漂移、调制和零化：脉冲星B1918 +19的另一种观察
Drifting, moding, and nulling: another look at pulsar B1918+19
摘要：
本文利用阿雷西博对锥形三重脉冲星B1918+19在0.327和1.4 GHz的观测，详细分析了它的次脉冲行为。我们确认存在三种不同的漂移模式（A，B，C）加上无序模式（N），并表明它们在特定的周期中相互跟随。解释脉冲星的轮廓，从视线穿越切割外锥和切向擦过内锥，我们证明了内锥的相位调制锁定在所有的漂移模式的外锥的振幅调制。9%的零被发现主要局限于占主导地位的B和N模式，并在N模式，创建交替串的零和发射的准周期性的方式与约12个旋转周期（$P_1$）的平均波动率。我们探讨的假设，即明显的漂移是第一个别名的更快的漂移的子光束周围的锥体等间距。这表明意味着所有模式A、B和C具有12 $P_1$的共同循环时间，并且仅在子束的数量上不同。该时间尺度与经典的{ \bf E} $\times$ { \bf B}漂移预测的量级相同，并且也与N模式调制一致。因此，我们得到一幅图，其中循环速度大致保持不变，而子光束的数量从模式A到B到C逐渐减少，然后在N模式期间重新建立。我们认为，混叠与子束损失相结合，可能是负责明显的戏剧性变化的漂移率，在其他激光器。
英文摘要：
Arecibo observations of the conal triple pulsar B1918+19 at 0.327- and 1.4-GHz are used to analyse its subpulse behaviour in detail. We confirm the presence of three distinct drift modes (A,B,C) plus a disordered mode (N) and show that they follow one another in specific cycles. Interpreting the pulsar's profile as resulting from a sightline traverse which cuts across an outer cone and tangentially grazes an inner cone, we demonstrate that the phase modulation of the inner cone is locked to the amplitude modulation of the outer cone in all the drift modes. The 9% nulls are found to be largely confined to the dominant B and N modes, and, in the N mode, create alternating bunches of nulls and emission in a quasi-periodic manner with an averaged fluctuation rate of about 12 rotation periods ($P_1$). We explore the assumption that the apparent drift is the first alias of a faster drift of subbeams equally spaced around the cones. This is shown to imply that all modes A, B and C have a common circulation time of 12 $P_1$ and differ only in the number of subbeams. This timescale is on the same order as predicted by the classic {\bf E}$\times${\bf B} drift and also coincides with the N-mode modulation. We therefore arrive at a picture where the circulation speed remains roughly invariant while the subbeams progressively diminish in number from modes A to B to C, and are then re-established during the N mode. We suggest that aliasing combined with subbeam loss may be responsible for apparently dramatic changes in drift rates in other pulsars.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
