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Observations of the 2001 Leonidsґ Storm from Northern Australia with "TIMES"
D. MartМnez-Delgado1, L.R. Bellot-Rubio2, аngel R. LСpez-SАnchez1, Miquel Serra-Ricart1 & P. RodrМguez-Gil1.
1

Instituto de AstrofМsica de Canarias, La Laguna, Tenerife, Spain 2 Kiepenheuer-Institut fЭr Sonnenphysik , Freiburg, Germany
ABSTRACT

We present the preliminary results on the scientific mission of the Instituto de Astrofisica de Canarias (Spain) to observe the 2001 Leonid meteor storm. Observations were made using image-intensified video cameras in double-station from the Northern territory of Australia. We will also introduce the TIMES (Teide Intensifier Meteor System) experiment, which is operating in the Teide Observatory (Tenerife, Canary Island, Spain). It is composed by two fixed automated image-intensified video cameras and it is based on the MetRec meteor detection and analysis software, which allows for efficient video observations of meteor with only a minimum of human interaction. It is the first video cameras ever that operates on a regular basis in Spain and it is expected that collects meteor data thoughout the full year.

THE TIMES EXPERIMENT IN THE TEIDE OBSERVATORY
TIMES (Teide Intensifier MEteor System) is operating in the Teide Observatory (longitude 16є 30' 35" W est, latitude 28є 18' 00" North, altitude 2200 m), located in the island of Tenerife (Canary Island, Spain). It deploys two fixed automated video-i ntensified video cameras (see Table 1). The data acquision and reduction is based i n the MetRec meteor detection software, which allows for efficient video observations of meteor with only a minimum of human interaction. In addition, it is possible to carry out double station observations i n collaboration with amateur astronomer operati ng a similar equipment from La Palma, a nearby island situated at 100 km from Tenerife. In addition, our equipment was portable and could be operated usi ng standard power supply. TIMES was used in this way in the observations of the 1999 Leonid storm from Vilaflor (Tenerife; Molau, Rendtel & Bellot 2001) and the 2001 Leonid storm from the Northern Territory in Australia. The mai n scientific target of TIMES is to build the complete survey of the meteoroid particle population along the orbit of the Earth. This i ncl udes to determine the space densities (BellotRubio 1994) and orbital parameter of the different meteoroid streams in the Earth neighbourhood.

OBSERVATIONS OF THE LEONIDS STORM 2001
Observations of the 2001 Leonid meteor storm were obtai ned from the Northern territory in Australia during the nights of November 17th and 18th, 2001. Two locations 100 km apart were used for the video observations i n double station: TIMES1 was situated i n Devil Marble's and TIMES2 i n a location close to Tennant Creek (see geographic coordinates in Table 2). Both cameras were aligned so that the center of view aimed at a heigh of 100 km. The preliminary analysis presented here has been obtai ned from visual inspection of the video tapes coveri ng only the Asian Leonid storm period. The total number of registered Leonid meteors and time interval (in Universal Time) of TIMES 1 and TIMES 2 are given in Table 2. The defi nitive data analysis using MetRec software is in progress.

RESULTS
Figure 1 shows the preliminary activity profile of the Asian Leonid storm obtai ned from the mean of the number of meteors registered by each camera i n interval of 5 minutes. From this profile, we concl ude that the highest activity was at 18h 17m ± 3 m UT, confirming the peak of activity reported by IMO (Arlt et al. 2001). This is in excellent agreement with the predictions of the theoretical model by Lyyti nen, Nissinen & van Flandern (2001) for the dust trail 4-revolution ago (perihelion passage in 1866). In addition, our observation a second peak at 18h 02m ± 3 m UT, in good agreement with the visual IMO observations too (Arlt et al. 2001). This additional enhancement is also predicted by Lyytinen et al. (2001) for the dust trail from 9revol ution ago (peri helion passage in 1699). However, we cannot confirm the additional peak at 18h 30m UT reported from visual observers (Arlt et al. 2001) visual observations, which was not predicted by any FIGURE 1 available model. Figure 2 displays the magnitude distributions for each camera. The distribution is unexpected flat and stri nkingly different from the visual magnitude distribution. A more detailed analysis is necessary to confirm this.

TABLE 2

FIGURE 2

REFERENCES
Arlt, R., Kac J., Krumov, V., Buchmann, A & Verbert, J. 2001, WGN Journal of the International Meteor Organization 29, 187 Bellot-Rubio, L. R. 1994, WGN, Journal of the International Meteor Organization 22, 118 Lyytinen, E., Nissinen, M. & van Flandern, T. 2001, WGN, Journal of the International Meteor Organization 29, 110 Molau, S., Rendtel, J., & Bellot Rubio, L. R. 2001, EM&P, 87, 1

TABLE 1