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On the spiral structure in the galactic distribution of co clouds

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Abstract

The CO distribution in the Galaxy is investigated through an analysis of longitude-velocity diagrams of CO emission lines for the two longitude ranges 20°<l<80° and 105°<l<140°. For the kinematics of the Galaxy we adopt the three typical models; the circular rotation, the linear density waves, and the galactic shock waves. It is shown that the distributions and kinematics of CO clouds are consistent with the predictions of the density wave model and the galactic shock model, and that the observed data of CO emissions do not contradict with the claim that the CO clouds form spiral arms.

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Author notes

  1. Tatsuya Kurita

    Present address: Aoba of Nisshin Junior High School, Nisshin, Aichi-gun, 470-01, Aichi, Japan

  2. Akira Sobue

    Present address: Kisogawa Junior High School, Kisogawa, Haguri-gun, 493, Aichi, Japan

Authors and Affiliations

  1. Department of Earth Science, Aichi University of Education, Kariya, Aichi, Japan

    Takeyasu Sawa, Tatsuya Kurita & Akira Sobue

  2. Astronomical Institute, Faculty of Science, Tohoku University, Sendai, Japan

    Yutaka Sabano

Authors
  1. Takeyasu Sawa
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  2. Tatsuya Kurita
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  3. Akira Sobue
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  4. Yutaka Sabano
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Sawa, T., Kurita, T., Sobue, A. et al. On the spiral structure in the galactic distribution of co clouds. Astrophys Space Sci 92, 181–190 (1983). https://doi.org/10.1007/BF00653599

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  • DOI: https://doi.org/10.1007/BF00653599

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