Hostname: page-component-848d4c4894-2xdlg Total loading time: 0 Render date: 2024-06-30T22:51:00.908Z Has data issue: false hasContentIssue false
  • English
  • Français

11. Some unusual spectra of meteors from the Palomar 18-inch Schmidt file

Published online by Cambridge University Press:  14 August 2015

R. Barbon  and
J. A. Russell
R. Barbon
Affiliation:
California Institute of Technology, Pasadena, Calif., U.S.A.*
J. A. Russell
Affiliation:
University of Southern California, Los Angeles, Calif., U.S.A.

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Five meteoric spectra have been studied that were obtained during the period mid-June to mid-December, 1966. They include spectra of a Perseid, a Geminid, and three sporadic meteors. Four were photographed on Royal Pan emulsion without a filter; the Geminid on Tri X Aerecon with a GG11 filter.

Lines in the spectrum of one of the sporadic meteors indicate that two meteoroidal fragments were involved which diverged with increasing atmospheric penetration and which flared at different altitudes, indicating that the flares were not the result of atmospheric stratification.

The second sporadic and the Perseid were photographed about 2½ hours apart. The sodium D line is strong in the Perseid but does not appear in the sporadic spectrum. If present, it is blended with the diagonal sequence Δv = + 4 of the first positive group of the neutral nitrogen molecule, which appears in both spectra. A line questionably identified as the forbidden line of oxygen at 5577 Å appears faintly in the sporadic. The strength of the N2 sequence in these two spectra, and the absence of the D line in the sporadic, are very unusual. The proximity in time of appearance of these two spectra, and the absence of the N2 bands from the other two sporadic spectra, suggest that a temporary atmospheric condition may be responsible for the strength of the nitrogen radiation.

The Geminid has as its principal feature the Δv = + 3 sequence of the first positive group of N2. We have not previously observed this band in meteors as low in velocity as the Geminids.

Type
Session 2
Information
Symposium - International Astronomical Union , Volume 33: Physics and Dynamics of Meteors , 1968 , pp. 119 - 127
Copyright
Copyright © Reidel 1968 

References

Cook, A.F., Millman, P.M. (1955) Astrophys. J., 121, 250.CrossRefGoogle Scholar
Halliday, I. (1960) Astrophys. J., 131, 25.CrossRefGoogle Scholar
Halliday, I. (1963) Smithson. Contr. Astrophys., 7, 161.Google Scholar
Millman, P.M. (1935) Ann. Harv. Col. Obs., 82, 149.Google Scholar
Millman, P.M. (1963) Smithson. Contr. Astrophys., 7, 119.Google Scholar
Millman, P.M., Cook, A.F. (1959) Astrophys. J., 130, 648.CrossRefGoogle Scholar
Moore, C.E. (1945) Contr. Princeton Univ. Obs., 20.Google Scholar
Rinehart, J. (1951) Private communication.Google Scholar
Russell, J.A. (1957) Publ. astr. Soc. Pacific, 69, 436.CrossRefGoogle Scholar
Russell, J.A. (1960) Publ. astr. Soc. Pacific, 72, 291.CrossRefGoogle Scholar
Russell, J.A. (1964) Meteoritics, 2, 117.CrossRefGoogle Scholar