Collisional balance of the meteoritic complex

Grün, E.; Zook, H. A.; Fechtig, H.; Giese, R. H.

doi:10.1016/0019-1035(85)90121-6

Cited by 942 publications

(832 citation statements)

References 38 publications

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“…The cumulative¯ux of Leonid meteoroids, for example, with masses e10 À5 g, at the time of maximum activity, during non-storm returns is H10 À12 meteoroids/m 2 /s. The cumulative¯ux of Leonid meteoroids during non-storm years is, therefore, some four orders of magnitude smaller than that from sporadic meteoroids with masses e10 À5 g [3]. While the¯ux of sporadic meteoroids may dominate that of the annual streams, this is not to say that spacecraft cannot be hit and damaged by stream meteoroids.…”

Section: Meteoroid Stream¯uxesmentioning

confidence: 95%

“…It is now a well-established observation that the annual meteoroid streams do not typically contribute in any signi®cant manner to the meteoroid¯ux experienced by Earth-orbiting spacecraft [36,3]. The cumulative¯ux of Leonid meteoroids, for example, with masses e10 À5 g, at the time of maximum activity, during non-storm returns is H10 À12 meteoroids/m 2 /s.…”

Section: Meteoroid Stream¯uxesmentioning

confidence: 99%

“…Cumulative¯uxes at maximum for the main annual meteor showers. The time axis is in solar longitude and the limiting mass is 10 À5 g. The¯ux is calculated according to the data in [14] and the sporadic¯ux is taken from [3]. is either based upon the observed radar cross-section, when known, or is assumed to be that of a sphere with a diameter equal to the average spacecraft dimensions.…”

Section: Satellites On Orbit 1964±1969mentioning

confidence: 99%

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Satellite impact probabilities: annual showers and the 1965 and 1966 Leonid storms

Beech

Jehn

Brown³

et al. 1999

Acta Astronautica

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AbstractÐThe stream meteoroid impact probability for space platforms is reviewed and found to be very low under normal circumstances. While the literature contains numerous accounts of spacecraft apparently su ering damage and/or interference during meteoroid stream encounters, we ®nd that there is, in fact, very little evidence to support such claims. This conclusion may not be valid, however, during meteor storms, when the¯ux of visual meteors can increase by factors in excess of 10 3 to 10 4 of that from the sporadic background. Special attention is directed towards the Leonid meteor storms of 1965 and 1966Ðthe only meteor storms since the dawn of the space age. The space platform impact probabilities during the 1966 storm were small but none negligible, being of order 1% for an exposed surface area of 2 m 2 at a limiting meteoroid mass of 10 À7 g (and assuming a stream mass index s = 2.0). The circumstances surrounding the possible encounters of the Pegasus II and III, and Mariner 4 spacecraft with Leonid stream meteoroids are discussed in some detail. While the 1966 Leonid meteor storm is the strongest on record (in the sense of the highest visual meteor rates) no apparent meteoroid in¯icted damage to a spacecraft can be unambiguously linked to it. This result is mostly a consequence of the small number and small size of spacecraft in Earth-orbit at the time of the 1966 storm. #

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Section: Meteoroid Stream¯uxesmentioning

confidence: 95%

Section: Meteoroid Stream¯uxesmentioning

confidence: 99%

Section: Satellites On Orbit 1964±1969mentioning

confidence: 99%

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Satellite impact probabilities: annual showers and the 1965 and 1966 Leonid storms

Beech

Jehn

Brown³

et al. 1999

Acta Astronautica

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“…Leinert and Grün, 1990) which contribute to the zodiacal brightness. The size distribution of interplanetary dust at 1 AU has been determined from lunar micro-craters and spacecraft data (Grün et al, 1985). From these observations it has been concluded that maximum scattering cross-section lies in the size range from 10 to 100 μπι and hence it is this size range which contributes most to the zodiacal light.…”

Section: Introductionmentioning

confidence: 97%

Dust Measurements in the Outer Solar System

Grün¹

1994

Symp. - Int. Astron. Union

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Abstract. In-situ measurements of micrometeoroids provide information on the spatial distribution of interplanetary dust and its dynamical properties. Pioneers 10 and 11, Galileo and Ulysses spaceprobes took measurements of interplanetary dust from 0.7 to 18 AU distance from the sun. Distinctly different populations of dust particles exist in the inner and outer solar system. In the inner solar system, out to about 3 AU, zodiacal dust particles are recognized by their scattered light, their thermal emission and by in-situ detection from spaceprobes. These particles orbit the sun on low inclination (i < 30°) and moderate eccentricity (e < 0.6) orbits. Their spatial density falls off with approximately the inverse of the solar distance. Dust particles on high inclination or even retrograde trajectories dominate the dust population outside about 3 AU. The dust detector onboard the Ulysses spaceprobe identified interstellar dust sweeping through the outer solar system on hyperbolic trajectories. Within about 2 AU from Jupiter Ulysses discovered periodic streams of dust particles originating from within the jovian system.

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“…These particles have large ratio of Q/m (Q is the charge of the dust particle and m is the mass of the dust particle). The collisions among the dust particles are important for particles of radii larger than hundred of micrometres, approximately (Grün et al 1985;Dermott et al 2001). The motion of micron-sized dust particles in the inner part of the Solar system is influenced beside the gravitation mainly by solar electromagnetic radiation and solar wind.…”

Section: Introductionmentioning

confidence: 99%

Positions of equilibrium points for dust particles in the circular restricted three-body problem with radiation

Pástor¹

2014

Monthly Notices of the Royal Astronomical Society

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For a body with negligible mass moving in the gravitational field of a star and one planet in a circular orbit (the circular restricted three-body problem) five equilibrium points exist and are known as the Lagrangian points. The positions of the Lagrangian points are not valid for dust particles because in the derivation of the Lagrangian points is assumed that no other forces beside the gravitation act on the body with negligible mass. Here we determined positions of the equilibrium points for the dust particles in the circular restricted three-body problem with radiation. The equilibrium points are located on curves connecting the Lagrangian points in the circular restricted threebody problem. The equilibrium points for Jupiter are distributed in large interval of heliocentric distances due to its large mass. The equilibrium points for the Earth explain a cloud of dust particles trailing the Earth observed with the Spitzer Space Telescope. The dust particles moving in the equilibrium points are distributed in interplanetary space according to their properties.

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Collisional balance of the meteoritic complex

Cited by 942 publications

References 38 publications

Satellite impact probabilities: annual showers and the 1965 and 1966 Leonid storms

Satellite impact probabilities: annual showers and the 1965 and 1966 Leonid storms

Dust Measurements in the Outer Solar System

Positions of equilibrium points for dust particles in the circular restricted three-body problem with radiation

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