了解几何和旋转对脉冲星强度剖面的影响
Understanding the effects of geometry and rotation on pulsar intensity profiles
摘要：
考虑观测几何和中子星的旋转效应，我们发展了一种计算典型脉冲星磁层射电辐射区可能分布的方法。对于给定的倾角、碰撞角、自旋周期、洛伦兹因子、磁力线常数和观测频率，我们的方法可以估算出发射高度和粒子轨道的曲率半径。此外，使用曲率辐射作为基本的发射机制，我们模拟的无线电强度分布，将观察到从一个给定的发射区域的分布，对于不同的值的射频和洛伦兹因子。我们清楚地表明，旋转效应可以引入显着的不对称性所观察到的无线电配置文件。我们调查的依赖性的轮廓特征上的各种脉冲星参数。我们发现，从一个给定的环场线的辐射可以看到在一个大范围的脉冲宽度，起源于不同的海拔高度，具有不同的光谱强度。沿离散的场线发射的优选高度需要再现现实的脉冲星配置文件，我们说明了这一点为一个已知的脉冲星。最后，我们展示了我们的模型是如何为核心发射的起源提供可行的解释，也为在一些恒星中观察到的单侧锥提供了可行的解释。
英文摘要：
We have developed a method to compute the possible distribution of radio emission regions in a typical pulsar magnetosphere, taking into account the viewing geometry and rotational effects of the neutron star. Our method can estimate the emission altitude and the radius of curvature of particle trajectory as a function of rotation phase for a given inclination angle, impact angle, spin-period, Lorentz factor, field line constant and the observation frequency. Further, using curvature radiation as the basic emission mechanism, we simulate the radio intensity profiles that would be observed from a given distribution of emission regions, for different values of radio frequency and Lorentz factor. We show clearly that rotation effects can introduce significant asymmetries into the observed radio profiles. We investigate the dependency of profile features on various pulsar parameters. We find that the radiation from a given ring of field lines can be seen over a large range of pulse longitudes, originating at different altitudes, with varying spectral intensity. Preferred heights of emission along discrete sets of field lines are required to reproduce realistic pulsar profiles, and we illustrate this for a known pulsar. Finally, we show how our model provides feasible explanations for the origin of core emission, and also for one-sided cones which have been observed in some pulsars.
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