arXivDaily arXiv每日学术速递 周一至周五更新
arXiv 1701.02554astro-ph.HE
收藏

脉冲星B1133 +16的XMM-牛顿观测

XMM-Newton observation of the nearby pulsar B1133+16

Andrzej Szary, Janusz Gil, Bing Zhang, Frank Haberl, George I. Melikidze, Ulrich Geppert, Dipanjan Mitra, Ren-Xin Xu

备注：
10 pages, 8 figuers, accepted for publication in ApJ
阅读 PDF
arXiv 页面 ↗HTML 原文 ↗

摘要：

用{ \it XMM-Newton}对附近的$(360\,{\rm pc})$，old（$5\,{\rm Myr}$）脉冲星B1133+16的X射线性质进行了约束，得到了$\sim 100\,{\rm ks}$的有效曝光时间.在0.2-3 keV能量范围内观测到的脉冲星通量为$\sim 10^{-14} \, {\rm erg \, cm}^{-2} \, {\rm s}^{-1}$，这导致EPIC pn和MOS探测器记录到$\sim 600$源计数。X射线辐射以非热辐射为主，可用单一的幂律模型（PL）和黑体与幂律辐射之和（BB+PL）来描述。BB+PL模型导致光谱光子指数$Γ=2.4^{+0.4}_{-0.3}$和$(7\pm 2) \times 10^{-15}\, {\rm erg \, cm}^{-2} \, {\rm s}^{-1}$的0.2-3 keV能量范围内的非热通量。热发射与半径为$R_{\rm pc} \approx 14^{+7}_{-5} \, {\rm m}$、温度为$T_{\rm s} = 2.9^{+0.6}_{-0.4} \, {\rm MK}$的小热点的黑体发射一致。假设热点对应于脉冲星的极帽，我们可以利用磁通量守恒定律来估计表面$B_{\rm s} \approx 3.9 \times 10^{14} \, {\rm G}$的磁场。观测结果与部分屏蔽间隙模型的预测吻合得很好，该模型假设极帽区域存在小尺度的表面磁场结构。

英文摘要：

We constrain the X-ray properties of the nearby $(360\,{\rm pc})$, old ($5\,{\rm Myr}$) pulsar B1133+16 with $\sim 100\,{\rm ks}$ effective exposure time by {\it XMM-Newton}. The observed pulsar flux in the 0.2-3 keV energy range is $\sim 10^{-14} \, {\rm erg \, cm}^{-2} \, {\rm s}^{-1}$, which results in the recording of $\sim 600$ source counts with the EPIC pn and MOS detectors. The X-ray radiation is dominated by nonthermal radiation and is well described by both a single power-law model (PL) and a sum of blackbody and power-law emission (BB+PL). The BB+PL model results in a spectral photon index $Γ=2.4^{+0.4}_{-0.3}$ and a nonthermal flux in the 0.2-3 keV energy range of $(7\pm 2) \times 10^{-15}\, {\rm erg \, cm}^{-2} \, {\rm s}^{-1}$. The thermal emission is consistent with the blackbody emission from a small hot spot with a radius of $R_{\rm pc} \approx 14^{+7}_{-5} \, {\rm m}$ and a temperature of $T_{\rm s} = 2.9^{+0.6}_{-0.4} \, {\rm MK}$. Assuming that the hot spot corresponds to the polar cap of the pulsar, we can use the magnetic flux conservation law to estimate the magnetic field at the surface $B_{\rm s} \approx 3.9 \times 10^{14} \, {\rm G}$. The observations are in good agreement with the predictions of the partially screened gap model, which assumes the existence of small-scale surface magnetic field structures in the polar cap region.

机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。

↑