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J/A+AS/103/83      Line identifications in a fireball spectrum  (Borovicka 1994)
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Line identifications in a fireball spectrum
     Borovicka J.
    <Astron. Astrophys. Suppl. Ser. 103, 83 (1994)>
    =1994A&AS..103...83B
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ADC_Keywords: Comets; Spectroscopy
Keywords: meteors: spectra - line: identification

Abstract:
    305 emission lines were found in a spectrum of a fireball of -9th
    magnitude. The identification of most of the lines is given. Also a
    detailed tracing of the spectrum in the range 3600-6600{AA} is
    presented. The tracing contains also computed synthetic spectrum and
    both spectra can be easily compared. The following species were found
    in the spectrum: Fe I, Na I, Mg I, Al I, Ca I, Ti I, Cr I, Mn I, Ni I,
    Mg II, Si II, Ca II, Fe II, FeO, probably also Si I, Ba II, C_2_, and
    possibly V I, Co I, Cu I, Ti II. The presence of other chemical
    elements in meteor spectra is discussed.


File Summary:
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 FileName   Lrecl   Records   Explanations
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ReadMe         80         .   This file
table1.dat     59       475   Identifications of spectral lines observed in
                              the spectrum of the bright meteor EN 151068
spec-a.dat     15      2020  *Observed calibrated spectrum in the range
                              3575-4080{AA} at the meteor point 15F (2nd order)
spec-b.dat     15      1477  *Observed calibrated spectrum in the range
                              4050-4420{AA} at the meteor point 19F (2nd order)
spec-c.dat     15      8800  *Observed calibrated spectrum in the range
                              4400-6600{AA} at the meteor point 13F (1st order)
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Note on spec-a.dat, spec-b.dat, spec-c.dat:
    The point 13F is the brightest meteor point. The short wavelengths
    were, however, better observable in the second order spectra at
    different meteor points and these spectra were used for line
    identifications. The spectra at different points cannot be simply
    joined, because the meteor brightness and physical conditions were
    different at different points. The data given in these three files
    were used for drawing the solid line in Fig.4 of the paper.
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Byte-by-byte Description of file: table1.dat
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   Bytes Format  Units     Label     Explanations
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   1-  3  I3     ---       No        [1,305]+=  Line number (1)
   4- 10  F7.1   0.1nm     LamObs    Observed wavelength
  11- 19  F9.2   0.1nm     LamLab    ? Laboratory wavelength
  22- 34  A13    ---       Atom      Identification: atom and multiplet or
                                     molecule and vibrational band or
                                     "?" for an unidentified line
  35- 39  F5.2   eV        E1        ?lower excitation potential
  40- 46  F7.2   ---       log(gf)   ? oscillator strength
  47- 53  F7.2   100W/sr   Icom      ?computed line intensity
  54- 60  A7     ---       Rem       Remark (2)
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Note (1): One observed line may be formed by several lines.
Note (2): the numbers have the following meaning:
      1)  contribution of Fe II 4583.85 A ?
      2)  possible contribution of C III - 1
      3)  contribution of C_2
      4)  only fragment?
      5)  cannot explain the whole line
      6)  overexposed line
          p.:  point (boundaries of meteor points used are marked)
          2nd: 2nd second spectrum
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Byte-by-byte Description of file: spec-a.dat, spec-b.dat, spec-c.dat
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   Bytes Format Units      Label   Explanations
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   1-  7  F7.2  0.1nm      Lambda  Wavelength (valid for the main piece)
   8- 15  F8.4  kW/nm/sr   OIR     Observed intensity of radiation (including
                                    the radiation of the fragments)
                                    in 10+9erg/s/A/sr
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(End)                                           Patricia Bauer [CDS] 13-Jan-1994