脉冲星B0943 +10 -- VI的束流拓扑和动态发射特性。'Q'模式前兆的发现以及与脉冲星B1822-09的比较
The beam topology and dynamic emission properties of pulsar B0943+10 -- VI. Discovery of a 'Q'-mode precursor and comparison with pulsar B1822-09
摘要：
本文报道了Arecibo天文台（AO）和巨米波射电望远镜（GMRT）对双星B 0943 +10和B1822- 09的新观测结果。这两颗恒星都有两种稳定的发射模式。我们报告发现在B 0943 +10的高度线性偏振的前体成分，主要发生在只有一个模式。这种发射特征非常类似于B1822-09的前体，它也只在一种模式下明亮地出现。B 0943 +10的另一个模式以其高度规则的漂移子脉冲而闻名，这些子脉冲显然是由20个细光束的旋转传送带系统产生的。类似地，B1822-09仅在其前体不存在的模式下表现出子脉冲调制行为。我们调查我们的18个小时的B 0943 +10观测，发现边带调制功能，从旋转木马旋转时间可以直接确定，很少发生-不到5%的时间-但总是指示20束。我们提出了一个分析B1822-09的模式调制特性在325 MHz，并详细比较它们与B 0943 +10。脉冲星似乎从来没有零，我们发现一个43旋转周期的功能，在恒星的Q模式，调制脉冲间以及圆锥功能的主脉冲。我们的结论是，B1822-09必须有一个近乎正交的几何形状，它的旋转木马循环时间是长的相比，在我们的观测模态子序列，和主脉冲/脉冲间的分离几乎正好是180度。我们得出结论，这两颗星的前兆是不相容的核心锥发射。我们评估了Dyks等人提出的有趣的建议，即向下辐射产生B1822-09的前体发射。
英文摘要：
This paper reports new observations of pulsars B0943+10 and B1822--09 carried out with the Arecibo Observatory (AO) and the Giant Metrewave Radio Telescope (GMRT), respectively. Both stars exhibit two stable emission modes. We report the discovery in B0943+10 of a highly linearly polarized precursor component that occurs primarily in only one mode. This emission feature closely resembles B1822-09's precursor which also occurs brightly in only one mode. B0943+10's other mode is well known for its highly regular drifting subpulses that are apparently produced by a rotating carousel system of 20 beamlets. Similary, B1822-09 exhibits subpulse-modulation behavior only in the mode where its precursor is absent. We survey our 18 hours of B0943+10 observations and find that the sideband-modulation features, from which the carousel-rotation time can be directly determined, occur rarely--less than 5% of the time--but always indicating 20 beamlets. We present an analysis of B1822-09's modal modulation characteristics at 325-MHz and compare them in detail with B0943+10. The pulsar never seems to null, and we find a 43-rotation-period feature in the star's Q mode that modulates the interpulse as well as the conal features in the main pulse. We conclude that B1822-09 must have a nearly orthogonal geometry and that its carousel circulation time is long compared to the modal sub-sequences available in our observations, and the mainpulse/interpulse separation is almost exactly 180 degrees. We conclude the precursors for both stars are incompatible with core-cone emission. We assess the interesting suggestion by Dyks et al. that downward-going radiation produces B1822-09's precursor emission.
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