We discuss $γ$-ray emissions from the outer gap accelerators of middle-aged pulsars for part of the series of our studies. A two-dimensional electrodynamic model is used to solve the distribution of accelerating electric fields with electron and positron pair creation and radiation processes in the magnetic meridional plane. We compute the curvature radiation and the synchrotron radiation by solving the evolution of the Lorentz factor and the pitch angle. The calculated spectra are compared with observed phase-averaged spectra. We also use a three-dimensional geometrical model to discuss the pulse profiles. We argue that the outer gap of middle-aged pulsars occupies the whole region between the last-open field lines and the critical magnetic field lines, which are perpendicular to the rotational axis at the light cylinder. We assume that there is no outer gap accelerator inside the light cylinder between the rotational axis and the critical magnetic field lines. For the Geminga pulsar, we demonstrate that the outward curvature radiation dominates in the spectrum above 10 MeV, while the inward synchrotron radiation dominates below 10 MeV. We find that the computed spectrum is consistent with the observations in X-ray through $γ$-ray bands. With the pulse morphology of the $γ$-ray emissions, we argue that the inclination angle and the viewing angle for the Geminga pulsar are $α\sim 50^{\circ}$ and $ξ\sim 90^{\circ}$, respectively.
Subaru optical observations of the two middle-aged pulsars PSR B0656+14 and Geminga
我们对这两颗中年恒星进行了深亚角秒BRI成像，以确定它们在光学范围内的特性。两种干扰都在>10 sigma水平下检测到。Geminga是第一次在I波段被可靠地探测到，震级为25.10+/-0.14。我们还重新分析档案ESO/NTT和HST宽带数据，发现一些公布的Geminga通量估计不准确。结果表明，这两颗双星的去红宽带光谱非常相似，并且在远紫外和近红外波段有显著的通量增加，在V-I波段有很宽的通量过剩。这表明光发射的多组分结构。脉冲星磁层起源的非热幂律分量在光学范围的大部分占主导地位。对于PSR B 0656 +14，它与硬X射线中看到的幂律尾部的低能扩展兼容。对于Geminga，相应的扩展超过了非热光通量的100倍，这比X射线的光谱斜率要小。这意味着在约IkeV的光子能量处的光谱断裂。远紫外辐射通量的增加与中子星整个表面黑体辐射中瑞利-金斯部分的贡献是一致的。PSR B 0656 +14中最显著的V-I过量表明第三种光谱成分的来源仍未确定。在我们最深的I波段图像中，在两个天体周围都可以看到垂直于双星自行方向延伸的微弱的、几角秒大小的星云。它们可能是Geminga弓形激波头和PSR B 0656 +14脉冲星风星云的光学对应物。
X-ray Observations of Parsec-Scale Tails behind Two Middle-Aged Pulsars
Chandra and XMM-Newton resolved extremely long tails behind two middle-aged pulsars, J1509-5850 and J1740+1000. The tail of PSR J1509-5850 is discernible up to 5.6' from the pulsar (6.5 pc at a distance of 4 kpc), with a flux of 2*10^{-13} erg s^{-1} cm^{-2} in 0.5-8 keV. The tail spectrum fits an absorbed power-law (PL) model with the photon index of 2.3 \pm 0.2, corresponding to the 0.5-8 keV luminosity of 1*10^{33} ergs s^{-1}, for n_H= 2.1*10^{22} cm^{-2}. The tail of PSR J1740+1000 is firmly detected up to 5' (2 pc at a 1.4 kpc distance), with a flux of 6*10^{-14} ergs cm^{-2} s^{-1} in 0…
BVRI observations of PSR B0656+14 with the 6-meter telescope
在6米望远镜上用CCD探测器观测了中年射电脉冲星0656+14。宽带BVRI图像显示了脉冲星对应物的以下星等：B = 24.85（+0.19，-0.16），V = 24.90（+0.16，-0.14），R = 24.52（+0.12，-0.11），I = 23.81（+0.27，-0.21）。我们拟合的紫外光（空间+地面）数据与两个组件的模型，结合了幂律（非热分量）与热光谱发射的中子星表面。能量幂律指数α=1.5（+1.1，-1.2）的幂律分量在观测范围内占主导地位。热分量上的约束对应于瑞利-金斯参数G \equiv T_6（R_{10} / d_{500}）^2=4.1（+2.1，-4.1），其中$T=10^6T_6$ K是亮度温度，R_ \infty = 10 R_{10} $ km is the neutron star radius as seen by a distant observer, and $ d=500 d_{500} $ pc是距离。PSR 0656+14的紫外光谱的形状与从其他哺乳动物中观察到的有很大的不同：中年的Geminga和年轻的Crab，Vela。
本文介绍了对中年射电脉冲星PSR B 0355 +54的XMM-牛顿和钱德拉X射线观测。我们的X射线观测揭示了发射不仅来自脉冲星本身，而且来自一个紧凑的扩散分量，该分量在脉冲星自行的相反方向上延伸约50“。也有证据表明存在从点源延伸~5'的较弱的漫射发射。紧凑的弥漫功能是很好的拟合幂律，其中的指数是与其他脉冲星风星云的发现值一致。的扩散组件的形态是类似的冲压压力限制脉冲星风星云检测到的其他来源。来自脉冲星本身的X射线辐射可以用热辐射加幂律拟合来描述，热辐射很可能起源于热的极冠。
