论文标题
与Elwa一起发现B0950+08周围的脉冲星云状星云
Discovery of a Pulsar Wind Nebula around B0950+08 with the ELWA
论文作者
论文摘要
随着扩展的长波长阵列（ELWA）和PULSAR binning技术，我们在76 MHz时搜索了PSR B0950+08的脉冲发射。先前的研究表明，脉冲发射可能是由于年轻脉冲星的脉冲星风云（pwne）。其他研究，例如Basu等人进行的研究。 （2012年），建议在较旧的脉冲星中，这种发射延伸至在光缸半径上的一定半径，并且是磁层的。通过成像分析，我们得出的结论是，这个年龄较低的年龄为17岁的pulsar周围有一个周围的PWN，这是出乎意料的，因为随着脉冲星的年龄，其PWN频谱被认为从同步转移到逆向compton-scatton的主导。在76 MHz时，脉冲发射的平均磁通密度为0.59 $ \ pm $ 0.16 JY。 B0950+08的脉冲发射为$ \ sim $ 110 $ \ pm $ 17 arcseconds（0.14 $ \ pm $ 0.02 pc），延长了光缸直径的良好，并排除了磁层的起源。使用我们的观察和调查VLSSR，TGSS，NVSS，First和Vlass的数据，我们发现B0950+08的频谱指数约为-1.36 $ \ pm $ 0.20，而PWN的频谱指数比-1.85 $ \ pm $ 0.45陡峭。
With the Expanded Long Wavelength Array (ELWA) and pulsar binning techniques, we searched for off-pulse emission from PSR B0950+08 at 76 MHz. Previous studies suggest that off-pulse emission can be due to pulsar wind nebulae (PWNe) in younger pulsars. Other studies, such as that done by Basu et al. (2012), propose that in older pulsars this emission extends to some radius that is on the order of the light cylinder radius, and is magnetospheric in origin. Through imaging analysis we conclude that this older pulsar with a spin-down age of 17 Myr has a surrounding PWN, which is unexpected since as a pulsar ages its PWN spectrum is thought to shift from being synchrotron to inverse-Compton-scattering dominated. At 76 MHz, the average flux density of the off-pulse emission is 0.59 $\pm$ 0.16 Jy. The off-pulse emission from B0950+08 is $\sim$ 110 $\pm$ 17 arcseconds (0.14 $\pm$ 0.02 pc) in size, extending well-beyond the light cylinder diameter and ruling out a magnetospheric origin. Using data from our observation and the surveys VLSSr, TGSS, NVSS, FIRST, and VLASS, we have found that the spectral index for B0950+08 is about -1.36 $\pm$ 0.20, while the PWN's spectral index is steeper than -1.85 $\pm$ 0.45.
