Context. The main problem in establishing a parent body for a meteoroid stream is the choice of a reliable meteoroid stream identification method. There are several identification methods based on three components: a dynamical similarity function, a threshold value, and meteoroid stream search algorithm. Aims. The French Meteor Network, developed in the CABERNET project (PODET-MET), will soon provide a large amount of meteor observation data aiming to establish a parent body for each observed meteor. We therefore aim to obtain the value of the upper limit to the criteria that we can later use for data provided by the French Meteor Network. Methods. We tested four D-criteria, using artificial data sets for which the parent body is known. We obtained threshold values and applied them to the Armagh Observatory meteor database. A detailed comparison is made between a similarity function based on the orbital elements and the function defined by quasi-invariants. Results. We detected major meteoroid streams in the Armagh Observatory meteor database. A few meteors were also found to be associated with the asteroid 2005 UW6 -an asteroids not considered as a possible parent body for Taurid complex before. However, the problem of finding the appropriate threshold value that would work with all meteoroid streams is still open.

Few high‐resolution video cameras have been used for observing meteors, so the orbits obtained have high uncertainty. Precise orbits are necessary so that the meteors can be integrated backwards in time and be identified with their parent body. Also, by comparing these orbits with a theoretical evolution model, the meteors can be associated with a particular dust trail. An electronic shutter system has been developed to enhance the temporal resolution for large CCD sensors. For the first time, an LH100 camera with an electronic shutter system has been tested for observing meteors. This new innovational technique has removed the theoretical upper limit – resulting from slow frame rates – to the size of CCD that can be used for the detection of meteors. Three such cameras will be installed in southern France to create a network for determining the orbits of meteors; this will be called the CAmera for BEtter Resolution NETwork (CABERNET). Here, we present preliminary results from the Geminid test campaign, which made use of this camera.

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A rare outburst of the Aurigid meteor shower was predicted to occur on 2007 September 1 at 11:36 ± 20 min ut due to Earth's encounter with the one‐revolution dust trail of long‐period comet C/1911 N1 (Kiess). The outburst was predicted to last ∼1.5 h with peak zenithal hourly rate of ∼200 h−1, which is ∼20 times higher than the annual Aurigid shower. Three members of Armagh Observatory observed this outburst from the general area of San Francisco, CA, USA, where the shower was anticipated to be best seen. Observed radiant, velocity and activity peak time were consistent with the predictions, whereas the zenithal hourly rate was about half of the predicted value. Five Aurigids were observed by two stations simultaneously, enabling their spatial trajectory to be worked out. The orbits of these double station meteors are in good agreement with that of their parent comet Kiess. The outburst was abundant in bright (−2 to +1 mag) meteors. The first high‐altitude Aurigid, with a beginning height of 137.1 km, was recorded.