The long-term dynamical evolution of objects with extremely high area-to-mass ratios released in synchronous and semi-synchronous orbits was simulated with a numerical propagator including all the relevant perturbations. In fact, as suggested by optical observations in the geosynchronous regime and orbital analysis of breakup fragments in low Earth orbit, artificial debris characterized by area-to-mass ratios hundreds or thousands of times greater than those of intact satellites or rocket bodies might be produced much more frequently than previously supposed. The results obtained show that even objects with area-to-mass ratios of tens of m2/kg may remain in space for several decades, or more, with very wide eccentricity excursions and orbit pole precessions, but maintaining a mean motion close to the original one, either synchronous or semi-synchronous.

Long term dynamical evolution of high area to mass ratio debris released into high earth orbits

Anselmo L
2009

Abstract

The long-term dynamical evolution of objects with extremely high area-to-mass ratios released in synchronous and semi-synchronous orbits was simulated with a numerical propagator including all the relevant perturbations. In fact, as suggested by optical observations in the geosynchronous regime and orbital analysis of breakup fragments in low Earth orbit, artificial debris characterized by area-to-mass ratios hundreds or thousands of times greater than those of intact satellites or rocket bodies might be produced much more frequently than previously supposed. The results obtained show that even objects with area-to-mass ratios of tens of m2/kg may remain in space for several decades, or more, with very wide eccentricity excursions and orbit pole precessions, but maintaining a mean motion close to the original one, either synchronous or semi-synchronous.
2009
Istituto di Scienza e Tecnologie dell'Informazione "Alessandro Faedo" - ISTI
High area-to-mass ratio orbital debris
Semi-synchronous orbits
Geosynchronous orbits
Orbit stability
Long-term dynamical evolution
Solar radiation pressure
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/20.500.14243/58572
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