Asteroids pp 459-468 | Cite as

Asteroid Capture



The scenario where a celestial body threatens to impact the Earth is very popular and many solutions have been proposed to mitigate the associated risk. Some of them can be considered “soft” and consist in landing on or rendez-vous with the incoming asteroid several years in advance of the collision and then altering its trajectory by various means, such as painting it in order to alter its albedo and therefore the radiation pressure or by pushing it gently using a gravitational tractor (Lu and Love 2005). The mechanical device described below could also be used to change the trajectory. All these scenarios need a lot of time, even discounting mission preparation. If the incoming body is not a near-earth object but, for instance, a comet nucleus, more than ten years are likely to be necessary to reach it. Some “hard” solutions do not require a rendez-vous, but an interception, possibly with a large relative velocity. They can be implemented on a much shorter timeframe. Detonating a nuclear device could disperse the incoming body as the gravitational binding energy of an asteroid is surprisingly low. The difficulty might then be the timing: the explosion should take place before the impact but late enough to create a strong absorption of its energy (mainly X rays), which would turn a percentage of the mass of the asteroid into hot gases generating a shock wave that could disperse the asteroid and additionally creating a mean impulse which would alter the trajectory of the centre of gravity of the cloud of debris. In (Massonnet and Meyssignac 2006), a two step procedure is proposed where a smaller asteroid is first captured and “parked” on a L1-L2 Earth-Sun Lagrange orbit, and then sent into a trajectory impacting the incoming threat.


Discrete Element Method Final Mass Lagrange Point Halo Orbit Solar Sail 


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  1. Brophy, J., Culik, F., Friedman, L., et al.: Asteroid Retrieval Feasibility Study. Keck Institute for Space Studies, Pasadena (2012)Google Scholar
  2. Delbo, M., dell’Oro, A., Harris, A.W., Mottola, S., Mueller, M.: Thermal inertia of near-Earth asteroids and implications for the magnitude of the Yarkovsky effect. Icarus 190, 236–249 (2007)CrossRefGoogle Scholar
  3. Dyson, G.: Project Orion: The True Story of the Atomic Spaceship. Henry Holt and Company, New York (2002)Google Scholar
  4. Harris, A.W.: The Rotation Rates of Very Small Asteroids: Evidence for ’Rubble Pile’ Structure. In: Lunar and Planetary Institute Conference Abstracts, vol. 27, p. 493 (1996)Google Scholar
  5. Hill, D.: Trebuchets. Viator 4, 99–115 (1973)Google Scholar
  6. Holsapple, K.A.: Equilibrium Configurations of Solid Ellipsoidal Cohesionless Bodies. Icarus 154, 432–448 (2001)CrossRefGoogle Scholar
  7. Holsapple, K.A.: Equilibrium Figures of Spinning Bodies with Self-Gravity. Icarus 172, 272–303 (2004)CrossRefGoogle Scholar
  8. Holsapple, K.A.: Spin limits of Solar System bodies: From the small fast-rotators to 2003 EL61. Icarus 187, 500–509 (2007)CrossRefGoogle Scholar
  9. Lu, E.T., Love, S.G.: Gravitational tractor for towing asteroids. Nature 438, 177–178 (2005)CrossRefGoogle Scholar
  10. McAndrews, H., Baker, A., Bidault, C., Bond, R., Browning, D., Fearn, D., Jameson, P., Roux, J.-P., Sweet, D., Weston, M.: Future power systems for space exploration. ESA-Report 14565/NL/WK, QinetiQ (2003)Google Scholar
  11. Massonnet, D., Meyssignac, B.: A captured asteroid: Our David’s stone for shielding Earth and providing the cheapest extraterrestrial material. Acta Astronautica 59, 77–83 (2006)CrossRefGoogle Scholar
  12. Meyssignac, B.: Personal communication (2012)Google Scholar
  13. Mueller, M.: Surface Properties of Asteroids from Mid-Infrared Observations and Thermophysical. Ph.D. Thesis, Freie Universitat, Berlin (2007)Google Scholar
  14. Murdoch, N.: Modelisation of granular material dynamics at the surface of asteroids and under various gravitational conditions (Mars, the Moon). PhD Thesis, Planetary and Space Sciences Research Institute, The Open University and the Côte d’Azur Observatory, The University of Nice, Sophia Antipolis, France (2011)Google Scholar
  15. Murdoch, N., Michel, P., Richardson, D.C., Nordstrom, K., Berardi, C.R., Green, S.F., Losert, W.: Numerical simulations of granular dynamics II: Particle dynamics in a shaken granular material. Icarus 219(1), 231–335 (2012)CrossRefGoogle Scholar
  16. Richardson, D.C., Walsh, K.J., Murdoch, N., Michel, P.: Numerical simulations of granular dynamics I: hard sphere discrete element method and tests. Icarus 212, 427–437 (2011)CrossRefGoogle Scholar
  17. Schwartz, S., Richardson, D., Michel, P.: An implementation of the soft-sphere discrete element method in a high-performance parallel gravity tree-code. Granular Matter 14, 363–380 (2012)CrossRefGoogle Scholar

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© Springer-Verlag Berlin Heidelberg 2013

Authors and Affiliations

  1. 1.Centre National d’Etudes SpatialesParisFrance

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