Meteoroid streams identification amongst 231 Southern hemisphere video meteors

Abstract

In this study, 231 video meteoroid orbits observed at the Southern hemisphere were searched for streams. Several searches have been made using three D‐criteria: DSH, DN and DV. The mutual D‐distances were processed by a cluster analysis algorithm based on the single neighbour linking technique. The values of the meteoroid association thresholds for groups of 2, 3, 4, … members were estimated by the statistical approach. In all three basic searches, about 29–33 per cent of the meteoroid sample turned out to belong to the stream component. The following streams have been detected: η Aquariids (ETA, #31), χ Capricornids (CCA, #420), May Microscopiids (MMI, #421), Northern and Southern Librids‐Luppids (NLL, #422; SLL, #423) and Northern and Southern May Ophiuchids (NOP, #149; SOP, #150). 12 η Aquariids were detected using each D‐function. Their mean orbital elements resemble the orbit of 1P/Haley; however, the mean semimajor axis and the activity time differ significantly from those determined by the other observers. 10 members of χ Capricornids and five members of May Microscopiids were found using the DN function only. For these streams, we did not find any counterparts among the streams listed in the IAU MDC. Our Librids‐Luppids and Ophiuchids form two separate complex groups which consist of 16 and 18 members, respectively. From a viewpoint of the cluster analysis technique, they are reliable significant structures. Our Ophiuchids are similar to the already known Northern and Southern May Ophiuchids. Near the mean radiant of Librids‐Luppids, we do not see any radiant of the known shower. Its possible counterpart, the Southern ω Scorpiids, has a radiant significantly shifted from our Librids‐Luppids. Thus, we consider Librids‐Luppids as a new stream or some new manifestation of the May Ophiuchids Complex. Also, this study has shown us that in case of complex structures, traditional procedures of meteor showers distinction are not sufficient tool to give unambiguous answers.

An orbital meteoroid stream survey using the Southern Argentina Agile MEteor Radar (SAAMER) based on a wavelet approach

“…The geocentric velocity of SZC from SAAMER-OS observations is approximately 10% lower than previously reported. We note that Jopek et al, 2010), however, the orbital elements for this shower are similar to those determined by Jopek et al (2010).…”

“…An effort to fill this gap utilizing optical and video observations has taken place in the past few years (Bland et al, 2012;Jopek et al, 2010;Molau and Kerr, 2014;Towner et al, 2015;Jenniskens et al, 2016a), focusing on larger fireballs but which are limited by weather and day/night cycles. We note that the Advanced Meteor Orbit Radar (AMOR) which operated in Christchurch, New Zealand during the 1990s, produced some 0.5 Megaorbits, but at such small particle sizes that only half a dozen of the strongest showers were visible in the resulting dataset (Galligan and Baggaley, 2004).…”

The Southern Argentina Agile Meteor Radar Orbital System (Saamer-Os): An Initial Sporadic Meteoroid Orbital Survey in the Southern Sky

“…The results show that SAAMER-OS is a system capable of providing significant statistical data of meteoroid orbital properties in the largely unexplored southern sky. An effort to fill the observational gap in this region utilizing optical and video observations has taken place in the past few years (Jopek et al 2010;Bland et al 2012;Molau & Kerr 2014;Towner et al 2015), which focus on larger fireballs and are limited by the weather conditions that optics suffer from. However, SAAMER-OS's survey introduces an important characteristicparticular of radar observations: the study of smaller and perhaps more dynamically evolved particles.…”

Association between meteor showers and asteroids using multivariate criteria

“…For the Taurids Complex the parent body is P/Encke (Whipple & El-Din Hamid 1952;Wiegert et al 2009). Several other parent bodies were also identified among the asteroids: 2003UV11, 2003WP21, 2004TG1, and 2005TF50 (Porubčan et al 2006Napier 2010;Jopek et al 2010).…”