arXiv 0809.42812008-09astro-ph

超新星遗迹G330 .2+1.0的非热X射线及其中心致密天体的特征

Nonthermal X-Rays from Supernova Remnant G330.2+1.0 and the Characteristics of its Central Compact Object

Sangwook Park, Oleg Kargaltsev, George G. Pavlov, Koji Mori, Patrick O. Slane, John P. Hughes, David N. Burrows, Gordon P. Garmire

备注：: 26 pages, 3 tables, 7 figures (4 color figures), Accepted by ApJ
发表信息：: Astrophys.J.695:431-441,2009
DOI：: 10.1088/0004-637X/695/1/431

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摘要：

我们给出了SNR G330.2+1.0及其CCO CX160103.1--513353（J1601）的X射线数据分析结果。利用我们的XMM-Newton和Chandra观测结果，我们发现J1601的X射线谱可以用中子星大气模型（T ~ 2.5- 3.7 MK）来描述。假设J1601的距离d ~ 5 kpc，如SNR G330.2+1.0所估计的，则意味着R ~ 1- 2 km的小发射区域。钱德拉先前提出的X射线脉动没有得到XMM-牛顿数据的证实，并且可能不是真实的。然而，我们对XMM-牛顿数据的定时分析受到光子统计差的限制，因此具有相对低振幅的脉动（即，不能排除内在脉冲分数< 40%）。结果表明，J1601是一个类似于仙后座A SNR的CCO，SNR G330.2+1.0的X射线发射主要由幂律连续谱（γ ~ 2.1--2.5）组成，主要来源于沿边界壳层的细丝。这个X射线光谱意味着来自冲击加速电子的同步辐射，其指数滚降频率约为2- 3 x 10^17 Hz。对于测量的X射线细丝宽度（D ~ 0.3 pc）和估算的激波速度（v_s ~几× 10^3 km·s^-1），导出了下游磁场B ~ 10- 50 $μ$ G。最大电子能量E_（max）约为27- 38 TeV，表明G330.2+1.0可能是一个TeV的γ源。我们在G330.2+1.0中探测到微弱的热X射线发射。我们估计震前密度n_0很低，约为0.1 cm^-3，这表明逆康普顿机制（而不是质子-质子碰撞）对未来的伽马射线辐射有着主要贡献。后续的深射电、X射线和伽马射线观测对于揭示该SNR中冲击参数的细节和粒子加速的性质至关重要。

英文摘要：

We present results from our X-ray data analysis of the SNR G330.2+1.0 and its CCO, CXOU J160103.1--513353 (J1601). Using our XMM-Newton and Chandra observations, we find that the X-ray spectrum of J1601 can be described by neutron star atmosphere models (T ~ 2.5--3.7 MK). Assuming the distance of d ~ 5 kpc for J1601 as estimated for SNR G330.2+1.0, a small emission region of R ~ 1--2 km is implied. X-ray pulsations previously suggested by Chandra are not confirmed by the XMM-Newton data, and are likely not real. However, our timing analysis of the XMM-Newton data is limited by poor photon statistics, and thus pulsations with a relatively low amplitude (i.e., an intrinsic pulsed-fraction < 40%) cannot be ruled out. Our results indicate that J1601 is a CCO similar to that in the Cassiopeia A SNR.X-ray emission from SNR G330.2+1.0 is dominated by power law continuum (Gamma ~ 2.1--2.5) which primarily originates from thin filaments along the boundary shell. This X-ray spectrum implies synchrotron radiation from shock-accelerated electrons with an exponential roll-off frequency ~ 2--3 x 10^17 Hz. For the measured widths of the X-ray filaments (D ~ 0.3 pc) and the estimated shock velocity (v_s ~ a few x 10^3 km s^-1), a downstream magnetic field B ~ 10--50 $μ$G is derived. The estimated maximum electron energy E_max ~ 27--38 TeV suggests that G330.2+1.0 is a candidate TeV gamma-ray source. We detect faint thermal X-ray emission in G330.2+1.0. We estimate a low preshock density n_0 ~ 0.1 cm^-3, which suggests a dominant contribution from an inverse Compton mechanism (than the proton-proton collision) to the prospective gamma-ray emission. Follow-up deep radio, X-ray, and gamma-ray observations will be essential to reveal the details of the shock parameters and the nature of particle accelerations in this SNR.

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