The penetration limit of thin films

Pailer, N.; Grün, E.

doi:10.1016/0032-0633(80)90021-5

Cited by 70 publications

(10 citation statements)

References 5 publications

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“…This hypothesis has been strongly indicated by crater residues on the Solar Max mission by Laurance and Brownlee (1986). However, it is shown that the choice of penetration formula referring those data to particulate mass (Pailer and Griin 1980) is at variance with other calibration data. The raw data of Laurance and Brownlee compare excellently with LDEF data; it is argued therefore that their data do not indicate a dominance of space debris below 10" 9 g. It could yet be found to be significant, and correspond to the excess flux seen on the East penetrations below approximately 25 ^im.…”

Section: Discussionmentioning

confidence: 99%

Particulate Detection in the Near Earth Space Environment Aboard the Long Duration Exposure Facility Ldef: Cosmic or Terrestrial?

McDonnell

Sullivan

Stevenson

et al. 1991

International Astronomical Union Colloquium

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Examination of surfaces exposed for more than five and a half years, from detectors with unique attitude stabilisation relative to the orbital velocity vector, offers scope for examining definitively the sources of hypervelocity space particulates. Surfaces reveal discrete crater morphologies, crater size distributions and incident flux distributions. Discrete crater studies will later also reveal the chemistry of residues which can, especially via the capture cell principle, lead to elemental analysis of micron dimensioned particles.First analyses of the flux data from the thin foil perforation experiments (MAP) involve a study of the statistics of the forward (ram) direction, the rear (trailing) direction and the space pointing direction. Modelling of the dynamics of geocentrically bound and unbound orbits yields evidence that the characteristics of the particles, and hence probably their source, change over the particle size range measured by the experiment. Smaller particles (< 1 μm diameter) have lower velocities which could include geocentrically bound particulates, whereas the larger particles (5-10 μm diameter) can be identified with “cosmic” particles of interplanetary or interstellar origin.

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Section: Discussionmentioning

confidence: 99%

Particulate Detection in the Near Earth Space Environment Aboard the Long Duration Exposure Facility Ldef: Cosmic or Terrestrial?

McDonnell

Sullivan

Stevenson

et al. 1991

International Astronomical Union Colloquium

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“…ii) It is clear from the study of Carey et al (this volume) that, in the case of the perforation limit for particles with p = 1 g/cm-5 impacting aluminium foil, the Pailer and Griin (1980) equation gives the highest d/f or, in other terms, systematically favors low densities, iii) After correcting for the difference in sensitivity between the ecliptic and the south sensor, the excess of impacts reduces to ^ 1.4; a simple inspection of the experimental results of Pailer and Griin (1980) shows that this reduction of sensitivity may well be accounted for by particles having densities between 1.25 and 7.8 g/cm 3 .…”

Section: The Helios Datamentioning

confidence: 98%

“…the density of impacting grains and concluded that 30 % of interplanetary dust particles have densities below 1 g/cm 3 . This analysis calls however for several remarks, i) The relevant calibrations performed by Pailer and Griin (1980) cover only the following ranges: 1.25 -7.85 g/cm 3 for the projectile density, 10-13 -io-!0 g for the mass and 1.4 -13 km/sec for the velocity. The range of velocities is probably too low, but more important, no experimantal results are avaible for p < 1.25 g/cm 3 ; henceforth, the interpretation of the Helios data is based on extrapolations.…”

Section: The Helios Datamentioning

confidence: 99%

Some Remarks on the Density of Interplanetary Dust Grains

Lamy

1985

International Astronomical Union Colloquium

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The relevance of the bulk density as a physical parameter characterizing interplanetary dust grains is discussed. The various measurements which lead to a determination of this parameter are reviewed. The specific case of the collected interplanetary dust grains is considered.The bulk density of interplanetary dust grains has been and is still a matter of controversy. This quantity cannot, in general, be directly measured; it is used to relate the mass and the size of a grain. This duality stems from physics itself as there are interactions sensitive to the mass (e.g., gravitational forces) while others are sensitive to the size or the cross-section (e.g., light scattering, radiation pressure, gas and plasma interactions). The measuring technics of the grains reflect this duality as, for instance, impact sensors are generally sensitive to the kinetic energy and thus to the mass, while optical sensors are sensitive to the cross-section. One sees that the density is not strictly speaking the relevant parameter, but what is needed is a relationship between mass and average cross-section.

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“…The only explanation of this observation is that the cover foil of the ecliptic sensor prevented a number of particles to be registered. An experimental investigation of the cover foil [13] showed that low density dust grains are not able to penetrate the foil. The relevant result [12] was the discovery that 2 types of particles orbit the sun: those of "normal" densities (between 3 and 8 g/cm3) on orbits with low eccentricities (g<0.6), and those of "low" densities ( rg 1 g/cm3) on orbits with high eccentricities (e>0.6).…”

Section: Properties Of Halley Dust Particlesmentioning

confidence: 98%

Dust in the Solar System

Fechtig¹

1989

Zeitschrift Für Naturforschung A

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Dedicated to Heinrich Wanke on the occasion of his 60 th birthday Properties of cometary dust particles are better known since the space missions to Comet Halley. Their properties (densities, atomic composition) are compared with relevant observations from lunar microcraters and in-situ experiments. At 1 AU in the eliptic, 2/3 of the dust grains are normal density particles, presumably of asteroidal origin and irregularly shaped, while the remaining 1/3 are low density particles, presumably of cometary origin, but due to solar irradiation in a processed state (corresponding to "Brownlee"-particles). Beyond the asteroidal belt only black cometary dust grains are observed which have recently been released from comet nuclei orbiting on highly eccentric trajectories.

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The penetration limit of thin films

Cited by 70 publications

References 5 publications

Particulate Detection in the Near Earth Space Environment Aboard the Long Duration Exposure Facility Ldef: Cosmic or Terrestrial?

Particulate Detection in the Near Earth Space Environment Aboard the Long Duration Exposure Facility Ldef: Cosmic or Terrestrial?

Some Remarks on the Density of Interplanetary Dust Grains

Dust in the Solar System

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