ROBOTIC SYSTEMS FOR THE DETERMINATION OFTHE COMPOSITION OF SOLAR SYSTEM MATERIALSBY MEANS OF FIREBALL SPECTROSCOPY.
J. M. Madiedo1,2. 1Facultad de Ciencias Experimentales. Universidad de Huelva. 21071 Huelva, Spain. E-mail: madiedo@cica.es. 2Dpto. de Física Atómica, Molecular y Nuclear. Facultad de Física, Universidad de Sevilla, 41012 Sevilla, Spain.
Introduction: Meteoroids are mostly originated from asteroids and comets. The mechanisms that deliver these particles toEarth provide a unique opportunity to measure from the groundthe physico-chemical properties of these Solar System materials.
Meteor spectroscopy is a useful technique to study the chemicalcomposition of these particles when they ablate in the atmosphere. Besides, the analysis of meteor spectra can provide useful
information about the mechanisms that control this ablation process, but also about the chemical nature of the parent bodies of thecorresponding meteoroids [1, 2, 3, 4]. For this reason we havedeveloped since 2006 a network of autonomous CCD devices toimage meteor spectra. This also involved the development ofsoftware for the analysis of the spectra but also for the autonomous operation of the recording devices. This research project,which has been partially funded by the University of Huelva, isnamed SMART, which is the acronym for Spectroscopy of Meteoroids in the Atmosphere with Robotic Technologies.
Instrumentation and methods: Our video spectrographs
work in a fully autonomous way by means of software specifically developed in the framework of the SMART project. These
slitless systems are based on the same low-lux CCD video cameras we employ since 2006 to monitor meteor and fireball activity [4, 5, 6]. The new higher-resolution spectral system consistsof two slitless slow-scan high-sensitivity CCD devices that employ 1000 lines/mm diffraction gratings. They operate since August 2012 from Sevilla, where an array of high-sensitivity CCD
video cameras is also used for the monitoring of meteor activity.
The new spectrographs generate imagery in FITS files which aresent to GPS synchronized computers. The exposition time is adjusted according to the conditions of the sky. These systems are
currently covering an extension of about 50ºx50º degrees in thenight sky.
Preliminary results: Most of the meteor spectra recorded byus correspond to materials with chondritic composition, althoughachondritic meteoroids have also been recorded. Although mostemission lines identified in these spectra correspond to Fe I multiplets, the contribution from the H and K lines of ionized calcium is typically detected. Other multiplets commonly identified
are Ca I-2 (422.7 nm), Na I-1 (588.9 nm) and Mg I-2 (516.7 nm).
The contributions from atmospheric N2 and O I are also seen.
Acknowledgements: This research has been partly fundedby the Spanish Ministry of Science and Innovation and the Juntade Andalucía (projects AYA2009-13227 and P09-FQM-4555).
References:[1] J.M. Trigo-Rodríguez et al. (2003) MAPS 38, 1283-1294.
[2] Trigo-Rodríguez et al. (2004) MNRAS 348, 802-810. [3] Borovicka, J. (1993) Astron. Astrophys. 279, 627-645. [4] Madiedo
J.M. and Trigo-Rodríguez J.M. (2008) EMP 102, 133-139.[5]Madiedo J.M. et al. (2010) Adv.in Astron, 2010, 1-5. [6] Madiedo J.M. et al. (2013) MNRAS, in press.