磁星快速射电暴的逃逸

Emanuele Sobacchi, Masanori Iwamoto, Lorenzo Sironi, Tsvi Piran
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摘要

快速射电暴(FRBs)是一种明亮的河外瞬变现象,很可能是由磁星产生的。我们研究了快速射电暴在磁星风中的传播,假设风是强磁化的,由电子-正电子对组成。我们重点研究了无线电波的强度参数$a_0$大于一,并且波的频率$\omega_0$大于背景磁场中的拉莫尔频率$\omega_{\rm L}$的情况。我们证明,当 $\omega_0 >a_0\omega_\{rm L}$ 时,由于等离子体电流是波电场的线性函数,所以 $a_0>1$ 的强无线电波能够传播。当 $\omega_0 > a_0\omega_{\rm L}$ 时,频散关系与波强参数无关。相反,当$\omega_0 < a_0\omega_\{rm L}$时,无线电波可能会被掩埋,因为相当一部分波能量被用来压缩等离子体和放大背景磁场。我们的研究结果表明,FRB应该是在距离磁星很远的地方产生的(即:$R>10^{12}{\rm\; cm}$,满足条件$\omega_0 >a_0\omega_{\rm L}$)。或者,磁星风的结构应该在耀斑期间发生强烈变化,以允许在半径$R<10^{12}{\rm\; cm}$时产生的FRB逃逸。
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Escape of fast radio bursts from magnetars
Fast radio bursts (FRBs) are bright extragalactic transients likely produced by magnetars. We study the propagation of FRBs in magnetar winds, assuming that the wind is strongly magnetized and composed of electron-positron pairs. We focus on the regime where the strength parameter of the radio wave, $a_0$, is larger than unity, and the wave frequency, $\omega_0$, is larger than the Larmor frequency in the background magnetic field, $\omega_{\rm L}$. We show that strong radio waves with $a_0>1$ are able to propagate when $\omega_0 > a_0\omega_{\rm L}$, as the plasma current is a linear function of the wave electric field. The dispersion relation is independent of the wave strength parameter when $\omega_0 > a_0\omega_{\rm L}$. Instead, radio waves could be damped when $\omega_0 < a_0\omega_{\rm L}$, as a significant fraction of the wave energy is used to compress the plasma and amplify the background magnetic field. Our results suggest that FRBs should be produced at large distances from the magnetar (i.e., $R>10^{12}{\rm\; cm}$, where the condition $\omega_0 > a_0\omega_{\rm L}$ is satisfied). Alternatively, the structure of the magnetar wind should be strongly modified during a flare to allow the escape of FRBs produced at radii $R<10^{12}{\rm\; cm}$.
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