LS I +61 ° 303的GeV发射周期的明显不连续性
The apparent discontinuity in the periodicity of the GeV emission from LS I +61°303
摘要：
LS I +61 ° 303的γ射线双星在其GeV辐射中表现出周期性的不连续性。在本文中，我们表明，在历元的定时分析未能确定的轨道周期性，周期性实际上是存在于两个轨道相位间隔$Φ= 0.0-0.5$和$Φ= 0.5-1.0$。也就是说，存在两个周期性信号，一个朝向近星点（即，$Φ= 0.0-0.5$）和另一个朝向远望子（$Φ= 0.5-1.0$）。这幅远日子的峰值显示了与射电爆发相同的轨道位移，此外，还显示了射电数据中存在的相同的两个周期$P_1$和$P_2$。在正常情况下，近星点峰值的伽马射线辐射只是加宽了近星点附近峰值的辐射。只有当它出现在$Φ= 0.8-1.0$时，由于轨道移动，它才与第一个峰分离得足够远，从而变得可识别为第二个轨道峰，这是时序分析失败的原因。几位作者针对LS I +61°303提出的偏心轨道双峰吸积模型预测了沿轨道的两个伽马射线峰。
英文摘要：
The gamma-ray binary LS I +61°303 shows a discontinuity of the periodicity in its GeV emission. In this paper, we show that during the epochs when the timing analysis fails to determine the orbital periodicity, the periodicity is in fact present in the two orbital phase intervals $Φ= 0.0-0.5$ and $Φ= 0.5-1.0$. That is, there are two periodic signals, one towards periastron (i.e., $Φ= 0.0-0.5$) and another one towards apastron ($Φ= 0.5-1.0$). The apastron peak shows the same orbital shift as the radio outburst and, in addition, reveals the same two periods $P_1$ and $P_2$ that are present in the radio data. The gamma-ray emission of the apastron peak normally just broadens the emission of the peak around periastron. Only when it appears at $Φ= 0.8-1.0$, because of the orbital shift, it is detached enough from the first peak to become recognizable as a second orbital peak, which is the reason why the timing analysis fails. Two gamma-ray peaks along the orbit are predicted by the two-peak accretion model for an eccentric orbit that was proposed by several authors for LS I +61°303.
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