Skip to main content
U.S. Department of Energy
Office of Scientific and Technical Information

THE ORIGIN OF THE 3.4 {mu}m FEATURE IN WILD 2 COMETARY PARTICLES AND IN ULTRACARBONACEOUS INTERPLANETARY DUST PARTICLES

Journal Article · · Astrophysical Journal
 [1];  [2]; ;
  1. Astronomy Department, University of Washington, Seattle, WA 98195 (United States)
  2. Department of Physics, SUNY-Plattsburgh, Plattsburgh, NY 12901 (United States)
We analyzed two ultracarbonaceous interplanetary dust particles (IDPs) and two cometary Wild 2 particles with infrared spectroscopy. We characterized the carrier of the 3.4 {mu}m band in these samples and compared its profile and the CH{sub 2}/CH{sub 3} ratios to the 3.4 {mu}m band in the diffuse interstellar medium (DISM), in the insoluble organic matter from three primitive meteorites, in asteroid 24 Themis, and in the coma of comet 103P/Hartley 2. We found that the 3.4 {mu}m band in both Wild 2 and IDPs is similar, but different from all of the other astrophysical environments that we compared it to. The 3.4 {mu}m band in the IDPs and Wild 2 particles is dominated by CH{sub 2} groups, the peaks are narrower and stronger than in the meteorites, asteroid Themis, and the DISM. Also, the presence of the carbonyl group C=O at {approx}1700 cm{sup -1} (5.8 {mu}m) in most of the spectra of our samples indicates that these aliphatic chains have O bonded to them, which is quite different from astronomical spectra of the DISM. Based on all of these observations, we conclude that the origin of the carrier of the 3.4 {mu}m band in the IDPs and Wild 2 samples is not interstellar; instead, we suggest that the origin lies in the outermost parts of the solar nebula.
OSTI ID:
22126958
Journal Information:
Astrophysical Journal, Journal Name: Astrophysical Journal Journal Issue: 2 Vol. 765; ISSN ASJOAB; ISSN 0004-637X
Country of Publication:
United States
Language:
English