Volume 652, August 2021
|Number of page(s)||29|
|Section||Planets and planetary systems|
|Published online||13 August 2021|
Luminous efficiency of meteors derived from ablation model after assessment of its range of validity
University of Oldenburg, Division for Medical Radiation Physics and Space Environment, Germany
e-mail: firstname.lastname@example.org; email@example.com
2 European Space Agency, ESTEC, Keplerlaan 1, 2201 AZ Noordwijk, The Netherlands
3 Chair of Astronautics, TU Munich, Germany
4 IMCCE, Observatoire de Paris, PSL Research University, CNRS UMR 8028, Sorbonne Université, France
5 Institut de Minéralogie, Physique des Matériaux et Cosmochimie (IMPMC), Muséum National d’Histoire Naturelle, CNRS UMR 7590, Sorbonne Université, 75005 Paris, France
6 FRIPON (Fireball Recovery and InterPlanetary Observation) and Vigie-Ciel Team, France
7 GEOPS-Géosciences, CNRS, Université Paris-Saclay, 91405, Orsay, France
8 Service Informatique Pythéas (SIP) CNRS – OSU Institut Pythéas - UMS 3470, Marseille, France
9 Aix Marseille Univ, CNRS, CNES, LAM, Marseille, France
10 INAF – Osservatorio Astrofisico di Torino – Via Osservatorio 20, 10025 Pino Torinese, TO, Italy
11 Astronomical Institute of the Romanian Academy, Bucharest, 040557, Romania
12 MOROI (Meteorites Orbits Reconstruction by Optical Imaging) Astronomical Institute of the Romanian Academy, Bucharest, Romania
13 SCAMP (System for Capture of Asteroid and Meteorite Paths), FRIPON, UK
14 Planétarium Rio Tinto Alcan / Espace pour la vie, Montréal, Québec, Canada
15 Réseau DOME, (Détection et Observation de Météores/Detection and Observation of Meteors), Canada
16 SPMN (SPanish Meteor Network), FRIPON, Spain
17 Institute of Space Sciences (CSIC), Campus UAB, Facultat de Ciències, 08193 Bellaterra, Barcelona, Catalonia, Spain
18 Institut d’Estudis Espacials de Catalunya (IEEC), 08034 Barcelona, Catalonia, Spain
19 FRIPON-Belgium, Belgium
20 Royal Belgian Institute for Space Aeronomy, Brussels, Belgium
21 Natural History Museum, Burgring 7, 1010 Vienna, Austria
22 FRIPON-Austria, Austria
23 Università degli Studi di Torino, Dipartimento di Fisica, Via Pietro Giuria 1, 10125 Torino, TO, Italy
24 INAF 0– Osservatorio di Astrofisica e Scienza dello Spazio Via Piero Gobetti 93/3, 40129 Bologna, BO, Italy
25 INAF – Istituto di Astrofisica e Planetologia Spaziali Via del Fosso del Cavaliere 100, 00133 Roma, RM, Italy
26 CNR – Istituto di Fisica Applicata Nello Carrara, Via Madonna del Piano, 10 50019 Sesto Fiorentino (FI), Italy
27 Space sciences, Technologies Astrophysics Research (STAR) Institute, Université de Liège, Liège 4000, Belgium
28 Università degli Studi di Firenze – Dipartimento di Scienze della Terra, Via Giorgio La Pira, 4, 50121 Firenze, FI, Italy
29 Natural History Museum, Cromwell Road, London, UK
30 Dep. Física Aplicada I, Escuela de Ingeniería de Bilbao, Universidad del País Vasco/Euskal Herriko Unibertsitatea, 48013 Bilbao, Spain
31 Aula EspaZio Gela, Escuela de Ingeniería de Bilbao, Universidad del País Vasco/Euskal Herriko Unibertsitatea, 48013 Bilbao, Spain
32 FRIPON-Netherlands, European Space Agency, SCI-SC, Keplerlaan 1, 2201 AZ Noordwijk, The Netherlands
33 Osservatorio Astronomico del Righi, Via Mura delle Chiappe 44R, 16136 Genova, GE, Italy
34 Departament de Química, Universitat Autònoma de Barcelona, 08193 Bellaterra, Catalonia, Spain
Accepted: 20 May 2021
Context. The luminous efficiency, τ, can be used to compute the pre-atmospheric masses of meteoroids from corresponding recorded meteor brightnesses. The derivation of the luminous efficiency is non-trivial and is subject to biases and model assumptions. This has led to greatly varying results in the last decades of studies.
Aims. The present paper aims to investigate how a reduction in various observational biases can be achieved to derive (more) reliable values for the luminous efficiency.
Methods. A total of 281 meteors observed by the Fireball Recovery and InterPlanetary Observation Network (FRIPON) are studied. The luminous efficiencies of the events are computed using an ablation-based model. The relations of τ as a function of the pre-atmospheric meteoroid velocity, ve, and mass, Me, are studied. Various aspects that could render the method less valid, cause inaccuracies, or bias the results are investigated. On this basis, the best suitable meteors were selected for luminous efficiency computations.
Results. The presented analysis shows the limits of the used method. The most influential characteristics that are necessary for reliable results for the τ computation were identified. We study the dependence of τ on the assumed meteoroid’s density, ρ, and include improved ρ-values for objects with identified meteoroid stream association. Based on the discovered individual biases and constraints we create a pre-debiased subset of 54 well-recorded events with a relative velocity change >80%, a final height <70 km, and a Knudsen number Kn < 0.01; this last value indicates that the events were observed in the continuum-flow regime. We find τ-values in the range between 0.012% and 1.1% for this pre-debiased subset and relations of τ to ve and Me of: τ=7.33⋅ve−1.10 and τ=0.28⋅Me−0.33.
Conclusions. The derived luminous efficiency of meteoroids depends on the assumed material density. Our results indicate that the applied debiasing method improves the analysis of τ from decelerated meteoroids. The underlying method is only valid for meteors in the continuum-flow regime. These events tend to have low end heights, large masses, and high deceleration.
Key words: meteorites, meteors, meteoroids / minor planets, asteroids: general / comets: general / techniques: photometric / atmospheric effects / methods: data analysis
© ESO 2021
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