TY - JOUR
T1 - Luminous efficiency based on FRIPON meteors and limitations of ablation models
AU - Drolshagen, E.
AU - Ott, T.
AU - Koschny, D.
AU - Drolshagen, G.
AU - Vaubaillon, J.
AU - Colas, F.
AU - Zanda, B.
AU - Bouley, S.
AU - Jeanne, S.
AU - Malgoyre, A.
AU - Birlan, M.
AU - Vernazza, P.
AU - Gardiol, D.
AU - Nedelcu, D. A.
AU - Rowe, J.
AU - Forcier, M.
AU - Trigo-Rodriguez, J. M.
AU - Peña-Asensio, E.
AU - Lamy, H.
AU - Ferrière, L.
AU - Barghini, D.
AU - Carbognani, A.
AU - Di Martino, M.
AU - Rasetti, S.
AU - Valsecchi, G. B.
AU - Volpicelli, C. A.
AU - Di Carlo, M.
AU - Knapic, C.
AU - Pratesi, G.
AU - Riva, W.
AU - Stirpe, G. M.
AU - Zorba, S.
AU - Hernandez, O.
AU - Grandchamps, A.
AU - Jehin, E.
AU - Jobin, M.
AU - King, A.
AU - Sanchez-Lavega, A.
AU - Toni, A.
AU - Rimola, A.
AU - Poppe, B.
N1 - Funding Information:
Acknowledgements. We thank the European Space Agency and the University of Oldenburg for funding this project. We would especially like to thank Maria Gritsevich for her support and constructive discussions on this matter. A special gratitude goes to the FRIPON Network for providing the data used for this study and to the FRIPON team for their support of this project. All the data used in the present publication were obtained and made available by the FRIPON network (www.fripon.org). FRIPON was initiated by funding from ANR (grant no. 13-BS05-0009-03), carried by the Paris Observatory, Muséum National d’Histoire Naturelle, Paris-Saclay University and Institut Pythéas (LAM-CEREGE). Vigie-Ciel was part of the 65 million d’Observateurs project, carried by the Muséum National d’Histoire Naturelle and funded by the French Investissements d’Avenir program. FRIPON data are hosted and processed at Institut Pythéas SIP (Service Informatique Pythéas), and a mirror is hosted at IMCCE (Institut de Mécanique Céleste et de Calcul des Éphémérides/Paris Observatory) with the help of IDOC8 (Integrated Data and Operation Center), supported by CNRS and CNES. PRISMA is the Italian Network for Systematic surveillance of Meteors and Atmosphere. It is a collaboration initiated and coordinated by the Italian National Institute for Astrophysics (INAF) that counts members among research institutes, universities, associations and schools. The complete list of PRISMA members is available here: http://www.prisma.inaf.it. PRISMA was funded by 2016/0476 and 2019/0672 Research and Education grants from Fondazione Cassa di Risparmio di Torino and by a 2016 grant from Fondazione Agostino De Mari (Savona). FRIPON-Spain is coordinated from the Institute of Space Sciences (CSIC-IEEC). J.M.T.-R. and E.P.A. acknowledge financial support from the Spanish Ministry (PGC2018-097374-B-I00, PI: J.M.T.-R.). We were additionally supported by the J.M.T.-R. research project PGC2018-097374-B-I00 funded by MCI-AEI-FEDER, EU.
Publisher Copyright:
© 2021 ESO.
PY - 2021/6/1
Y1 - 2021/6/1
N2 - Context. In meteor physics, the luminous efficiency τ is used to convert the meteor's magnitude to the corresponding meteoroid's mass. However, a lack of sufficiently accurate verification methods or adequate laboratory tests mean that discussions around this parameter are a subject of controversy. Aims. In this work, we aim to use meteor data obtained by the Fireball Recovery and InterPlanetary Observation to calculate the luminous efficiencies of the recorded meteors. We also show the limitations of the methods presented herein. Methods. Deceleration-based formulas were used to calculate the masses of the pre-atmospheric meteoroids. These can in turn be compared to the meteor brightnesses to assess the luminous efficiencies of the recorded objects. Fragmentation of the meteoroids is not considered within this model. Good measurements of the meteor deceleration are required. Results. We find τ-values, as well as the shape change coefficients, of 294 meteors and fireballs with determined masses in the range of 10-6-100 kg. The derived τ-values have a median of τmedian = 2.17%. Most of them are of the order of 0.1-10%. We present how our values are obtained, compare them with data reported in the literature, and discuss several methods. A dependence of τ on the pre-atmospheric velocity of the meteor, ve, is noticeable with a relation of τ = 0.0023 ve2.3. Furthermore, a dependence of τ on the initial meteoroid mass, Me, is found with negative linear behaviour in log-log space: τ = 0.48 Me-0.47. Conclusions. The higher luminous efficiency of fast meteors could be explained by the higher amount of energy released. Fast meteoroids produce additional emission lines that radiate more efficiently in specific wavelengths due to the appearance of the so-called second component of higher temperature. Furthermore, the negative dependence of τ on Me implies that the radiation of smaller meteoroids is more efficient. The results of this study also show the limitations of the ablation-based model for the determination of the luminous efficiency.
AB - Context. In meteor physics, the luminous efficiency τ is used to convert the meteor's magnitude to the corresponding meteoroid's mass. However, a lack of sufficiently accurate verification methods or adequate laboratory tests mean that discussions around this parameter are a subject of controversy. Aims. In this work, we aim to use meteor data obtained by the Fireball Recovery and InterPlanetary Observation to calculate the luminous efficiencies of the recorded meteors. We also show the limitations of the methods presented herein. Methods. Deceleration-based formulas were used to calculate the masses of the pre-atmospheric meteoroids. These can in turn be compared to the meteor brightnesses to assess the luminous efficiencies of the recorded objects. Fragmentation of the meteoroids is not considered within this model. Good measurements of the meteor deceleration are required. Results. We find τ-values, as well as the shape change coefficients, of 294 meteors and fireballs with determined masses in the range of 10-6-100 kg. The derived τ-values have a median of τmedian = 2.17%. Most of them are of the order of 0.1-10%. We present how our values are obtained, compare them with data reported in the literature, and discuss several methods. A dependence of τ on the pre-atmospheric velocity of the meteor, ve, is noticeable with a relation of τ = 0.0023 ve2.3. Furthermore, a dependence of τ on the initial meteoroid mass, Me, is found with negative linear behaviour in log-log space: τ = 0.48 Me-0.47. Conclusions. The higher luminous efficiency of fast meteors could be explained by the higher amount of energy released. Fast meteoroids produce additional emission lines that radiate more efficiently in specific wavelengths due to the appearance of the so-called second component of higher temperature. Furthermore, the negative dependence of τ on Me implies that the radiation of smaller meteoroids is more efficient. The results of this study also show the limitations of the ablation-based model for the determination of the luminous efficiency.
KW - Atmospheric effects
KW - Comets: general
KW - Meteorites, meteors, meteoroids
KW - Methods: data analysis
KW - Minor planets, asteroids: general
KW - Techniques: photometric
UR - http://www.scopus.com/inward/record.url?scp=85108835768&partnerID=8YFLogxK
U2 - 10.1051/0004-6361/202040204
DO - 10.1051/0004-6361/202040204
M3 - Article
AN - SCOPUS:85108835768
SN - 0004-6361
VL - 650
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
M1 - A159
ER -