论文标题
旋转驱动的脉冲星无线电发射机制
A rotation-driven pulsar radio emission mechanism
论文作者
论文摘要
我们提出并讨论了一种依赖于旋转驱动的等离子体振荡的替代脉冲星无线电发射机制，而不是梁驱动的不稳定性，并建议它可能是脉冲星的通用无线电发射机制。我们将这些振荡识别为Pulsar血浆中的静脉纵向波，并指出这些波可以在O〜模式下直接逸出。我们认为，振荡的频率为$ω_0\ ofcom {\ rm p}（2 \langleγ\ rangle）^{1/2}/γ_ {\ rm s} $，其中$γ_ {\ rm s} $是lorentz; is is $ iss $ iss $ is $ is Mortion;在等离子体的其余框架中的洛伦兹因子。等离子体频率$ω_ {\ rm p} $对径向距离的依赖性意味着特定的频到radius映射，$ω_0\ propto r^{ - 3/2} $。如果能量在我们称为纤维的过度密集，野外对齐的区域中产生，则可以逃脱这些振荡。波能最初被折射成纤维之间的不足区域，这些区域充当导管。讨论了该模型对脉冲星无线电发射解释的某些含义。
We propose and discuss an alternative pulsar radio emission mechanism that relies on rotation-driven plasma oscillations, rather than on a beam-driven instability, and suggest that it may be the generic radio emission mechanism for pulsars. We identify these oscillations as superluminal longitudinal waves in the pulsar plasma, and point out that these waves can escape directly in the O~mode. We argue that the frequency of the oscillations is $ω_0\approxω_{\rm p}(2\langleγ\rangle)^{1/2}/γ_{\rm s}$, where $γ_{\rm s}$ is the Lorentz factor of bulk streaming motion and $\langleγ\rangle$ is the mean Lorentz factor in the rest frame of the plasma. The dependence of the plasma frequency $ω_{\rm p}$ on radial distance implies a specific frequency-to-radius mapping, $ω_0\propto r^{-3/2}$. Escape of the energy in these oscillations is possible if they are generated in overdense, field-aligned regions that we call fibers; the wave energy is initially refracted into underdense regions between the fibers, which act as ducts. Some implications of the model for the interpretation of pulsar radio emission are discussed.
