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|Title:||Multi-instrumental observations of the 2014 Ursid meteor outburst|
Trigo-Rodríguez, J. M.
Madiedo, J. M.
Williams, I. P.
Morillas, L. G.
|Publisher:||Oxford University Press|
|Citation:||Multi-instrumental observations of the 2014 Ursid meteor outburst / M. Moreno-Ibáñez, J. M. Trigo-Rodríguez, J. M. Madiedo, et al. — DOI 10.1093/mnras/stx592 // Monthly Notices of the Royal Astronomical Society. — 2017. — Vol. 468. — Iss. 2. — P. 2206-2213.|
|Abstract:||The Ursid meteor shower is an annual shower that usually shows little activity. However, its Zenith hourly rate sometimes increases, usually either when its parent comet, 8P/Tuttle, is close to its perihelion or its aphelion. Outbursts when the comet is away from perihelion are not common and outbursts when the comet is close to aphelion are extremely rare. The most likely explanation offered to date is based on the orbital mean motion resonances. The study of the aphelion outburst of 2000 December provided a means of testing that hypothesis. A new aphelion outburst was predicted for 2014 December. The SPanish Meteor Network, in collaboration with the French Fireball Recovery and InterPlanetary Observation Network, set up a campaign to monitor this outburst and eventually retrieve orbital data that expand and confirm previous preliminary results and predictions. Despite unfavourable weather conditions over the south of Europe over the relevant time period, precise trajectories from multistation meteor data recorded over Spain were obtained, as well as orbital and radiant information for four Ursid meteors. The membership of these four meteors to the expected dust trails that were to provoke the outburst is discussed, and we characterize the origin of the outburst in the dust trail produced by the comet in the year AD 1392. © 2017 The Authors.|
|Appears in Collections:||Научные публикации, проиндексированные в SCOPUS и WoS CC|
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