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Chemical abundances in cold, dark interstellar clouds.

W M Irvine1, M Ohishi, N Kaifu

  • 1Nobeyama Radio Observatory, Nagano, Japan.

Icarus
|May 1, 1991
PubMed
Summary
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The Sun may have formed in cold, dark clouds. Researchers cataloged interstellar molecules in these clouds, finding chemical differences between Taurus Molecular Cloud 1 (TMC-1) and Lynd

Area of Science:

  • Astrochemistry
  • Interstellar Medium Physics
  • Star Formation

Background:

  • The Sun's origin is hypothesized to be within cold, dark interstellar clouds.
  • Understanding interstellar cloud chemistry is crucial for deciphering star and planet formation.

Purpose of the Study:

  • To compile a comprehensive list of known interstellar molecules.
  • To analyze molecular abundances in cold clouds, specifically Taurus Molecular Cloud 1 (TMC-1) and Lynd's 134N (L134N).
  • To investigate chemical variations between these clouds as potential indicators of evolutionary stages.

Main Methods:

  • Compilation of existing astronomical databases for interstellar molecules.
  • Spectroscopic analysis of molecular composition in cold cloud regions.
  • Comparative abundance analysis of molecules in TMC-1 and L134N.
Keywords:
NASA Discipline ExobiologyNon-NASA Center

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Main Results:

  • A comprehensive tabulation of known interstellar molecules is presented.
  • Molecular abundances were determined for TMC-1 and L134N.
  • Significant chemical differences were observed between TMC-1 and L134N, despite their physical similarities.

Conclusions:

  • TMC-1 and L134N exhibit distinct chemical signatures.
  • These chemical variations may reflect different evolutionary stages of cold, dark clouds.
  • Further research is needed to confirm the evolutionary link between cloud chemistry and star formation.