An observational synthesis of the Taurid meteor complex
| العنوان: | An observational synthesis of the Taurid meteor complex |
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| المؤلفون: | A Egal, P G Brown, P Wiegert, Y Kipreos |
| المساهمون: | Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS) |
| المصدر: | Monthly Notices of the Royal Astronomical Society Monthly Notices of the Royal Astronomical Society, 2022, 512, pp.2318-2336. ⟨10.1093/mnras/stac397⟩ |
| بيانات النشر: | HAL CCSD, 2022. |
| سنة النشر: | 2022 |
| مصطلحات موضوعية: | Earth and Planetary Astrophysics (astro-ph.EP), comets: individual: 2P/Encke, Space and Planetary Science, [SDU]Sciences of the Universe [physics], minor planets, FOS: Physical sciences, Astronomy and Astrophysics, meteors, meteoroids, meteorites, asteroids: general, Astrophysics - Earth and Planetary Astrophysics |
| الوصف: | 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 Beta Taurids (#173 BTA) and the Zeta 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 fireball-producing 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. Accepted for publication in MNRAS (Acceptation date: 2022 February 10) |
| اللغة: | English |
| تدمد: | 0035-8711 1365-2966 |
| DOI: | 10.1093/mnras/stac397⟩ |
| URL الوصول: | https://explore.openaire.eu/search/publication?articleId=doi_dedup___::c7143c681c6ded73b0512a887c6235e4 https://hal-insu.archives-ouvertes.fr/insu-03718981/document |
| Rights: | OPEN |
| رقم الانضمام: | edsair.doi.dedup.....c7143c681c6ded73b0512a887c6235e4 |
| قاعدة البيانات: | OpenAIRE |
| تدمد: | 00358711 13652966 |
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| DOI: | 10.1093/mnras/stac397⟩ |