Modeling the Sporadic Meteoroid Background Cloud

Dikarev, Valeri; Grün, E.; Baggaley, J.; Galligan, D. P.; Landgraf, M.; Jehn, R.

doi:10.1007/s11038-005-9017-y

Cited by 19 publications

(17 citation statements)

References 16 publications

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“…Surprisingly, 2P/Encke is the largest contributor with approximately 50% of the total, followed by 79P/duToit-Hartley. The asteroidal contribution in our model hovers around 4%, which is consistent with the results from the ESA model (Dikarev et al, 2004).…”

Section: The Low-velocity Flux At Earthsupporting

confidence: 91%

“…Eventually, perturbations accumulate and disperse the meteoroid stream, the original close orbital relationship between individual meteoroids becoming difficult to determine. allels in some ways that of the ESA meteoroid model (Landgraf et al, 2001;Dikarev et al, 2002Dikarev et al, , 2004. In fact, the ESA meteoroid model incorporates more observational constraints than our own, including many obtained by spacecraft, while we rely only on Earth-bound radar measurements.…”

Section: Introductionmentioning

confidence: 99%

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A dynamical model of the sporadic meteoroid complex

Wiegert

Vaubaillon

Campbell-Brown

2009

Icarus

134

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Section: The Low-velocity Flux At Earthsupporting

confidence: 91%

Section: Introductionmentioning

confidence: 99%

A dynamical model of the sporadic meteoroid complex

Wiegert

Vaubaillon

Campbell-Brown

2009

Icarus

134

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“…In order to predict the IDP fluxes on CDA between Jupiter and Saturn, we adopted the interplanetary meteoroid model by Divine [1993]. More recently developed models by Staubach et al [1997] and Dikarev et al [2005] were not based on any data acquired beyond Jupiter, and thus their numbers should be taken cautiously in the region under consideration. Figure 12 shows how drastically the frequent spacecraft orientation maneuvers affect the instrument sensitivity, the magnitude of variation reaches four orders of magnitude!…”

Section: Discussionmentioning

confidence: 99%

“…Asteroids and short‐period comets of the Jupiter family were found to be the major source of dust in the inner solar system [ Dermott et al , 1992; Liou et al , 1995]. Although their relative contribution is still a matter of debate, the large number of in situ measurements lead to quite a reliable modeling of the dust populations forming the zodiacal cloud inside 5 AU [ Divine , 1993; Staubach et al , 2001; Dikarev et al , 2005].…”

Section: Introductionmentioning

confidence: 99%

Cassini/Cosmic Dust Analyzer in situ dust measurements between Jupiter and Saturn

Altobelli¹,

Dikarev

Kempf

et al. 2007

J. Geophys. Res.

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[1] We report an analysis of the Cosmic Dust Analyzer data obtained during the interplanetary cruise of the Cassini spacecraft between Jupiter and Saturn. The data cover the time period between the Jupiter flyby and the Saturn orbit insertion. Seventeen dust particles on bound and unbound (hyperbolic) orbits were also detected, with sizes in the submicrometer to the micrometer range. Our measurements are compared with the Pioneer dust data obtained 30 years ago and model predictions. Particles on bound orbits have low eccentricities and low inclinations. Possible sources are short-period Jupiter family comets and circumsolar dust. The impactors on hyperbolic orbits were identified as being most likely interstellar dust (ISD) grains with a radius of %0.4 mm. The corresponding flux of %2 Â 10 À5 m À2 s À1 is in a very good agreement with the ISD flux measurements performed by the Ulysses spacecraft over the same time period.

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“…Inside and outside 1au the data are scarcer, although various models exist and are in use by NASA and ESA [e.g. [40][41][42][43][44]. The differential size distribution slope of particles larger than ∼100 µm was found to be steeper than −4, so that the mass density is dominated by particles ∼100 µm in radius.…”

Section: Size Distributionmentioning

confidence: 99%

Exozodiacal clouds: hot and warm dust around main sequence stars

Kral

Krivov

Defrère

et al. 2017

Astronomical Review

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A warm/hot dust component (at temperature >300 K) has been detected around ∼20% of A, F, G, K stars. This component is called 'exozodiacal dust' as it presents similarities with the zodiacal dust detected in our solar system, even though its physical properties and spatial distribution can be significantly different. Understanding the origin and evolution of this dust is of crucial importance, not only because its presence could hamper future detections of Earthlike planets in their habitable zones, but also because it can provide invaluable information about the inner regions of planetary systems. In this review, we present a detailed overview of the observational techniques used in the detection and characterisation of exozodiacal dust clouds ('exozodis') and the results they have yielded so far, in particular regarding the incidence rate of exozodis as a function of crucial parameters such as stellar type and age, or the presence of an outer cold debris disc. We also present the important constraints that have been obtained, on dust size distribution and spatial location, using state-of-the-art radiation transfer models on some of these systems. Finally, we investigate the crucial issue of how to explain the presence of exozodiacal dust around so many stars (regardless of their ages) despite the fact that such dust so close to its host star should disappear rapidly due to the coupled effect of collisions and stellar radiation forces. Several potential mechanisms have been proposed to solve this paradox and are reviewed in detail in this paper. The review finishes by presenting the future of this growing field.

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Modeling the Sporadic Meteoroid Background Cloud

Cited by 19 publications

References 16 publications

A dynamical model of the sporadic meteoroid complex

A dynamical model of the sporadic meteoroid complex

Cassini/Cosmic Dust Analyzer in situ dust measurements between Jupiter and Saturn

Exozodiacal clouds: hot and warm dust around main sequence stars

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