Star Forming Dense Cloud Cores in the TeV ��-ray SNR RX J1713.7-3946
| Autor: | Sano, H., Sato, J., Horachi, H., Moribe, N., Yamamoto, H., Hayakawa, T., Torii, K., Kawamura, A., Okuda, T., Mizuno, N., Onishi, T., Maezawa, H., Inoue, T., Inutsuka, S., Tanaka, T., Matsumoto, H., Mizuno, A., Ogawa, H., Stutzki, J., Bertoldi, F., Anderl, S., Bronfman, L., Koo, B. -C., Burton, M. G., Benz, A. O., Fukui, Y. |
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| Rok vydání: | 2010 |
| Předmět: | |
| DOI: | 10.48550/arxiv.1005.3409 |
| Popis: | RX J1713.7-3946 is one of the TeV ��-ray supernova remnants (SNRs) emitting synchrotron X rays. The SNR is associated with molecular gas located at ~1 kpc. We made new molecular observations toward the dense cloud cores, peaks A, C and D, in the SNR in the 12CO(J=2-1) and 13CO(J=2-1) transitions at angular resolution of 90". The most intense core in 13CO, peak C, was also mapped in the 12CO(J=4-3) transition at angular resolution of 38". Peak C shows strong signs of active star formation including bipolar outflow and a far-infrared protostellar source and has a steep gradient with a r^{-2.2$\pm$0.4} variation in the average density within radius r. Peak C and the other dense cloud cores are rim-brightened in synchrotron X rays, suggesting that the dense cloud cores are embedded within or on the outer boundary of the SNR shell. This confirms the earlier suggestion that the X rays are physically associated with the molecular gas (Fukui et al. 2003). We present a scenario where the densest molecular core, peak C, survived against the blast wave and is now embedded within the SNR. Numerical simulations of the shock-cloud interaction indicate that a dense clump can indeed survive shock erosion, since shock propagation speed is stalled in the dense clump. Additionally, the shock-cloud interaction induces turbulence and magnetic field amplification around the dense clump that may facilitate particle acceleration in the lower-density inter-clump space leading to the enhanced synchrotron X rays around dense cores. 22 pages, 7 figures, to accepted in The Astrophysical Journal. A full color version with higher resolution figures is available at http://www.a.phys.nagoya-u.ac.jp/~sano/ApJ10/ms_sano.pdf |
| Databáze: | OpenAIRE |
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