Seta, Masumichi; Winnewisser, Gisbert; Hasegawa, Tetsuo; White, Glenn J. and Oka, Tomoharu
Due to copyright restrictions, this file is not available for public download
|Google Scholar:||Look up in Google Scholar|
Recent high resolution CO images of the Galactic center (GC) molecular clouds reveal many arc and/or shell structures. 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. Our study of the SNR W44 supports this SNR-induced shell formation scenario in the GC. By using the Tokyo-NRO 60-cm survey telescope, the 45-m telescope at Nobeyama,and the 15-m JCMT on Mauna Kea, we established that W44 is the first unambiguous example of interaction between a SNR and giant molecular clouds. Our millimeter and submillimeter observations revealed that the SNR changed the surface of the giant molecular clouds into filaments of shocked molecular gas. They run perpendicular to the direction of the SNR expansion. Sequential interactions between SNRs and the molecular cloud which are expected in the GC may further form these molecular filaments into networks, which are observed as shell/arc structures often made of high density molecular gas.
|Item Type:||Conference Item|
|Copyright Holders:||1998 IAU|
|Extra Information:||The central regions of the Galaxy and galaxies,
Proceedings of the 184th symposium of the International Astronomical Union, held in Kyoto, Japan, August 18-22, 1997.
Edited by Yoshiaki Sofue.
Dordrecht: Kluwer, 1998.
|Academic Unit/Department:||Science > Physical Sciences|
|Interdisciplinary Research Centre:||Centre for Earth, Planetary, Space and Astronomical Research (CEPSAR)|
|Depositing User:||Glenn White|
|Date Deposited:||08 Mar 2012 14:35|
|Last Modified:||11 May 2012 17:08|
Actions (login may be required)
|Report issue / request change|