  Simulations of structure formation in the standard cold dark matter
cosmological model quantify the dark matter halos of galaxies. Taking into
account dynamical friction between the dark matter halos, we investigate the
past orbital dynamical evolution of the Magellanic Clouds in the presence of
the Galaxy. Our calculations are based on a three-body model of rigid
Navarro-Frenk-White profiles for the dark matter halos, but were verified in a
previous publication by comparison to high-resolution N-body simulations of
live self-consistent systems. Under the requirement that the LMC and SMC had an
encounter within 20 kpc between 1 and 4 Gyr ago, in order to allow the
development of the Magellanic Stream, and using the latest astrometric data,
the dynamical evolution of the MW/LMC/SMC system is calculated backwards in
time. With the employment of the genetic algorithm and a Markov-Chain
Monte-Carlo method, the present state of this system is unlikely with a
probability of <10^{-9} (6 sigma complement), because solutions found do not
fit into the error bars for the observed plane-of-sky velocity components of
the Magellanic Clouds. This implies that orbital solutions that assume dark
matter halos according to cosmological structure formation theory to exist
around the Magellanic Clouds and the Milky Way are not possible with a
confidence of more than 6 sigma
