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Spectral Analysis of Meteors and Meteor Trains

Explore meteor photography and spectroscopy, showcasing a detailed look at meteor heights, speeds, and elemental abundances in vapor clouds. Learn about spectral lines and their implications in meteor science.

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Spectral Analysis of Meteors and Meteor Trains

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  1. Spectra of meteors and meteor trains Jiří Borovička Department of Interplanetary Matter

  2. Meteor photograph

  3. All-sky image Kouřim bolide (– 13 mag)

  4. Bolide – 18 mag

  5. Double-station video meteor

  6. Meteor speeds 11 – 73 km/s Faint meteors: 110 – 80 km Fireballs: 200 – 20 km Meteor heights

  7. HIGH RESOLUTION PHOTOGRAPHIC SPECTRA OF FIREBALLS

  8. Battery of six photographic grating cameras with rotating shutter in Ondřejov

  9. Example of a photographic prism spectrum of a bright Perseid meteor

  10. Detail of the prism spectrum

  11. Example of photographic grating spectrum of a slow sporadic fireball zero order first order second order

  12. detail of grating spectrum

  13. Detail of a Perseid spectrum almost head-on meteor blue part shown (3700–4600 Å)

  14. Radiative transfer in spectral lines

  15. Assuming thermal equilibrium

  16. Emission curve of growth

  17. Model assumptions • The radiation originates in a finite slab of gas (plasma) with a cross section P • Atomic level population is described by the Boltzmann law for an excitation temperature T • Self-absorption is taken into account (the gas is not optically thin)

  18. Free parameters • Excitation temperature, T • Column densities of observable atoms, Nj • Meteor cross-section, P • Damping constant, 

  19. Total number of Fe atoms

  20. Temperature

  21. Cross-section

  22. Electron density

  23. Two components in meteor spectra • The spectra can be explained by the superposition of two components with different temperatures • The main component, T = 4500 K - present in all spectra - temperature does not depend on velocity! - originates from a relaxed vapor cloud near and behind the meteoroid

  24. The second component, T = 10 000 K - present in bright and fast meteors (vapor lines – air lines present also in faint fast meteors) - temperature does not depend on velocity (or only slightly) - originates from a transition zone in the front of the vapor cloud - typical lines: Ca II, Mg II, Si II

  25. Two components Example of a Perseid fireball

  26. Determination of elemental abundances • Estimation of electron density • Use of Saha equation • Determine ionization degree • Recompute neutral atom abundances to total abundances

  27. Estimation of electron density • From meteor size and atom column densities + neutrality condition • From CaII/CaI ratio (if the high temperature component is absent) • By combining both components podivat se podrobneji !

  28. Electron density from atom densities

  29. Abundances in meteor vapors low cometary Fe/Mg volatile depletion in Geminids incomplete evaporation Cr ??

  30. Incomplete evaporation

  31. Abundances along the trajectory

  32. Ca/Fe model evaporation Schaefer & Fegley (2005)

  33. LOW RESOLUTION VIDEO SPECTRA OF METEORS

  34. Spectral and direct cameras in Ondřejov

  35. LEONID METEOR SPECTRUM November 18, 2001 10:24:14 UT Mt. Lemmon Meteor magnitude: –1.5

  36. frame 21P height 109 km IR end O [O] 557nm Na Mg blue end

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