Some Features of Evolution of Meteor Streams

Abstract

It is shown that a number of features of meteor showers such as the correlation of orbital semimajor axes and longitudes of the ascending nodes with meteor magnitudes, the restriction of visibility periods and the displacement of maximum activity dates is explained by the joint influence of planetary perturbations, the Poynting-Robertson effect and its corpuscular analogue, light pressure and ejection velocities of different mass meteoroids from cometary nuclei.

The meteor-shower complex of 96P/Machholz revisited

“…However, Babadzhanov & Obrubov (1993) reported the shower named α-Cetids with the observed parameters vaguely consistent with those predicted for filament 4 (Tables 1 and 2), except for a larger declination and geocentric velocity. Specifically, they gave q = 0.06−0.18 AU, e = 0.89−0.99,…”

“…Only the observation of radio meteors is not affected by this circumstance. Babadzhanov & Obrubov (1993) reported the shower named κ-Velids with the declination of the mean radiant δ g = −52 • more or less corresponding to a that is predicted for filament 6. The κ-Velid right ascension (149 • ), perihelion distance (0.97 AU), argument of perihelion (18 • ), and inclination (77 • ) also roughly agree with the values for filament 6 (Tables 1 and 2), but the observed mean eccentricity of the κ-Velids is only 0.51, i.e.…”

“…A more detailed analysis of this structure reveals four separated subareas. Three of these, separated from the fourth by the declination of −50.5 • , have very similar characteristics, therefore can be regarded as a unique (southern) In this context, it is perhaps worth mentioning a possible relationship of the southern substructure with the shower of Carinids reported by Babadzhanov & Obrubov (1993). These authors characterized the Carinids with q = 0.98 AU, e = 0.61,…”

“…Both branches of δ-Aquarids, daytime Arietids, and one weak shower (identified by Babadzhanov & Obrubov (1993) with the α-Cetids) constitute the ecliptical substructure of the complex. The Quadrantids and another shower with the radiant situated deeply in the southern sky, so almost not observed until now, constitute the toroidal substructure of the 96P complex.…”

“…5, plot (d), we can see an excursion of some radiants toward a higher declination. Babadzhanov & Obrubov (1993) assigned this more or less smooth continuation of Quadrantids to another shower: Ursids. We can confirm that the predicted argument of perihelion of high-declination Quadrantids is recognizable higher (consistent with the range given by Babadzhanov & Obrubov for the Ursids) than that of common Quadrantids.…”