model Of Cometamentioning

confidence: 99%

Understanding measured water rotational temperatures and column densities in the very innermost coma of Comet 73P/Schwassmann–Wachmann 3 B

Fougere

Combi

Tenishev

et al. 2012

Icarus

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“…The sublimation rate at the surface of a comet depends on its temperature distribution, spin rate, conductivity, and composition, with estimated values of order Z 16 ∼ 10-30 (Whipple and Huenber 1976). Small ice particles are colder than a large slab and hence sublimate more slowly, with Z 16 ∼ 0.2 for R = 0.1 cm and Z 16 ∼ 7 × 10 −4 for R = 0.01 cm (Patashnick and Rupprecht 1975). Heterogeneous particles may however be warmer, with Z 16 ∼ 10 3 for R = 0.5 cm (Mukai 1986).…”

Section: Sublimation and Survivalmentioning

confidence: 99%

Distribution and properties of fragments and debris from the split Comet 73P/Schwassmann-Wachmann 3 as revealed by Spitzer Space Telescope

Reach

Vaubaillon

Kelley

et al. 2009

Icarus

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we used the IRAC and MIPS instruments on the Spitzer Space Telescope to study the infrared emission from the ensemble of fragments, meteoroids, and dust tails in the more than 3 degree wide 73P/Schwassmann-Wachmann 3 debris field.We also investigated contemporaneous ground based and HST observations. In 2006 May, 55 fragments were detected in the Spitzer image. The wide spread of fragments along the comet's orbit indicates they were formed from the 1995 splitting event. While the number of major fragments in the Spitzer image is similar to that seen from the ground by optical observers, the correspondence between the fragments with optical astrometry and those seen in the Spitzer images cannot be readily established, due either to strong non-gravitational terms, astrometric uncertainties, or transience of the fragments outgassing. The Spitzer data resolve the structure of the dust comae at a resolution of ∼ 1000 km, and they reveal the infrared emission due to large (mm to cm size) particles in a continuous dust trail that closely follows the projected orbit. We detect fluorescence from outflowing CO 2 gas from the largest fragments (B and C), and we measure the CO 2 :H 2 O proportion (1:10 and 1:20, respectively). We use three dimensionless parameters to explain dynamics of the solid particles: the rocket parameter α is the reaction force from day-side sublimation divided by solar gravity, the radiation pressure parameter β is the force due to solar radiation pressure divided by solar gravity, and the ejection velocity parameter ν is the particle ejection speed divided by the orbital speed of the comet at the time of ejection. The major fragments have ν > α > β and are dominated by the kinetic energy imparted to them by the fragmentation process. The small, ephemeral fragments seen by HST in the tails of the major fragments have α > ν > β and are dominated by rocket forces (until they become devolatilized). The meteoroids along the projected orbit seen by Spitzer have β ∼ ν ≫ α and are dominated by radiation pressure and ejection velocity, though both influences are much less than gravity.Dust in the fragments' tails has β ≫ (ν + α) and is dominated by radiation pressure.

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“…Many researchers have examined the sublimation rates of water ice as a function of particle size and purity, with pure water ice having a minimum in sublimation rate at ∼10-20 µm size particles (Patashnick and Rupprecht, 1975;Hanner, 1981;Mukai, 1986;Lichtenegger and Komle, 1991). However, the presence of even minute amounts of impurities in the ice increases the absorptivity (and thus the temperature) and significantly decreases the lifetime of particles (Patashnick and Rupprecht, 1975). Lifetimes on the order of hours, as observed in these look-back data, require either sub-micron pure water ice grains or dirty water ice grains >700 µm (Mukai, 1986).…”

Section: Look-back Datamentioning

confidence: 99%

“…It is unlikely that such superfine particles embedded in an ice mantle would completely segregate as a result of an impact. In addition, the small particle size observed in the interior of Tempel 1 also suggests that the size distribution of ice in comae is primary in origin, rather than a net result of the sublimation history of ice grains in the coma (e.g., Patashnick and Rupprecht, 1975).…”

Section: Implications Of the Physical Structure Of The Ejected Water Icementioning

confidence: 99%

The distribution of water ice in the interior of Comet Tempel 1

Sunshine

Groussin

Schultz

et al. 2007

Icarus

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The Deep Impact flyby spacecraft includes a 1.05 to 4.8 µm infrared (IR) spectrometer. Although ice was not observed on the surface in the impact region, strong absorptions near 3 µm due to water ice are detected in IR measurements of the ejecta from the impact event. Absorptions from water ice occur throughout the IR dataset beginning three seconds after impact through the end of observations, ∼45 min after impact. Spatially and temporally resolved IR spectra of the ejecta are analyzed in conjunction with laboratory impact experiments. The results imply an internal stratigraphy for Tempel 1 consisting of devolatilized materials transitioning to unaltered components at a depth of approximately one meter. At greater depths, which are thermally isolated from the surface, water ice is present. Up to depths of 10 to 20 m, the maximum depths excavated by the impact, these pristine materials consist of very fine grained (∼1 ± 1 µm) water ice particles, which are free from refractory impurities.

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The size dependence of sublimation rates for interplanetary ice particles

Cited by 32 publications

References 0 publications

Understanding measured water rotational temperatures and column densities in the very innermost coma of Comet 73P/Schwassmann–Wachmann 3 B

Understanding measured water rotational temperatures and column densities in the very innermost coma of Comet 73P/Schwassmann–Wachmann 3 B

Distribution and properties of fragments and debris from the split Comet 73P/Schwassmann-Wachmann 3 as revealed by Spitzer Space Telescope

The distribution of water ice in the interior of Comet Tempel 1

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