STAR-FORMING DENSE CLOUD CORES IN THE TeV GAMMA-RAY SNR RX J1713.7−3946-猫眼课题宝

DOI：

10.1088/0004-637x/724/1/59

发表时间：

2010-05

期刊：

The Astrophysical Journal

影响因子：

通讯作者：

中科院分区：

其他

文献类型：

作者：

H. Sano;J. Sato;H. Horachi;N. Moribe;H. Yamamoto;T. Hayakawa;K. Torii;A. Kawamura;T. Okuda;N. Mizuno;T. Onishi;H. Maezawa;T. Inoue;S. Inutsuka;T. Tanaka;H. Matsumoto;A. Mizuno;H. Ogawa;J. Stutzki;F. Bertoldi;S. Anderl;L. Bronfman;B. Koo;M. Burton;A. Benz;Y. Fukui

RX J1713.7−3946是发射同步辐射X射线的γ超新星残骸之一。信噪比与位于∼1kpc的分子气体有关。我们在角分辨率为90“的12CO(J=2-1)和13CO(J=2-1)跃迁的SNR中对致密云核A、C和D进行了新的分子观测。在角分辨率为38“的12Co(J=4-3)跃迁中，也出现了最强的~(13)CO核，即C峰。峰C显示出强烈的活动恒星形成的迹象，包括双极外流和远红外原星源，并且具有陡峭的梯度，在半径r内的平均密度变化为rSNR2.2±0.4.在同步辐射X射线中，峰C和其他致密云核的边缘变亮，表明致密云核嵌入在−壳层的外部边界之内或之上.这证实了早先的观点，即X射线在物理上与分子气体有关。我们提出了一种情况，其中最密集的分子核心，峰C，在爆炸波中幸存下来，现在嵌入到SNR中。激波-云团相互作用的数值模拟表明，由于激波传播速度在致密团块中停滞，致密团块确实可以在激波侵蚀中幸存下来。此外，激波-云相互作用在致密核周围引起湍流和磁场放大，这可能有助于粒子在较低密度的簇间空间中加速，从而在致密核周围产生增强的同步辐射X射线。

RX J1713.7−3946 is one of the TeV γ-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 an angular resolution of 90″. The most intense core in 13CO, peak C, was also mapped in the 12CO(J = 4–3) transition at an 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±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. We present a scenario where the densest molecular core, peak C, survived 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 the 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 enhanced synchrotron X-rays around dense cores.

STAR-FORMING DENSE CLOUD CORES IN THE TeV GAMMA-RAY SNR RX J1713.7−3946

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