Parkes observations for project P995 semester 2018OCTS_06

We propose to perform observations of the very young pulsar PSR B0540–69 in the Large Magellanic Cloud to detect pulsed flux from this traditionally radio-quiet source. We are motivated to do so due to a relatively recent X-ray observation of a 36% change in its spin down rate, thought to be due to a state change in its magnetospheric processes. There is reason to believe this may be accompanied by an increase in pulsed flux, as has been seen in intermittent pulsar behaviour, for example. Additionally, PSR B0540–69 is known to emit giant pulses, one of only a small number of pulsars to do so. With the new Ultra Wideband Low-frequency (UWL) receiver system, we will be able to conduct the highest sensitivity observations of this source yet achieved at radio wavelengths. A successful detection of pulsed flux will provide important insight into the magnetospheric evolution and behaviour in this pulsar, and a better understanding of how its glitch behaviour may influence its emission. Even without such a detection, we will be able to study the giant pulse behaviour of PSR B0540–69 with unprecedented sensitivity.

我们提议对大麦哲伦云中的极年轻脉冲星PSR B0540–69开展观测，以探测这一传统射电宁静天体的脉冲辐射流量。开展此项观测的核心动因在于：近期一项X射线观测发现其自转减慢速率发生了36%的变化，该现象被认为源于其磁层过程的状态改变。有理由推测，此次状态改变可能伴随脉冲辐射流量的增强——例如在间歇性脉冲星的行为中就曾观测到此类现象。此外，已知PSR B0540–69会发射巨脉冲，此类天体仅占脉冲星总数的极少数。借助全新的超宽频低频(Ultra Wideband Low-frequency, UWL)接收机系统，我们将能够开展该源在射电波段迄今最高灵敏度的观测。若成功探测到脉冲辐射流量，将为深入理解该脉冲星的磁层演化与行为模式，以及其自转突变(glitch)行为如何影响其辐射过程提供关键科学洞见。即便未能探测到脉冲辐射流量，我们也能够以前所未有的灵敏度开展对PSR B0540–69巨脉冲行为的研究。