Synthesis of Observations

Staubach, P.; Grün, E.; Matney, Mark

doi:10.1007/978-3-642-56428-4_8

Cited by 14 publications

(14 citation statements)

References 33 publications

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“…We employ the model by Staubach et al [2001] which is primarily based on in situ data. The orbit of an IDP is characterized by its orbital elements (a, e, i, W, w), where a is the semimajor axis, e is the eccentricity, i is the inclination, W is the ecliptic longitude of the ascending node, and w is the argument of the perihelion.…”

Section: Spacecraft's Trajectory and Geometrymentioning

confidence: 99%

Interstellar dust flux measurements by the Galileo dust instrument between the orbits of Venus and Mars

et al. 2005

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[1] We present an analysis of the data obtained by the Galileo in situ dust instrument for interstellar dust (ISD). Between December 1989 and the end of 1993, three orbit segments were favorable for the detection of ISD at less than 3 AU heliocentric distance. After removing background events from the data sample, which were mostly due to interplanetary dust impactors, we infer that the flux of ISD grains between 0.7 AU and 3 AU is about 4 Â 10 À5 m À2 s À1 . This result is compatible with the ISD flux of 3 Â 10 À5 m À2 s À1 (grain size % 0.4 mm) derived from the Cassini measurements at about 1 AU. Using a new concept called ''ISD b spectroscopy,'' we are able to estimate at different locations in the inner solar system the ISD flux alteration resulting from the competing effects of radiation pressure and gravitation. In particular, we confirm results of previous Ulysses dust data analysis showing that radiation pressure prevents smaller ISD grains (radius smaller than % 0.3 mm) from reaching the innermost region of the solar system. Furthermore, our analysis shows the relevance of gravitational focusing in the dynamics of bigger ISD grains (micron-sized grains). The Galileo measurements were performed 10 years before the Cassini measurements. Thus the available ISD data now cover almost a full 11-year solar cycle. Nonetheless, the flux of ISD grains with radius bigger than 0.4 mm shows no significant temporal variation. This suggests that the dynamics of these ISD grains is not influenced much by the interaction with the time-dependent solar magnetic field.

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Section: Spacecraft's Trajectory and Geometrymentioning

confidence: 99%

Interstellar dust flux measurements by the Galileo dust instrument between the orbits of Venus and Mars

et al. 2005

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“…This model also takes no account of particle composition. All modelled and experimental data to date have used spherical iron particles as projectiles and these are not representative of real micrometeoroids and space debris, which have complex structures and much lower densities, typically 2000 kg m −3 for the smallest cometary dust particles (Kessler 1990) and 3500 kg m −3 for asteroidal dust particles (Staubach et al 2001).…”

Section: Propagation Of Particles In X-ray Telescopesmentioning

confidence: 99%

Meteoroid and space debris impacts in grazing-incidence telescopes

Wells

Abbey

Ambrosi

2008

A&A

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Context. Micrometeoroid or space debris impacts have been observed in the focal planes of the XMM-Newton and Swift-XRT (X-ray Telescope) X-ray observatories. These impacts have resulted in damage to, and in one case the failure of, focal-plane Charge-Coupled Device (CCDs) detectors. Aims. We aim to quantify the future risks of focal-plane impacts in present and future X-ray observatories.Methods. We present a simple model for the propagation of micrometeoroids and space debris particles into telescopes with grazingincidence X-ray optics, which is based on the results of previous investigations into grazing-incidence hypervelocity impacts by microscopic particles. We then calculate micrometeoroid and space debris fluxes using the Micrometeoroid and Space Debris Terrestrial Environment Reference model (MASTER2005). The risks of future focal-plane impact events in three present (Swift-XRT, XMM-Newton, and Chandra) and two future (SIMBOL-X and XEUS) X-ray observatories are then estimated on the basis of the calculated fluxes and the model for particle propagation.Results. The probabilities of at least one impact occurring in the Swift-XRT, XMM-Newton, and Chandra focal planes, in a one year period from the time of writing in November 2007 are calculated to be ∼5% and ∼50% and ∼3%. First-order predictions of the impact rates expected for the future SIMBOL-X and XEUS X-ray observatories yield probabilities for at least one focal-plane impact, during nominal 5-year missions, of more than 94% and 99%, respectively. Conclusions. The propagation of micrometeoroids and space debris particles into the focal planes of X-ray telescopes is highest for Wolter optics with the largest collecting areas and the lowest grazing angles. Telescopes in low-Earth orbits encounter enhanced particle fluxes compared with those in higher orbits and a pointing avoidance strategy for certain directions can reduce the risk of impacts. Future X-ray observatories, with large collecting areas and long focal lengths, may experience much higher impact rates on their focal-plane detectors than those currently in operation. This should be considered in the design and planning of future missions.

