X-Ray Synchrotron Emission from 10-100 TeV Cosmic-Ray Electrons in the Supernova Remnant SN 1006
X-Ray Synchrotron Emission from 10-100 TeV Cosmic-Ray Electrons in the Supernova Remnant SN 1006
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DOI：
10.1086/322470
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发表时间：
2001-07
期刊：
影响因子：
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通讯作者：
G. Allen;R. Petre;E. Gotthelf
中科院分区：
文献类型：
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作者：
G. Allen;R. Petre;E. Gotthelf
我们给出了超新星遗迹SN1006的RXTE PCA、ASCA SIS和ROSAT PSPC数据的联合光谱分析结果。这项工作是第一次尝试对从0.12到17keV整个X射线能带上的热和非热X射线发射进行建模。热流符合非平衡电离模型，电子温度kte=0.6keV，电离时间n0t=9×10~9 cm~(-3)S，硅的相对元素丰度是太阳丰度的10-18倍。低能光子指数Γ1=2.1，高能光子指数Γ2=3.0的非热X射线谱符合破缺幂定律模型。由于非热X射线谱随能量的增加而变陡，本文的分析结果证实了以前的说法，即非热X射线发射是由同步辐射产生的。我们认为磁场强度比以前估计的约10μG要大得多，并任意使用40μG的值来估计残余物的宇宙射线电子、质子和氦光谱参数。质子和电子数密度比(1GeV时R=160时)、宇宙线总能量(ECR=1×1050ergs)和1GeV处电子的谱指数(Γe=2.14±0.12)的结果与银河系宇宙线主要在超新星残骸的激波中加速的假设一致。然而，残余物可能会也可能不会将原子核加速到“膝盖”能量那么高的能量，这取决于电子的最大能量只有10TeV的原因。
We present the results of a joint spectral analysis of RXTE PCA, ASCA SIS, and ROSAT PSPC data of the supernova remnant SN 1006. This work represents the first attempt to model both the thermal and nonthermal X-ray emission over the entire X-ray energy band from 0.12 to 17 keV. The thermal flux is described by a nonequilibrium ionization model with an electron temperature kTe = 0.6 keV, an ionization timescale n0t = 9 × 109 cm-3 s, and a relative elemental abundance of silicon that is 10-18 times larger than the solar abundance. The nonthermal X-ray spectrum is described by a broken power law model with low- and high-energy photon indices Γ1 = 2.1 and Γ2 = 3.0, respectively. Since the nonthermal X-ray spectrum steepens with increasing energy, the results of the present analysis corroborate previous claims that the nonthermal X-ray emission is produced by synchrotron radiation. We argue that the magnetic field strength is significantly larger than previous estimates of about 10 μG and arbitrarily use a value of 40 μG to estimate the parameters of the cosmic-ray electron, proton, and helium spectra of the remnant. The results for the ratio of the number densities of protons and electrons (R = 160 at 1 GeV), the total energy in cosmic rays (Ecr = 1 × 1050 ergs), and the spectral index of the electrons at 1 GeV (Γe = 2.14 ± 0.12) are consistent with the hypothesis that Galactic cosmic rays are accelerated predominantly in the shocks of supernova remnants. Yet, the remnant may or may not accelerate nuclei to energies as high as the energy of the "knee," depending on the reason why the maximum energy of the electrons is only 10 TeV.