Radar Observations of Taurid Complex Meteor Showers in 2003: Activity and Mass Distribution

Pećina, P.; Porub–an, V.; Pecinová, D.; Tóth, Juraj

doi:10.1007/s11038-005-4504-8

Cited by 6 publications

(12 citation statements)

References 1 publication

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“…Another method employed to distinguish between underdense and overdense trails is via the duration of the specular trails. Underdense specular trails are shorter in duration (≤0.4 seconds) as compared to overdense trails (>0.4 seconds) [e.g., Pecina et al , 2004]. The underdense trails have a distinct amplitude and phase signature ‐ the Fresnel pattern ‐ due to the “unwinding of the trail” as it approaches the radar “t 0 ” point (the point of closest approach to the radar and the k (wave vector) ⟂ trajectory point).…”

Section: Introductionmentioning

confidence: 99%

Low‐altitude meteor trail echoes

Malhotra

Mathews

2009

Geophysical Research Letters

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We present here the first observations of a new type of meteor echo. These Low‐Altitude Trail Echoes (LATE), observed almost exclusively below 90 km altitude using the Jicamarca Research Observatory 50 MHz radar, exhibit very different features and characteristics from the other well studied and reported meteor trails ‐ the specular meteor trails and the Range Spread Trail Echoes. Some of these features include strong altitude dependence, low aspect sensitivity and no gap between the head echo and the trail. Perhaps most importantly, almost 80% of the head echoes below 85 km altitude in our data set exhibit LATE trails. The study of these echoes provides valuable insights into the role of diffusion and plasma instabilities in the formation and evolution of meteor trails.

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Section: Introductionmentioning

confidence: 99%

Low‐altitude meteor trail echoes

Malhotra

Mathews

2009

Geophysical Research Letters

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“…Radio measurements of the BTA and ZPE show similar variability in the showers' mass index 𝑠 (Pecina et al 2004;Porubčan et al 2007;Dewsnap & Campbell-Brown 2021). From observations of the showers between 2000 and 2005, Porubčan et al (2007) estimated that 𝑠 ranged from 1.98±0.04 and 2.28±0.21 for the ZPE, and from 2.10±0.02 to 2.37±0.09 for the BTA.…”

Section: Size Distributionmentioning

confidence: 86%

“…From observations of the showers between 2000 and 2005, Porubčan et al (2007) estimated that 𝑠 ranged from 1.98±0.04 and 2.28±0.21 for the ZPE, and from 2.10±0.02 to 2.37±0.09 for the BTA. In addition, observations of the ZPE in 2004 and 2005 in Ondrejov displayed evident hints of mass segregation, with the maximum of activity of faint radar meteors appearing two days prior to the maximum measured for overdense echoes (Pecina et al 2004;Porubčan et al 2007). Similar variation with mass was observed for the BTA and the STA, but not for the NTA (Pecina et al 2004).…”

Section: Size Distributionmentioning

confidence: 94%

“…All solar longitudes are J2000. References are As: Aspinall & Hawkins (1951), C: Cook (1973), S: computed from dates in Sekanina (1973) for observation year 1965, R: Roggemans (1989), Pe: Pecina et al (2004), Du: Dubietis & Arlt (2006), P: Porubčan et al (2007), De : Dewsnap & Campbell-Brown (2021), A: Arlt (2000). Uncertain times of maximum are given in parenthesis; in these cases the real maximum was probably missed because of bad observing conditions.…”

Section: Photographic and Video Observationsmentioning

confidence: 99%

“…Radio measurements of the BTA and ZPE between 2000 and 2005 were also performed using the Ondřejov backscatter meteor radar (Pecina et al 2004;Porubčan et al 2007) and the Budrio-Lecce-Modra (BLM) forward-scatter system (Porubčan et al 2007). The time of maximum activity of the ZPE and BTA was found to vary from year-to-year by a few days (cf.…”

Section: Previous Radar Observationsmentioning

confidence: 99%

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An observational synthesis of the Taurid meteor complex

Egal,

Brown,

Wiegert

et al. 2022

Preprint

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We provide an overview of the observational properties of the four major Taurid showers, namely the Northern and Southern Taurids (#017 NTA and #002 STA), the 𝛽 Taurids (#173 BTA) and the 𝜁 Perseids (#172 ZPE). Analysing more than two decades of meteor observations from visual, optical and radar measurements we present the Taurids average activity, annual variations in strength, radiant drift and orbital variations as a function of solar longitude and particle size. The Taurid showers are detected over several weeks in the spring and autumn, but their annual activity level is generally low (less than 15 visual meteors per hour). We find the STA to be predominant in autumn, while its twin the ZPE dominates over the BTA in spring. Due to their long duration, the position of each shower's radiant and orbital elements are variable with time. Optical measurements have previously recorded enhanced STA activity and increased fireball rates caused by the return of a swarm of meteoroids trapped in the 7:2 mean motion resonance with Jupiter. However, we find no presence of the swarm in radar data, suggesting that small meteoroids are removed from the resonance faster than fireballproducing meteoroids. We also find the STA to be enriched in smaller particles early in their activity period. The differences we identify in our analysis between the showers at different particle sizes provide strong observational constraints to future dynamical modelling of the Taurid Meteoroid Complex.

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Radar Meteors Range Distribution and Some Parameters of Meteoroids: Application to ζ Perseids and β Taurids Showers

Pecinová¹,

Pećina²

Modern Meteor Science an Interdisciplinary View

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Radar Observations of Taurid Complex Meteor Showers in 2003: Activity and Mass Distribution

Cited by 6 publications

References 1 publication

Low‐altitude meteor trail echoes

Low‐altitude meteor trail echoes

An observational synthesis of the Taurid meteor complex

Radar Meteors Range Distribution and Some Parameters of Meteoroids: Application to ζ Perseids and β Taurids Showers

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