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4.14. Molecular shell formation by supernova remnants in the Galactic center—what we learn from the case of W44

Published online by Cambridge University Press:  25 May 2016

Masumichi Seta ,
Gisbert Winnewisser ,
Tetsuo Hasegawa ,
Glenn J. White  and
Tomoharu Oka
Masumichi Seta
Affiliation:
Communications Research Laboratory, Nukui-kitamachi, Koganei, Tokyo 184, Japan
Gisbert Winnewisser
Affiliation:
I Physikalishes Institut, Universitaet zu Koeln, Zuelpicher Str. 77, 50937, Koeln, Germany
Tetsuo Hasegawa
Affiliation:
Institute of Astronomy, The University of Tokyo, Osawa, Mitaka, Tokyo 181, Japan
Glenn J. White
Affiliation:
Queen Mary Westfield College, London Univerisity, Mile End Road, London E1 4 NS, UK
Tomoharu Oka
Affiliation:
The Institute of Physical and Chemical Research (RIKEN), Wako, Saitama 351-01, Japan

Extract

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Recent high resolution CO images of the Galactic center (GC) molecular clouds reveal many arc and/or shell structures (Oka et al. 1997). A considerable fraction of them may most probably be formed by an interaction between supernova remnants (SNRs) and molecular clouds. Studies of such cases in less confused areas are needed to clarify this picture. The SNR W44 is a good place for examining the SNR induced shell formation scenario.

Type
Part II. Nuclear Interstellar Medium
Information
Symposium - International Astronomical Union , Volume 184: The Central Regions of the Galaxy and Galaxies , 1998 , pp. 195 - 196
Copyright
Copyright © Kluwer 1998 

References

Handa, T., Sofue, Y., Nakai, N., Hirabayashi, H. & Inoue, M. 1987, PASJ, 39.Google Scholar
Oka, T., Hasegawa, T., Hayashi, M., Handa, T., & Sakamoto, S. 1997, ApJ, in press.Google Scholar
Seta, M., Hasegawa, T., Dame, T.M., Sakamoto, S. Oka, T. Handa, T., Hayashi, M., Morino, J.-I., Sorai, I. & Usuda, S. K., ApJ, submitted.Google Scholar