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Causes and Consequences of the Existence of Nanodust in Interplanetary Space

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Nanodust in the Solar System: Discoveries and Interpretations

Part of the book series: Astrophysics and Space Science Library ((ASSL,volume 385))

Abstract

Nanodust is observed in the solar system in situ from spacecraft when the particles impact onto the detectors with high speed. Nanodust is now observed with the STEREO spacecraft in interplanetary space near 1AU for more than 3 years and it is plausible to assume that this nanodust is a component of the interplanetary dust cloud of the solar system. The total mass flux observed in the nanodust is a small fraction of the mass that is destroyed by mutual collisions inside 1AU, although the collision models have large uncertainties. Further studies are needed in order to understand the exact processes by which the nanodust forms in interplanetary space. Measuring its composition and mass distribution will help to understand the dust cloud inside 1AU and the formation of nanodust during hypervelocity collisions.

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Notes

  1. 1.

    This is the model of dust flux vs. mass at 1 AU suggested by Grün et al. (1985) which will be further discussed in Sect. 3.3 and Sect. 4.

  2. 2.

    Meteoroids are larger solid particles that cause meteor phenomena when entering the atmosphere.

  3. 3.

    An additional component is the interstellar dust entering the solar system (cf. Mann, 2010), which we do not consider here.

  4. 4.

    The calculated flux in the 1–5 nm size range (radii) for the particular set of parameters used is 0.9 m − 2s − 1 and not 150 m  − 2s − 1 as given in Czechowski and Mann (2010).

  5. 5.

    As a caveat to the considerations of Poynting–Robertson lifetimes, we point out that those are not only influenced by the radiation pressure force, but also by a drag force that is caused by the momentum transfer from the solar wind particles that hit the dust and this also applies to the nanodust (Minato et al., 2004).

  6. 6.

    This distribution of geometric cross section is derived from the flux assuming dust relative velocities of 20 km/s. Since the small particles have larger velocities, their number densities are overestimated when applying this model.

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Acknowledgements

This work was partly supported by the Belgium Solar Terrestrial Center of Excellence and the Polish Ministry of Science (grant No N203 4159 33). Parts of this chapter were prepared while IM stayed as Visiting Astronomer at LESIA, CNRS, Observatoire de Paris Meudon and as Visiting Professor at Universite Pierre et Marie Curie in Paris and this support is greatly acknowledged. This work was initiated and partly carried out with support from the International Space Science Institute (ISSI) in the framework of an International Team entitled “Nano Dust in the Solar System: Formation, Interactions, and Detections.”

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Authors and Affiliations

  1. Belgium Institute for Space Aeronomie, 3 Avenue Circulaire, 1180, Brussels, Belgium

    Ingrid Mann

  2. Laboratoire d’Etudes Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, Universite Pierre et Marie Curie, Universite de Paris Diderot, CNRS, Meudon, France

    Ingrid Mann

  3. EISCAT Scientific Association, 812, SE-981 28, Kiruna, Sweden

    Ingrid Mann

  4. Space Research Centre, Polish Academy of Sciences, Bartycka 18A, 00-716, Warsaw, Poland

    Andrzej Czechowski

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  1. , EISCAT Scientific Association, Head of Projects, Rymdcampus 1, Kiruna, 981 92, Sweden

    Ingrid Mann

  2. , Observatoire de Paris, LESIA, Place Jules Janssen 5, Meudon Cedex, 92195, France

    Nicole Meyer-Vernet

  3. , Polish Academy of Sciences, Space Research Centre, Bartycka 18 A, Warsaw, 00716, Poland

    Andrzej Czechowski

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Mann, I., Czechowski, A. (2012). Causes and Consequences of the Existence of Nanodust in Interplanetary Space. In: Mann, I., Meyer-Vernet, N., Czechowski, A. (eds) Nanodust in the Solar System: Discoveries and Interpretations. Astrophysics and Space Science Library, vol 385. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-642-27543-2_10

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