EGU General Assembly 2023
© Author(s) 2023. This work is distributed under
the Creative Commons Attribution 4.0 License.

Physical parameters of meteoroids

Ioana Lucia Boaca1, Maria Gritsevich2,3,4, Alin Nedelcu1,5, Tudor Boaca6,7, François Colas5, Adrien Malgoyre8, Brigitte Zanda5, and Pierre Vernazza9
Ioana Lucia Boaca et al.
  • 1Astronomical Institute Bucharest, Fundamental Astronomy, Bucharest, Romania (
  • 2Finnish Geospatial Research Institute (FGI), Vuorimiehentie 5, FI-02150 Espoo, Finland
  • 3University of Helsinki, Faculty of Science, Gustaf Hällsrömin katu 2, FI-00014 Helsinki, Finland
  • 4Finnish Fireball Network, Ursa Astronomical Association, Kopernikuksentie 1, FI-00130 Helsinki, Finland
  • 5IMCCE, Observatoire de Paris, 77 av Denfert Rochereau, 75014 Paris Cedex, France
  • 6Department of Computer Science, Information Technology, Mathematics and Physics, Petroleum-Gas University of Ploiesti, 39 Bucharest Bvd Street, 100680 Ploiesti, Romania
  • 7Simion Stoilow Institute of Mathematics of the Romanian Academy, 21 Calea Grivitei Street, 010702 Bucharest, Romania
  • 8Service Informatique Pythéas (SIP) CNRS – OSU Institut Pythéas – UMS 3470, Marseille, France
  • 9Aix Marseille Univ, CNRS, CNES, LAM, Marseille, France

In this work we present the main characteristics that derive from the analysis of the luminous part of the trajectory of a meteoroid. Our study is based on applying the α-β algorithm (Gritsevich 2008, Gritsevich 2009, Gritsevich et al. 2012, Lyytinen and Gritsevich 2016, Sansom et al. 2019, Boaca et al. 2022) to the latest detections recorded by the MOROI (Nedelcu et al. 2018) component of the FRIPON network (Colas et al. 2020). Our input parameter are the height and velocity of the meteoroid and the way they change with time. Based on this we determine the ballistic coefficient α and the mass loss parameter β for each analysed meteor event. The α-β algorithm is used in order to decide which of the fireball events produce meteorites and which are fully ablating in the atmosphere. Furthermore, the α and β parameters allow us to determine the mass of the studied meteoroids e.g. at the beginning and at the end of the luminous trajectory.

Boaca I., et al. (2022), ApJ, 936, 150.

Colas, F., et al. (2020), A&A, 644, A53.

Gritsevich, M. I. (2008), DokPh, 53, 97.

Gritsevich, M. I. (2009), AdSpR, 44, 323.

Gritsevich, M. I., et al., (2012), CosRe, 50, 56.

Lyytinen, E., & Gritsevich, M. (2016), P&SS, 120, 35.

Nedelcu, D. A., et al. (2018), RoAJ, 28, 57.

Sansom, E. K., et al. (2019), ApJ, 885, 115.


The work of IB and AN was partially supported by a grant of the Ministry of National Education and Scientific Research, PNIII-P2-1214/25.10.2021, program no. 36SOL/2021.  MG acknowledges the Academy of Finland project no. 325806 (PlanetS).

How to cite: Boaca, I. L., Gritsevich, M., Nedelcu, A., Boaca, T., Colas, F., Malgoyre, A., Zanda, B., and Vernazza, P.: Physical parameters of meteoroids, EGU General Assembly 2023, Vienna, Austria, 24–28 Apr 2023, EGU23-8154,, 2023.