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Complementary Laboratory Measurements of Individual Interplanetary Dust Particles

Published online by Cambridge University Press:  12 April 2016

A. Fahey ,
K.D. McKeegan ,
S.A. Sandford ,
R.M. Walker ,
B. Wopenka  and
E. Zinner
A. Fahey
Affiliation:
McDonnell Center for the Space Sciences, Washington University, St. Louis, MO 63130, USA
K.D. McKeegan
Affiliation:
McDonnell Center for the Space Sciences, Washington University, St. Louis, MO 63130, USA
S.A. Sandford
Affiliation:
McDonnell Center for the Space Sciences, Washington University, St. Louis, MO 63130, USA
R.M. Walker
Affiliation:
McDonnell Center for the Space Sciences, Washington University, St. Louis, MO 63130, USA
B. Wopenka
Affiliation:
McDonnell Center for the Space Sciences, Washington University, St. Louis, MO 63130, USA
E. Zinner
Affiliation:
McDonnell Center for the Space Sciences, Washington University, St. Louis, MO 63130, USA

Abstract

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Complementary analysis techniques including electron microscopy (SEM/EDX and TEM), molecular spectroscopy (FTIR and Raman), and secondary ion mass spectrometry (SIMS), are used to study individual dust particles collected in the stratosphere. Large deuterium enrichments and solar flare tracks show that most particles in the “chondritic” class are interplanetary dust particles (IDPs). Infrared transmission spectra of most IDPs fall into three major classes (layer-lattice silicates, pyroxenes and olivines). TEM and Raman measurements confirm this classification. The IR spectra show certain similarities to spectra observed in comets and protostars. In particular the 6.8 μm features observed in protostars and IDPs may have a common origin. Large D excesses are observed in IDPs of the first two IR classes. The correlation of D/H ratios with the C concentration indicates a carbonaceous carrier of the excess D. The D enrichments and IR spectra provide links to interstellar molecular cloud material.

Type
III. Interplanetary Dust: Laboratory Studies
Information
International Astronomical Union Colloquium , Volume 85: Properties and Interactions of Interplanetary Dust , 1985 , pp. 149 - 155
Copyright
Copyright © Reidel 1985

References

[1] Brownlee, D.E., Pilachowski, L., Olszewski, E., and Hodge, P.W. (1980) In Solid Particles in the Solar System, (eds. Halliday, I. and McIntosh, B.A.), D. Reidel.Google Scholar
[2] Rajan, R.S. Brownlee, D.E., Tomandl, D., Hodge, P.W., Farrar, H. IV, and Britten, R.A. (1977) Nature 267, 133.Google Scholar
[3] Hudsson, B. Flynn, G.J., Fraundorf, P., Hoheiiberg, C.M., and Shirek, J. (1981) Science 211, 383–386.Google Scholar
[4] Zinner, E., McKeegan, K.D., and Walker, R.M. (1983) Nature 305, 119.Google Scholar
[5] McKeegan, K.D., Walker, R.M. and Zinner, E., Geochim. Cosmochim. Acta, submitted.Google Scholar
[6] Bradley, J.P. and Brownlee, D.E. (1984) 47th Meteoriticai Soc. Conf. U-l.Google Scholar
[7] Fraundorf, P., McKeegan, K.D., Sandford, S.A., Swan, P., and Walker, R.M. (1982) J. Geophvs. Res. 83. A403.Google Scholar
[8] Sandford, S.A. and Walker, R.M. (1984) Astrophvs. J., submitted.Google Scholar
[9] Sandford, S.A., Fraundorf, P., Patel, R., and Walker, R.M. (1982) Meteoritics 17, 276.Google Scholar
[10] Soifer, V.T., Puetter, R.C., Russell, R.W., Willner, S.P., Harvey, P.M. and Geillett, F.C. (1979) Ap. J. 232, L53.Google Scholar
[11] Fraundorf, P. (1981) Geochim. Cosmochim. Acta 45, 915.Google Scholar
[12] Christoffersen, R. and Buseck, P.R. (1983) Science 222, 1327.Google Scholar
[13] Bradley, J.P., Brownlee, D.E., and Veblen, D.R. (1983) Nature 301, 473.Google Scholar
[14] Tomeoka, K. and Buseck, P.R. (1984) 47th Meteoriticai Soc. Conf., S-l.Google Scholar
[15] Tomeoka, K. and Buseck, P.R. (1984) Earth Planet. Sci. Lett. 69, 243.Google Scholar
[16] Bradley, J.P., Christofferson, R., Tomeoka, K., personal communication.Google Scholar
[17] Fraundorf, P., Patel, R.I., Walker, R.M., Freeman, JJ. and Adar, F. (1982) Lunar Planet. Science XIII. 231.Google Scholar
[18] Wopenka, B. and Sandfotd, S.A. (1984) 47th Meteoriticai Soc. Conf., S-5.Google Scholar
[19] Christoffersen, R. and Buseck, P.R., to be published.Google Scholar
[20] Yang, J. and Epstein, S. (1983) Geochim. Cosmochim. Acta 47, 2199.CrossRefGoogle Scholar