Physics of pulsar radio emission outside of the main pulse
S. A. Petrova
备注：
4 pages, no figures. To appear in the Proceedings of the Low-Frequency Radio Universe Conference held at NCRA-TIFR, Pune, 8-12 December 2008, eds. D.J. Saikia, D. Green, Y. Gupta, and T. Venturi
We for the first time propose a physical model of the precursor (PR) and interpulse (IP) components of the radio pulsar profiles. It is based on propagation effects in the secondary plasma flow of a pulsar. The components are suggested to result from the induced scattering of the main pulse (MP) into background. The induced scattering appears efficient enough to transfer a significant part of the MP energy to the background radiation. In the regimes of superstrong and moderately strong magnetic field, the scattered components are approximately parallel and antiparallel to the velocity of the scattering particles and can be identified with the PR and IP, respectively. The spectral evolution, polarization properties, and fluctuation behaviour of the scattered components are examined and compared with the observational results. The perspectives of the complex profile studies are outlined as well.
Scintillation based search for off-pulse radio emission from pulsars
我们提出了一种新的方法来检测关闭脉冲（非脉冲和/或连续）发射的恒星，使用与星际闪烁的强度调制。我们的技术包括获得动态光谱，分别为脉冲窗口和脉冲区域，时间和频率分辨率，适当采样的强度变化，由于衍射闪烁，然后估计它们的相互关系作为衡量脉冲发射，如果有的话。我们描述和说明这种技术的基本细节的帮助下，模拟，以及真实的数据。我们还讨论了这种方法的优势，较早的方法来检测脉冲发射。特别是，我们指出如何测量设置固有的某些非理想性可能会影响早期方法的估计，并认为目前的技术是免疫这种非理想性。我们验证了上述两种情况与相关的模拟。我们应用这种方法观察PSR B 0329 +54在730和810 MHz的频率，与绿岸望远镜和目前的上限在这两个频率的关断脉冲强度。我们希望这种技术能够为广泛的调查关闭脉冲发射铺平道路，甚至现有的动态光谱数据的帮助下，当然，更敏感的长期数据，从新的观测。
