Evolution of NEO rotation rates due to close encounters with earth and venus (Articolo in rivista)

Type
Label
  • Evolution of NEO rotation rates due to close encounters with earth and venus (Articolo in rivista) (literal)
Anno
  • 2004-01-01T00:00:00+01:00 (literal)
Http://www.cnr.it/ontology/cnr/pubblicazioni.owl#doi
  • 10.1016/j.icarus.2004.03.017 (literal)
Alternative label
  • Scheeres D.J.; Marzari F.; Rossi A. (2004)
    Evolution of NEO rotation rates due to close encounters with earth and venus
    in Icarus (N.Y.N.Y. 1962)
    (literal)
Http://www.cnr.it/ontology/cnr/pubblicazioni.owl#autori
  • Scheeres D.J.; Marzari F.; Rossi A. (literal)
Pagina inizio
  • 312 (literal)
Pagina fine
  • 323 (literal)
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  • 170 (literal)
Rivista
Http://www.cnr.it/ontology/cnr/pubblicazioni.owl#note
  • Elsevier, 2004. (literal)
Note
  • ISI Web of Science (WOS) (literal)
Http://www.cnr.it/ontology/cnr/pubblicazioni.owl#affiliazioni
  • Department of Aerospace Engineering, The University of Michigan, Ann Arbor, MI 48109-2140, USA; Dipartimento di Fisica, Università di Padova, 35131 Padova, Italy; ISTI-CNR, CNR-Area della Ricerca di Pisa, 56124 Pisa, Italy (literal)
Titolo
  • Evolution of NEO rotation rates due to close encounters with earth and venus (literal)
Abstract
  • In this paper we study the statistical effect of planetary flybys on the rotation rates and states of Near Earth Objects (NEOs). Our approach combines numerical and analytical methods within a Monte Carlo model that simulates the evolution of the NEO spin rates. We take as input for the simulation a source distribution of spin states and evolve it to find their steady state distribution. In performing this evolution we track the changes in the spin rate and state distribution for the different components of the NEO population. We show that the cumulative effect of planetary encounters is to spin up the overall population of NEOs. This spin up effect holds on average only, and particular members of the population may experience an overall decrease in rotation rate. This effect is clearly seen across all components of the NEO population and is significant both statistically and physically. For initially slow rotators the spin up effect is strong, lowering the mean rotation period by 32%. For faster rotating populations the effect is less, lowering the spin period by 15% for the intermediate case, 6% for fast rotating rubble piles, and 8% for fast rotating monoliths. Physically, the spin up effect pushes 1% of the fast rotating rubble pile NEOs over the disruption limit, while 6% of these bodies experience a sub-disruption event that could modify their physical structure. For monolithic NEOs, the spin up effect is self-limiting, reaching a minimum spin period of 1.1 hours, with a strong cut-off between 2-3 hours. This has two implications. First, it may not be necessary to invoke the rubble pile hypothesis to recover a cut-off in spin period. Second, it shows that planetary flybys cannot account for the extremely rapid rotation rates of some small NEOs, implying that their rotation periods are probably due to collisional processes in the main belt. We also tested a different balance between the effects of Earth and Venus by treating the Aten sub-class of asteroids separately. Due to increased interactions with the p (literal)
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