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Remnant Molecular Clouds in the Ori OB 1 Association

Published online by Cambridge University Press:  16 May 2016

Katsuo Ogura  and
Koji Sugitani
Katsuo Ogura
Affiliation:
Kokugakuin University, Higashi, Shibuya-ku, Tokyo 150-8440, Japan; [email protected]
Koji Sugitani
Affiliation:
Institute for Natural Sciences, Nagoya-City University, Mizuho-ku, Nagoya 467-8501, Japan
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Abstract

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We suggest and give some evidence that as an HII region expands and the O stars evolve into B giants, remains of the molecular clouds first appear as bright-rimmed clouds, then as cometary globules and finally as small clouds which are visible by the reflected light from the B giants. We propose to call the last of these ‘reflection clouds’ and all three categories collectively ‘remnant clouds’. A list is presented of about 80 objects of these remnant clouds in the Ori OB 1 association. In the Belt region there is a beautiful spatial sequence from bright-rimmed clouds through cometary globules to reflection clouds. We suspect that retarded star formation in remnant clouds can explain the presence of so-called dispersed T Tau stars in the peripheries of OB associations.

Keywords

ISM: molecular cloudsISM: globulesHII regionsOB associationsstars: formation
Type
Research Article
Information
Publications of the Astronomical Society of Australia , Volume 15 , Issue 1 , 1998 , pp. 91 - 98
Copyright
Copyright © Astronomical Society of Australia 1998

References

Bally, J., Langer, W. D., Wilson, R. W., Stark, A. A., & Pound, M. W. 1991, in IAU Symp. 147, Fragmentation of Molecular Clouds and Star Formation, ed. I. Falgarone, F. Boulanger & G. Duvert (Dordrecht: Kluwer), p. 11 CrossRefGoogle Scholar
Briceño, C., Hartmann, L. W., Stauffer, J. R., Gagne, M., Stern, R. A., & Caillault, J.-P. 1997, AJ, 113, 740 Google Scholar
Clemens, D. P., & Barvainis, R. 1988, ApJS, 68, 257 Google Scholar
Dorschner, J., & Gürtler, J. 1964, Astron. Nachr., 287, 257 Google Scholar
Feigelson, E. D. 1996, ApJ, 468, 306 Google Scholar
Lefloch, B., & Lazareff, B. 1994, A&A, 289, 559 Google Scholar
Maddalena, R. J., Morris, M., Moscowitz, J., & Thaddeus, P. 1986, ApJ, 303, 375 CrossRefGoogle Scholar
Lynds, B. T. 1965, ApJS, 12, 163 Google Scholar
Maddalena, R. J., Morris, M., Moscowitz, J., & Thaddeus, P. 1986, ApJ, 303, 375 Google Scholar
Nakano, M., Kogure, T., & Wiramihardja, S. 1995, PASJ, 48, 889 Google Scholar
Nakano, M., Ogura, K., Sugitani, K., & Tamura, M. 1998, in preparationGoogle Scholar
Reipurth, B. 1983, A&A, 117, 183 Google Scholar
Sterzik, M. F., Alcala, J. M., Neuhäuser, R., & Schmidt, J. H. M. M. 1995, A&A, 297, 418 Google Scholar
Sterzik, M. F., & Durisen, R. H. 1995, A&A, 304, L9 Google Scholar
Sugitani, K., Fukui, Y., & Ogura, K. 1991, ApJS, 77, 59 CrossRefGoogle Scholar
Sugitani, K., & Ogura, K. 1994, ApJS, 92, 163 CrossRefGoogle Scholar
Sugitani, K., Tamura, M., & Ogura, K. 1995, ApJL, 455, L39 CrossRefGoogle Scholar
Tatematsu, K., et al. 1993, ApJ, 404, 643 Google Scholar
Zealey, W. J., Ninkov, Z., Rice, E., Hartley, M., & Tritton, S. B. 1983, ApJ Lett., 23, 119 Google Scholar