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“…10.4, the original naming conventions for the halo, inclined, and eccentric populations lost their meaning. Hence, and due to the integration of new measurement data from Ulysses and Galileo, Staubach re-fitted the probability densities, and renamed them as A, B, and C populations (Staubach et al, 2001). Fig.…”

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confidence: 99%

“…The integrals which need to be determined for the spatial density D in Eq. 10.5 are generally solved by means of numerical quadrature for discrete probability densities of the 3 phase space parameters r p , e and i, and of the mass m. (Divine, 1993;Staubach et al, 2001). The curves show cumulative fluxes F(> m) due to meteoroids of masses larger than m.…”

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confidence: 99%

“…With the auxiliary variables χ = arcsin(r p /r) and e χ = (1 − sin χ)/(1 + sin χ), the number density D of meteoroids with masses larger than m can be expressed by integrals over the three probability densities (Staubach et al, 2001). with H m representing the differential number of meteoroids in a bin dm, at mass m, divided by the number of meteoroids of mass m > 1 g. The velocity vector v = (v x , v y , v z ) of a meteoroid in the heliocentric coordinate system x, y, z can be derived as a function of the phase space parameters r p , e, and i (Staubach et al, 2001). For the same parameter set, 4 different orientations of the velocity vector must be considered: inbound or outbound, and towards the north or south of the ecliptic.…”

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Modeling of the Terrestrial Meteoroid Environment

Klinkrad¹,

Grün²

Springer Praxis Books

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During almost 50 years of space activities approximately 27,000 tons of man-made material re-entered into the Earth atmosphere at a mean rate of ∼600 tons per year. This compares with an estimated 40,000 tons of natural meteoroid material which reaches the Earth atmosphere each year. If this is so, why are meteoroids only dealt with at the end of this book? The answer lies in the size spectrum of meteoroids, which is dominated by particles with diameters of ∼200 µm and corresponding masses of ∼1.5 ×10 −5 g. The resulting risk to operational spacecraft is generally low as compared with space debris, in spite of much higher impact velocities of up to 72 km/s (corresponding to a heliocentric escape orbit of 42 km/s intercepted by the Earth orbit at 30 km/s). THE DIVINE-STAUBACH METEOROID MODELThe meteoroid environment of the Earth is comparatively well known from groundbased photographic and radar observations of meteors, from space-borne detector experiments, from retrieved space surfaces, from meteoritic material captured by high-flying airplanes, and from micro-craters on returned lunar rocks. In contrast with the highly dynamic space debris environment, the dominant part of the meteoroid environment can be assumed to be sporadic and invariant with time. There are, however, seasonally recurring meteoroid stream events, associated with material in cometary orbits, which can give noticeable contributions, particularly in the case of meteoroid storms. The topic of cosmic dust and meteoroid research has many interesting facets, and it deserves more attention than can be given in this brief summary. A comprehensive overview of the current state of research and its historic roots is provided in .During the Apollo Program, meteoroids were identified as a potential risk,

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Synthesis of Observations

Cited by 14 publications

References 33 publications

Interstellar dust flux measurements by the Galileo dust instrument between the orbits of Venus and Mars

Interstellar dust flux measurements by the Galileo dust instrument between the orbits of Venus and Mars

Meteoroid and space debris impacts in grazing-incidence telescopes

Modeling of the Terrestrial Meteoroid Environment

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