arXiv 1904.017652019-04astro-ph.HE

Gamma-Ray脉冲星的一个基平面

A Fundamental Plane for Gamma-Ray Pulsars

Constantinos Kalapotharakos, Alice K. Harding, Demosthenes Kazanas, Zorawar Wadiasingh

备注：: 8 pages, 6 figures, accepted for publication in ApJL
DOI：: 10.3847/2041-8213/ab3e0a

摘要：

我们表明，$γ$射线脉冲星观测，即，它们的总$γ$射线光度$L_γ$、光谱截止能量$ε_{\rm cut}$、恒星表面磁场$B_{\star}$和自旋下降功率$\dot{\mathcal{E}}$服从$L_γ=f(ε_{\rm cut},B_{\star},\dot{\mathcal{E}})$形式的关系，该关系表示它们的4D对数空间中的3D平面。通过对第二个费米脉冲星星表中88颗脉冲星数据的拟合，我们证明了这种关系是脉冲星基平面（FP）的关系$L_γ\propto ε_{\rm cut}^{1.18\pm 0.24}B_{\star}^{0.17\pm 0.05}\dot{\mathcal{E}}^{0.41\pm 0.08}$。我们发现，所观察到的FP是非常接近的理论关系$L_γ\propto ε_{\rm cut}^{4/3}B_{\star}^{1/6}\dot{\mathcal{E}}^{5/12}$得到假设脉冲星$γ$射线发射是由于曲率辐射粒子加速在脉冲星赤道电流片外面的光柱。有趣的是，FP似乎与同步辐射发射不相容。对应的FP的散射是$\sim 0.35$ dex，只能部分地由观测误差解释，而其余的可能是由于倾角和观测者角度的变化。我们还预测，年轻和毫秒双星的$ε_{\rm cut}\propto \dot{\mathcal{E}}^{7/16}$都趋向于低$\dot{\mathcal{E}}$，这意味着观测到的$γ$射线双星的死亡线是由于$ε_{\rm cut}$下降到费米带以下。我们的结果提供了一个全面的解释$γ$射线天体的观测，成功的理论建模设置的要求。

英文摘要：

We show that the $γ$-ray pulsar observables, i.e., their total $γ$-ray luminosity, $L_γ$, spectral cut-off energy, $ε_{\rm cut}$, stellar surface magnetic field, $B_{\star}$, and spin-down power $\dot{\mathcal{E}}$, obey a relation of the form $L_γ=f(ε_{\rm cut},B_{\star},\dot{\mathcal{E}})$, which represents a 3D plane in their 4D log-space. Fitting the data of 88 pulsars of the second Fermi pulsar catalog, we show this relation to be $L_γ\propto ε_{\rm cut}^{1.18\pm 0.24}B_{\star}^{0.17\pm 0.05}\dot{\mathcal{E}}^{0.41\pm 0.08}$, a pulsar fundamental plane (FP). We show that the observed FP is remarkably close to the theoretical relation $L_γ\propto ε_{\rm cut}^{4/3}B_{\star}^{1/6}\dot{\mathcal{E}}^{5/12}$ obtained assuming that the pulsar $γ$-ray emission is due to curvature radiation by particles accelerated at the pulsar equatorial current sheet just outside the light cylinder. Interestingly, the FP seems incompatible with emission by synchrotron radiation. The corresponding scatter about the FP is $\sim 0.35$dex and can only partly be explained by the observational errors while the rest is probably due to the variation of the inclination and observer angles. We predict also that $ε_{\rm cut}\propto \dot{\mathcal{E}}^{7/16}$ toward low $\dot{\mathcal{E}}$ for both young and millisecond pulsars implying that the observed death-line of $γ$-ray pulsars is due to $ε_{\rm cut}$ dropping below the Fermi-band. Our results provide a comprehensive interpretation of the observations of $γ$-ray pulsars, setting requirement for successful theoretical modeling.

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