Drouard A. auteur aut IRD Vernazza P. auteur aut IRD Loehle S. auteur aut IRD Gattacceca J. auteur aut IRD Vaubaillon J. auteur aut IRD Zanda B. auteur aut IRD Birlan M. auteur aut IRD Bouley S. auteur aut IRD Colas François auteur aut IRD Eberhart M. auteur aut IRD Hermann T. auteur aut IRD Jorda L. auteur aut IRD Marmo C. auteur aut IRD Meindl A. auteur aut IRD Oefele R. auteur aut IRD Zamkotsian F. auteur aut IRD Zander F. auteur aut IRD text journalArticle eng text/pdf reformatted digital access Context. Determining the source regions of meteorites is one of the major goals of current research in planetary science. Whereas asteroid observations are currently unable to pinpoint the source regions of most meteorite classes, observations of meteors with camera networks and the subsequent recovery of the meteorite may help make progress on this question. The main caveat of such an approach, however, is that the recovery rate of meteorite falls is low (< 20%), implying that the meteoritic analogues of at least 80% of the observed falls remain unknown. Aims. Spectroscopic observations of incoming bolides may have the potential to mitigate this problem by classifying the incoming meteoritic material. Methods. To probe the use of spectroscopy to determine the meteoritic analogues of incoming bolides, we collected emission spectra in the visible range (320-880 nm) of five meteorite types (H, L, LL, CM, and eucrite) acquired in atmospheric entry-like conditions in a plasma wind tunnel at the Institute of Space Systems (IRS) at the University of Stuttgart (Germany). A detailed spectral analysis including a systematic line identification and mass ratio determinations (Mg/Fe, Na/Fe) was subsequently performed on all spectra. Results. It appears that spectroscopy, via a simple line identification, allows us to distinguish the three main meteorite classes (chondrites, achondrites and irons) but it does not have the potential to distinguish for example an H chondrite from a CM chondrite. Conclusions. The source location within the main belt of the different meteorite classes (H, L, LL, CM, CI, etc.) should continue to be investigated via fireball observation networks. Spectroscopy of incoming bolides only marginally helps precisely classify the incoming material (iron meteorites only). To reach a statistically significant sample of recovered meteorites along with accurate orbits (> 100) within a reasonable time frame (10-20 years), the optimal solution may be the spatial extension of existing fireball observation networks. specialized meteorites meteors meteoroids techniques: spectroscopic 020 060 613 A54 [16 p.] 2018 1432-0746 https://www.documentation.ird.fr/hor/fdi:010073056 10.1051/0004-6361/201732225 1432-0746 [F B010073056] https://www.documentation.ird.fr/hor/fdi:010073056 https://horizon.documentation.ird.fr/exl-doc/pleins_textes/divers18-06/010073056.pdf IRD - Base Horizon / Pleins textes 2018-07-03 2023-07-11 fdi:010073056 fre