CAOSP abstracts, Volume: 24, year: 1994
- Author(s): SVOREN, J.; NESLUSAN, L.; PORUBCAN, V.
- Journal: Contributions of the Astronomical Observatory Skalnate Pleso,
vol. 24, p. 5-18.
- Date: 08/1994
- Title: Applicability of meteor radiant determination methods depending on orbit type. II. Low-eccentric orbits
- Keyword(s): ASTEROIDS, METEOR STREAMS
- Pages: 5 -- 18
All known parent bodies of meteor showers belong to bodies moving in
high-eccentricity orbits (e => 0.5). Recently, asteroids in low-eccentricity
orbits (e < 0.5) approaching the Earth's orbit, were suggested as another
population of possible parent bodies of meteor streams. This paper deals with
the problem of calculation of meteor radiants connected with the bodies in
low-eccentricity orbits from the point of view of optimal results depending on
the method applied. The paper is a continuation of our previous analysis of
high-eccentricity orbits (Svoren, J., Neslusan, L., Porubcan, V.: 1993,
Contrib. Astron. Obs. Skalnate Pleso 23, 23). Some additional methods
resulting from mathematical modelling are presented and discussed together
with Porter's, Steel-Baggaley's and Hasegawa's methods. In order to be able
to compare how suitable the application of the individual radiant determination
methods is, it is necessary to determine the accuracy with which they
approximate real meteor orbits. To verify the accuracy with which the orbit of
a meteoroid with at least one node at 1 AU fits the original orbit of the
parent body, the Southworth-Hawkins D-criterion (Southworth, R.B.,
Hawkins, G.S.: 1963, Smithson. Contr. Astrophys. 7, 261) was applied.
D <= 0.1 indicates a very good fit of orbits, 0.1 < D <= 0.2 is considered for
a good fit and D > 0.2 means that the fit is rather poor and the change of
orbit unrealistic. The optimal method, i.e. the one which results in the
smallest D values for the population of low-eccentricity orbits, is that of
adjusting the orbit by varying both the eccentricity and perihelion distance.
A comparison of theoretical radiants obtained by various methods was
made for typical representatives from each group of the NEA (near-Earth
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