Looking Before We Leap: Recent Results From An Ongoing Quantitative Investigation Of Asteroid And Comet Impact Hazard Mitigation.

Details Looking Before We Leap: Recent Results From An Ongoing Quantitative Investigation Of Asteroid And Comet Impact Hazard Mitigation. Looking Before We Leap: Recent Results From An Ongoing Quantitative Investigation Of Asteroid And Comet Impact Hazard Mitigation.

Oct 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010dps....42.6007p&link_type=abstract

American Astronomical Society, DPS meeting #42, #60.07; Bulletin of the American Astronomical Society, Vol. 42, p.1087

Astronomy and Astrophysics

Astronomy

Scientific paper

The asteroid and comet impact hazard is now part of public consciousness, as demonstrated by movies, Super Bowl commercials, and popular news stories. However, there is a popular misconception that hazard mitigation is a solved problem. Many people think, `we'll just nuke it.’ There are, however, significant scientific questions remaining in the hazard mitigation problem. Before we can say with certainty that an explosive yield Y at height of burst h will produce a momentum change in or dispersion of a potentially hazardous object (PHO), we need to quantify how and where energy is deposited into the rubble pile or conglomerate that may make up the PHO. We then need to understand how shock waves propagate through the system, what causes them to disrupt, and how long gravitationally bound fragments take to recombine.
Here we present numerical models of energy deposition from an energy source into various materials that are known PHO constituents, and rigid body dynamics models of the recombination of disrupted objects. In the energy deposition models, we explore the effects of porosity and standoff distance as well as that of composition. In the dynamical models, we explore the effects of fragment size and velocity distributions on the time it takes for gravitationally bound fragments to recombine. Initial models indicate that this recombination time is relatively short, as little as 24 hours for a 1 km sized PHO composed of 1000 meter-scale self-gravitating fragments with an initial velocity field of v/r = 0.001 1/s.

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