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Selection effects in the discovery of NEAs

Published online by Cambridge University Press:  05 March 2015

G. B. Valsecchi
Affiliation:
IAPS-INAF, Roma, Italy IFAC-CNR, Sesto Fiorentino, Italy
G. D'Abramo
Affiliation:
SpaceDyS, Navacchio, Italy
A. Boattini
Affiliation:
LPL, University of Arizona, USA
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To highlight discovery selection effects, we consider four NEA subpopulations:

  1. (a) “Taurid asteroids”, the Apollos with orbits similar to those of 2P/Encke and of the Taurid meteoroid complex;

  2. (b) Atens, to which we add the Inner Earth Objects;

  3. (c) non-Taurid Apollos;

  4. (d) Amors.

The “Taurid asteroids“ are identified by Asher et al. (1993) with a reduced version of the D-criterion (Southworth and Hawkins 1963), involving only a, e and i:
\begin{displaymath} D=\sqrt{\left(\frac{a-2.1}{3}\right)^2+(e-0.82)^2+\left(2\sin{\frac{i-4^\circ}{2}}\right)^2}\leq0.25. \end{displaymath}
It turns out that the distribution of the longitudes of perihelion ϖ of NEAs with D<0.25 is significantly non-random, due to the existence of two groups whose apse lines are approximately aligned with those of 2P/Encke and of (2212) Hephaistos.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2015 

References

Asher, D. J., Clube, S. V. M., & Steel, D. I. 1993, MNRAS 264, 93Google Scholar
Kresák, Ľ. & Klačka, J. 1989, Icarus 78, 287CrossRefGoogle Scholar
Southworth, R. B. & Hawkins, G. S. 1963, Smithson. Contr. Astrophys. 7, 261Google Scholar
Valsecchi, G. B., Morbidelli, A., Gonczi, R., Farinella, P., Froeschlé, Ch., & Froeschlé, Cl. 1995, Icarus 118, 169CrossRefGoogle Scholar