RT Journal Article
T1 Multi-instrumental observations of the 2014 Ursid meteor outburst
A1 Moreno Ibáñez, Manuel
A1 Madiedo Gil, José María
A1 Dupouy, Philippe
AB 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.
PB Oxford University Press
SN 0035-8711
SN 1365-2966
YR 2017
FD 2017
LK http://hdl.handle.net/10272/15563
UL http://hdl.handle.net/10272/15563
LA eng
NO Moreno-Ibáñez, M., Trigo-Rodríguez, J. M., Madiedo, J. M., Vaubaillon, J., Williams, I. P., Gritsevich, M., … Dupouy, P. (2017). Multi-instrumental observations of the 2014 Ursid meteor outburst. Monthly Notices of the Royal Astronomical Society, 468(2), 2206-2213. https://doi.org/10.1093/mnras/stx592
NO This study was supported by the Spanish grants AYA2011-26522 and AYA2015-67175-P (PI: JMTR), AYA2015-68646-P andAYA2014-61357-EXP (JMM). The FRIPON project is funded byANR. MG acknowledges support from the ERC Advanced GrantNo. 320773, and the Russian Foundation for BasicResearch, projectnos. 16-07-01072 and 16-05-00004. Research at the Ural FederalUniversity is supported by the Act 211 of the Government of theRussian Federation, agreement No 02.A03.21.0006. EB is supportedby the Universitat Ramon Llull project 2016-URL-IR-001supported by ‘Generalitat de Catalunya’. The authors acknowledgebeing a part of the network supported by the COST Action TD1403‘Big Data Era in Sky and EarthObservation’. The CINES supercomputerwas used for theoretical work. This research has been madein the framework of EURONEAR. We thank Dr Aswin Sekhar forhis valuable comments that helped to enhance this paper. This studywas done in the frame of a PhD on Physics at the AutonomousUniversity of Barcelona (UAB) under the direction of Dr. Josep M.Trigo-Rodr´ıguez and Dr. Maria Gritsevich.
DS Repositorio Institucional de la Universidad de Huelva
RD 14 jul 2026