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Optical study of pulsars (Optical photometry).

机译：脉冲星的光学研究（光学测光）。

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摘要

The Crab Pulsar emits radiation at all wavelengths from radio to extreme γ-rays including the optical. We have performed extremely high time resolution multicolor photometry of the Crab Pulsar at optical wavelengths to constrain the high energy emission models for pulsars. Our observations with 1 microsecond time resolution are a factor of 20 better than the previous best observations.; We have completely resolved the peak of the main pulse of the Crab Pulsar in optical passbands. The peaks of the main pulse and the interpulse move smoothly from the rising branch to the falling branch with neither a flat top nor a cusp. We find that the peak of the Crab Pulsar main pulse in the B band arrives 140 microseconds before the peak of the radio pulse.; The color of the emission changes across the phase. The maximum variation in the color ratio is about 25%. The bluest color occurs in the bridge region between the main pulse and the interpulse. The Crab Pulsar has faded by 2 ± 2.8% since the previous observations in 1991 using the same instrument.; The statistics of photon arrival times are consistent with atmospheric scintillation causing most of the variations in addition to the mean pulse variations in the shape. However, the autocorrelation function (ACF) of the Crab Pulsar light curve shows extra correlations at very short time scales. We identify two time scales, one at about 20 microseconds and another one at about 1000 microseconds at which we observe a break in the ACF. We conclude that these short timescale correlations are internal to the pulsar.; We attribute the extra correlation observed in our data to microstructures. This is the first time evidence for microstructures has been observed outside the radio wavelengths. The upturn in the ACF at short time scales depends on the color. The U band shows about 10% more correlation at short time scales while the R band shows only about 3% change.; We have also observed the young X-ray pulsar PSR 0656+14 at optical wavelengths. We do not detect any periodicity at the radio pulsar period up to a limiting magnitude of about 26.5.
机译：蟹状脉冲星发出的所有波长的辐射都从无线电到极端的γ射线，包括光学射线。我们对蟹形脉冲星在光学波长上进行了极高的时间分辨率多色光度法，以限制脉冲星的高能发射模型。我们具有1微秒时间分辨率的观察结果比以前的最佳观察结果高20倍。我们已经完全解决了光学通带中螃蟹脉冲星主脉冲的峰值。主脉冲和互脉冲的峰值从上升分支到下降分支平稳地移动，顶部既不平坦，也不尖。我们发现，B波段蟹状脉冲星主脉冲的峰值在无线电脉冲的峰值之前140微秒到达。发射的颜色在整个相中变化。颜色比率的最大变化约为25％。最蓝的颜色出现在主脉冲和互脉冲之间的桥接区域中。自从1991年以前使用同一仪器观测以来，螃蟹脉冲星已经衰减了2±2.8％。光子到达时间的统计与大气闪烁一致，除了形状中的平均脉冲变化外，还会引起大多数变化。但是，蟹状脉冲星光曲线的自相关函数（ACF）在非常短的时间尺度上显示出额外的相关性。我们确定了两个时间尺度，一个在大约20微秒，另一个在大约1000微秒，观察到ACF中断。我们得出结论，这些短时标相关性是脉冲星内部的。我们将数据中观察到的额外相关性归因于微观结构。这是首次在无线电波长之外观察到微结构的证据。在短时间内，ACF的上升取决于颜色。 U波段在短时间尺度上显示出约10％的相关性，而R波段仅显示约3％的变化。我们还观察到了在光学波长下的年轻X射线脉冲星PSR 0656 + 14。我们没有在无线电脉冲星周期检测到任何周期性，直到大约26.5的极限幅度。

著录项

  • 作者

    Sanwal, Divas.;

  • 作者单位

    The University of Texas at Austin.;

  • 授予单位 The University of Texas at Austin.;
  • 学科 Physics Astronomy and Astrophysics.
  • 学位 Ph.D.
  • 年度 1999
  • 页码 139 p.
  • 总页数 139
  • 原文格式 PDF
  • 正文语种 eng
  • 中图分类 天文学;
  • 关键词

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